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2,030 results on '"Zhang, X. ‐ J."'

1. The Love Wave Immunosensor for Detecting the Pneumonia Biomarker Procalcitonin (PCT)

Author

Zhang, X. J., Xiong, H. M., Sun, J. Y., Hu, Y. J., Zhou, Y., Wan, H., Wang, T. X., Wang, P., Magjarević, Ratko, Series Editor, Ładyżyński, Piotr, Associate Editor, Ibrahim, Fatimah, Associate Editor, Lackovic, Igor, Associate Editor, Rock, Emilio Sacristan, Associate Editor, Wang, Guangzhi, editor, Yao, Dezhong, editor, Gu, Zhongze, editor, Peng, Yi, editor, Tong, Shanbao, editor, and Liu, Chengyu, editor

Published
2024
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2. Force-free current sheets in the Jovian magnetodisk: the key role of electron field-aligned anisotropy

Author

Artemyev, A. V., Ma, Q., Ebert, R. W., Zhang, X. -J., and Allegrini, F.

Subjects
Physics - Space Physics, Physics - Plasma Physics
Abstract

Current sheets are an essential element of the planetary magnetotails, where strong plasma currents self-consistently support magnetic field gradients. The current sheet configuration is determined by plasma populations that contribute to the current density. The most commonly investigated configuration is supported by diamagnetic cross-field currents of hot ions, typical for the magnetospheres of magnetized planets. In this study, we examine a new type of the current sheet configuration supported by field-aligned currents from electron streams in the Jovian magnetodisk. Such bi-directional streams increase the electron thermal anisotropy close to the fire-hose instability threshold and lead to strong magnetic field shear. The current sheet configuration supported by electron streams is nearly force-free, with B=const across the sheet. Using Juno plasma and magnetic field measurements, we investigate the internal structure of such current sheets and discuss possible mechanisms for their formation.

Published
2023
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3. Energetic electron precipitation driven by electromagnetic ion cyclotron waves from ELFIN's low altitude perspective

Author

Angelopoulos, V., Zhang, X. -J., Artemyev, A. V., Mourenas, D., Tsai, E., Wilkins, C., Runov, A., Liu, J., Turner, D. L., Li, W., Khurana, K., Wirz, R. E., Sergeev, V. A., Meng, X., Wu, J., Hartinger, M. D., Raita, T., Shen, Y., An, X., Shi, X., Bashir, M. F., Shen, X., Gan, L., Qin, M., Capannolo, L., Ma, Q., Russell, C. L., Masongsong, E. V., Caron, R., He, I., Iglesias, L., Jha, S., King, J., Kumar, S., Le, K., Mao, J., McDermott, A., Nguyen, K., Norris, A., Palla, A., Roosnovo, Tam, J., Xie, E., Yap, R. C., Ye, S., Young, C., Adair, L. A., Shaffer, C., Chung, M., Cruce, P., Lawson, M., Leneman, D., Allen, M., Anderson, M., Arreola-Zamora, M., Artinger, J., Asher, J., Branchevsky, D., Cliffe, M., Colton, K., Costello, C., Depe, D., Domae, B. W., Eldin, S., Fitzgibbon, L., Flemming, A., Frederick, D. M., Gilbert, A., Hesford, B., Krieger, R., Lian, K., McKinney, E., Miller, J. P., Pedersen, C., Qu, Z., Rozario, R., Rubly, M., Seaton, R., Subramanian, A., Sundin, S. R., Tan, A., Thomlinson, D., Turner, W., Wing, G., Wong, C., and Zarifian, A.

Subjects
Physics - Space Physics, Physics - Plasma Physics
Abstract

We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data from the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at 0.5 MeV which are abrupt (bursty) with significant substructure (occasionally down to sub-second timescale). Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Using two years of ELFIN data, we assemble a statistical database of 50 events of strong EMIC wave-driven precipitation. Most reside at L=5-7 at dusk, while a smaller subset exists at L=8-12 at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an L-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio's spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of 1.45 MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven 1MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to 200-300 keV by much less intense higher frequency EMIC waves. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation.

Published
2022
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4. Energetic Electron Precipitation Driven by Electromagnetic Ion Cyclotron Waves from ELFIN's Low Altitude Perspective.

Author

Angelopoulos, V, Zhang, X-J, Artemyev, AV, Mourenas, D, Tsai, E, Wilkins, C, Runov, A, Liu, J, Turner, DL, Li, W, Khurana, K, Wirz, RE, Sergeev, VA, Meng, X, Wu, J, Hartinger, MD, Raita, T, Shen, Y, An, X, Shi, X, Bashir, MF, Shen, X, Gan, L, Qin, M, Capannolo, L, Ma, Q, Russell, CL, Masongsong, EV, Caron, R, He, I, Iglesias, L, Jha, S, King, J, Kumar, S, Le, K, Mao, J, McDermott, A, Nguyen, K, Norris, A, Palla, A, Roosnovo, A, Tam, J, Xie, E, Yap, RC, Ye, S, Young, C, Adair, LA, Shaffer, C, Chung, M, Cruce, P, Lawson, M, Leneman, D, Allen, M, Anderson, M, Arreola-Zamora, M, Artinger, J, Asher, J, Branchevsky, D, Cliffe, M, Colton, K, Costello, C, Depe, D, Domae, BW, Eldin, S, Fitzgibbon, L, Flemming, A, Frederick, DM, Gilbert, A, Hesford, B, Krieger, R, Lian, K, McKinney, E, Miller, JP, Pedersen, C, Qu, Z, Rozario, R, Rubly, M, Seaton, R, Subramanian, A, Sundin, SR, Tan, A, Thomlinson, D, Turner, W, Wing, G, Wong, C, and Zarifian, A

Subjects
Electromagnetic ion cyclotron waves, Magnetosphere, Plasma waves, Radiation belts, Relativistic electron precipitation, Whistler-mode chorus, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We review comprehensive observations of electromagnetic ion cyclotron (EMIC) wave-driven energetic electron precipitation using data collected by the energetic electron detector on the Electron Losses and Fields InvestigatioN (ELFIN) mission, two polar-orbiting low-altitude spinning CubeSats, measuring 50-5000 keV electrons with good pitch-angle and energy resolution. EMIC wave-driven precipitation exhibits a distinct signature in energy-spectrograms of the precipitating-to-trapped flux ratio: peaks at >0.5 MeV which are abrupt (bursty) (lasting ∼17 s, or ΔL∼0.56) with significant substructure (occasionally down to sub-second timescale). We attribute the bursty nature of the precipitation to the spatial extent and structuredness of the wave field at the equator. Multiple ELFIN passes over the same MLT sector allow us to study the spatial and temporal evolution of the EMIC wave - electron interaction region. Case studies employing conjugate ground-based or equatorial observations of the EMIC waves reveal that the energy of moderate and strong precipitation at ELFIN approximately agrees with theoretical expectations for cyclotron resonant interactions in a cold plasma. Using multiple years of ELFIN data uniformly distributed in local time, we assemble a statistical database of ∼50 events of strong EMIC wave-driven precipitation. Most reside at L∼5-7 at dusk, while a smaller subset exists at L∼8-12 at post-midnight. The energies of the peak-precipitation ratio and of the half-peak precipitation ratio (our proxy for the minimum resonance energy) exhibit an L-shell dependence in good agreement with theoretical estimates based on prior statistical observations of EMIC wave power spectra. The precipitation ratio's spectral shape for the most intense events has an exponential falloff away from the peak (i.e., on either side of ∼1.45 MeV). It too agrees well with quasi-linear diffusion theory based on prior statistics of wave spectra. It should be noted though that this diffusive treatment likely includes effects from nonlinear resonant interactions (especially at high energies) and nonresonant effects from sharp wave packet edges (at low energies). Sub-MeV electron precipitation observed concurrently with strong EMIC wave-driven >1 MeV precipitation has a spectral shape that is consistent with efficient pitch-angle scattering down to ∼ 200-300 keV by much less intense higher frequency EMIC waves at dusk (where such waves are most frequent). At ∼100 keV, whistler-mode chorus may be implicated in concurrent precipitation. These results confirm the critical role of EMIC waves in driving relativistic electron losses. Nonlinear effects may abound and require further investigation.

Published
2023

5. Tens to hundreds of keV electron precipitation driven by kinetic Alfv\'en waves during an electron injection

Author

Shen, Y., Artemyev, A. V., Zhang, X. -J., Angelopoulos, V., Vasko, I., Turner, D., Tsai, E., Wilkins, C., Weygand, J., Russell, C. T., Ergun, R. E., and Giles, B. L.

Subjects
Physics - Space Physics, Physics - Fluid Dynamics, Physics - Plasma Physics
Abstract

Electron injections are critical processes associated with magnetospheric substorms, which deposit significant electron energy into the ionosphere. Although wave scattering of $<$10 keV electrons during injections has been well studied, the link between magnetotail electron injections and energetic ($\geq$100 keV) electron precipitation remains elusive. Using conjugate observations between the ELFIN and Magnetospheric Multiscale (MMS) missions, we present evidence of tens to hundreds of keV electron precipitation to the ionosphere potentially driven by kinetic Alfv\'en waves (KAWs) associated with magnetotail electron injections and magnetic field gradients. Test particle simulations adapted to observations show that dipolarization-front magnetic field gradients and associated $\nabla B$ drifts allow Doppler-shifted Landau resonances between the injected electrons and KAWs, producing electron spatial scattering across the front which results in pitch-angle decreases and subsequent precipitation. Test particle results show that such KAW-driven precipitation can account for ELFIN observations below $\sim$300 keV., Comment: 25 pages, 5 figures, with supporting information, the manuscript has been accepted for publication by JGR space physics

Published
2022
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6. Extreme Energy Spectra of Relativistic Electron Flux in the Outer Radiation Belt

Author

Mourenas, D, Artemyev, AV, Zhang, X‐J, and Angelopoulos, V

Subjects
radiation belt, extreme electron flux, extreme energy spectra, chorus wave, EMIC wave, attractor, Astronomical and Space Sciences, Atmospheric Sciences
Abstract

Electron diffusion by whistler-mode chorus waves is one of the key processes controlling the dynamics of relativistic electron fluxes in the Earth's radiation belts. It is responsible for the acceleration of sub-relativistic electrons injected from the plasma sheet to relativistic energies as well as for their precipitation and loss into the atmosphere. Based on analytical estimates of chorus wave-driven quasi-linear electron energy and pitch-angle diffusion rates, we provide analytical steady-state solutions to the corresponding Fokker-Planck equation for the relativistic electron distribution and flux. The impact on these steady-state solutions of additional electromagnetic ion cyclotron waves, and of ultralow frequency waves are examined. Such steady-state solutions correspond to hard energy spectra at 1-4 MeV, dangerous for satellite electronics, and represent attractors for the system dynamics in the presence of sufficiently strong driving by continuous injections of 10-300 keV electrons. Therefore, these analytical steady-state solutions provide a simple means for estimating the most extreme electron energy spectra potentially encountered in the outer radiation belt, despite the great variability of injections and plasma conditions. These analytical steady-state solutions are compared with numerical simulations based on the full Fokker-Planck equation and with relativistic electron flux spectra measured by satellites during one extreme event and three strong events of high time-integrated geomagnetic activity, demonstrating a good agreement.

Published
2022

8. A Climatology of Long-Duration High 2-MeV Electron Flux Periods in the Outer Radiation Belt.

Author

Mourenas, D, Agapitov, O, Artemyev, A, and Zhang, X-J

Subjects
electron acceleration, electron flux, forecast, radiation belt, return levels, space weather
Abstract

Since the advent of the Space Age, the importance of understanding and forecasting relativistic electron fluxes in the Earths radiation belts has been steadily growing due to the threat that such particles pose to satellite electronics. Here, we provide a model of long-duration periods of high time-integrated 2-MeV electron flux deep inside the outer radiation belt, based on the significant correlation obtained in 2001-2017 between time-integrated electron flux measured by satellites and a measure of the preceding time-integrated homogenized aa H geomagnetic index. We show that this correlation is likely due to a stronger cumulative chorus wave-driven acceleration of relativistic electrons and a stronger cumulative inward radial diffusion of such electrons during periods of higher time-integrated geomagnetic activity. Return levels of 2-MeV electron flux are provided based on Extreme Value analysis of time-integrated geomagnetic activity over 1868-2017, in rough agreement with estimates based on 20-year data sets of measured flux. A high correlation is also found between our measure of time-integrated geomagnetic activity averaged over each solar cycle and averaged sunspot numbers, potentially paving the way for forecasts of time-integrated relativistic electron flux during future solar cycles based on predictions of solar activity.

Published
2022

9. Characterization of Pedestal Burst Instabilities during I-mode to H-mode Transition in the EAST Tokamak

Author

Zhong, X. M., Zou, X. L., Liu, A. D., Song, Y. T., Zhuang, G., Li, E. Z., Zhang, B., Zhang, J., Zhou, C., Feng, X., Duan, Y. M., Ding, R., Liu, H. Q., Lv, B., Wang, L., Xu, L. Q., Zhang, L., Zhao, Hailin, Zhang, Tao, Zang, Qing, Ding, B. J., Li, M. H., Qin, C. M., Wang, X. J., Zhang, X. J., and Team, EAST

Subjects
Physics - Plasma Physics
Abstract

Quasi-periodic Pedestal Burst Instabilities (PBIs), featuring alternative turbulence suppression and bursts, have been clearly identified by various edge diagnostics during I-mode to H-mode transition in the EAST Tokamak. The radial distribution of the phase perturbation caused by PBI shows that PBI is localized in the pedestal. Prior to each PBI, a significant increase of density gradient close to the pedestal top can be clearly distinguished, then the turbulence burst is generated, accompanied by the relaxation of the density profile, and then induces an outward particle flux. The relative density perturbation caused by PBIs is about $6 \sim 8\%$. Statistic analyses show that the pedestal normalized density gradient triggering the first PBI has a threshold value, mostly in the range of $22 \sim 24$, suggesting that a PBI triggering instability could be driven by the density gradient. And the pedestal normalized density gradient triggering the last PBI is about $30 \sim 40$ and seems to increase with the loss power and the chord-averaged density. In addition, the frequency of PBI is likely to be inversely proportional to the chord-averaged density and the loss power. These results suggest that PBIs and the density gradient prompt increase prior to PBIs can be considered as the precursor for controlling I-H transition.

Published
2021
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10. Short Chorus Wave Packets: Generation Within Chorus Elements, Statistics, and Consequences on Energetic Electron Precipitation

Author

Mourenas, D, Zhang, X‐J, Nunn, D, Artemyev, AV, Angelopoulos, V, Tsai, E, and Wilkins, C

Subjects
chorus wave, nonlinear generation, wave superposition, wave beating, anomalous trapping, quasi-linear diffusion, quasi‐linear diffusion, Astronomical and Space Sciences, Atmospheric Sciences
Abstract

Short and intense lower-band chorus wave packets are ubiquitous in the Earth's outer radiation belt. In this article, we perform various Vlasov hybrid simulations, with one or two triggering waves, to study the generation of short chorus packets/subpackets inside long rising tone elements. We show that the length of the generated short wave packets is consistent with a criterion of resonance non-overlap for two independent superposed waves, and that these chorus packets have similar characteristics as in Van Allen Probes observations. We find that short wave packets are mainly formed near the middle/end of long rising tones for moderate linear growth rates, and everywhere for stronger linear growth rates. Finally, we analyze an event characterized by Time History of Events and Macroscale Interactions during Substorms spacecraft measurements of chorus rising tones near the equator and simultaneous measurements by low altitude ELFIN CubeSats of precipitating and trapped electron fluxes in the same sector. The measured precipitating electron fluxes are well recovered by test particle simulations performed using measured plasma and wave properties. We show that short chorus wave packets of moderate amplitudes (160-250 pT) essentially lead to a more diffusive-like transport of 50-200 keV electrons toward the loss cone than long packets. In contrast, long chorus packets are found to produce important nonlinear effects via anomalous trapping, which significantly reduces electron precipitation below 150 keV, especially for higher wave amplitudes.

Published
2022

11. Charged particle scattering in dipolarized magnetotail

Author

Lukin, A. S., Artemyev, A. V., Petrukovich, A. A., and Zhang, X. -J.

Subjects
Physics - Space Physics, Physics - Plasma Physics
Abstract

The Earth's magnetotail is characterized by stretched magnetic field lines. Energetic particles are effectively scattered due to the field-line curvature, which then leads to isotropization of energetic particle distributions and particle precipitation to the Earth's atmosphere. Measurements of these precipitation at low-altitude spacecraft are thus often used to remotely probe the magnetotail current sheet configuration. This configuration may include spatially localized maxima of the curvature radius at equator (due to localized humps of the equatorial magnetic field magnitude) that reduce the energetic particle scattering and precipitation. Therefore, the measured precipitation patterns are related to the spatial distribution of the equatorial curvature radius that is determined by the magnetotail current sheet configuration. In this study, we show that, contrary to previous thoughts, the magnetic field line configuration with the localized curvature radius maximum can actually enhance the scattering and subsequent precipitation. The spatially localized magnetic field dipolarization (magnetic field humps) can significantly curve magnetic field lines far from the equator and create off-equatorial minima in the curvature radius. Scattering of energetic particles in these off-equatorial regions alters the scattering (and precipitation) patterns, which has not been studied yet. We discuss our results in the context of remote-sensing the magnetotail current sheet configuration with low-altitude spacecraft measurements.

Published
2021
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12. The ELFIN Mission

Author

Angelopoulos, V., Tsai, E., Bingley, L., Shaffer, C., Turner, D. L., Runov, A., Li, W., Liu, J., Artemyev, A. V., Zhang, X. -J., Strangeway, R. J., Wirz, R. E., Shprits, Y. Y., Sergeev, V. A., Caron, R. P., Chung, M., Cruce, P., Greer, W., Grimes, E., Hector, K., Lawson, M. J., Leneman, D., Masongsong, E. V., Russell, C. L., Wilkins, C., Hinkley, D., Blake, J. B., Adair, N., Allen, M., Anderson, M., Arreola-Zamora, M., Artinger, J., Asher, J., Branchevsky, D., Capitelli, M. R., Castro, R., Chao, G., Chung, N., Cliffe, M., Colton, K., Costello, C., Depe, D., Domae, B. W., Eldin, S., Fitzgibbon, L., Flemming, A., Fox, I., Frederick, D. M., Gilbert, A., Gildemeister, A., Gonzalez, A., Hesford, B., Jha, S., Kang, N., King, J., Krieger, R., Lian, K., Mao, J., McKinney, E., Miller, J. P., Norris, A., Nuesca, M., Palla, A., Park, E. S. Y., Pedersen, C. E., Qu, Z., Rozario, R., Rye, E., Seaton, R., Subramanian, A., Sundin, S. R., Tan, A., Turner, W., Villegas, A. J., Wasden, M., Wing, G., Wong, C., Xie, E., Yamamoto, S., Yap, R., Zarifian, A., and Zhang, G. Y.

Subjects
Physics - Space Physics, Physics - Geophysics, Physics - Instrumentation and Detectors, Physics - Plasma Physics
Abstract

The Electron Loss and Fields Investigation with a Spatio-Temporal Ambiguity-Resolving option (ELFIN-STAR, or simply: ELFIN) mission comprises two identical 3-Unit (3U) CubeSats on a polar (~93deg inclination), nearly circular, low-Earth (~450 km altitude) orbit. Launched on September 15, 2018, ELFIN is expected to have a >2.5 year lifetime. Its primary science objective is to resolve the mechanism of storm-time relativistic electron precipitation, for which electromagnetic ion cyclotron (EMIC) waves are a prime candidate. From its ionospheric vantage point, ELFIN uses its unique pitch-angle-resolving capability to determine whether measured relativistic electron pitch-angle and energy spectra within the loss cone bear the characteristic signatures of scattering by EMIC waves or whether such scattering may be due to other processes. Pairing identical ELFIN satellites with slowly-variable along-track separation allows disambiguation of spatial and temporal evolution of the precipitation over minutes-to-tens-of-minutes timescales, faster than the orbit period of a single low-altitude satellite (~90min). Each satellite carries an energetic particle detector for electrons (EPDE) that measures 50keV to 5MeV electrons with deltaE/E<40% and a fluxgate magnetometer (FGM) on a ~72cm boom that measures magnetic field waves (e.g., EMIC waves) in the range from DC to 5Hz Nyquist (nominally) with <0.3nT/sqrt(Hz) noise at 1Hz. The spinning satellites (T_spin~3s) are equipped with magnetorquers that permit spin-up/down and reorientation maneuvers. The spin axis is placed normal to the orbit plane, allowing full pitch-angle resolution twice per spin. An energetic particle detector for ions (EPDI) measures 250keV-5MeV ions, addressing secondary science. Funded initially by CalSpace and the University Nanosat Program, ELFIN was selected for flight with joint support from NSF and NASA between 2014 and 2018., Comment: Submitted to Space Science Reviews April 2020. 51 pages, 7 tables, 21 figures

Published
2020
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13. Helicon plasma in a magnetic shuttle

Author

Chang, L., Liu, J., Yuan, X. G., Yang, X., Zhou, H. S., Luo, G. N., Zhang, X. J., Peng, Y. K., Dai, J., and Hang, G. R.

Subjects
Physics - Plasma Physics
Abstract

The definition of magnetic shuttle is introduced to describe the magnetic space enclosed by two tandem magnetic mirrors with the same field direction and high mirror ratio. Helicon plasma immersed in such a magnetic shuttle which can provide the confinement of charged particles is modeled using an electromagnetic solver. The perpendicular structure of wave field along this shuttle is given in terms of stream vector plots, showing significant change from midplane to ending throats, and the vector field rotates and forms a circular layer that separating plasma column radially into core and edge regions near the throats. The influences of driving frequency, plasma density and field strength on the wave field and power absorption are computed in detail. It is found that the wave magnitude and power absorption decrease for increased driving frequency and reduced field strength, and maximize around a certain level of plasma density. The axial standing-wave feature always exists, due to the interference between forward and reflected waves from ending magnetic mirrors, while the radial wave field structure largely stays the same. Distributions of wave energy density and power absorption density all show shrinking feature from midplane to ending throats, which is consistent with the nature of helicon mode that propagating along field lines. Theoretical analysis based on a simple magnetic shuttle and the governing equation of helicon waves shows consistency with computed results and previous studies.

Published
2020

14. Systematic Regularity of Solar Coronal Rotation During the Time Interval 1939-2019

Author

Deng, L. H., Zhang, X. J., Deng, H., Mei, Y., and Wang, F.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Temporal variation of the solar coronal rotation appears to be very complex and its relevances to the eleven-year solar activity cycle are still unclear. Using the modified coronal index for the time interval from 1939 January 1 to 2019 May 31, the systematic regularities of the solar coronal rotation are investigated. Our main findings are as follows: (1) from a global point of view, the synodic coronal rotation period with a value of 27.5 days is the only significant period at the periodic scales shorter than 64 days; (2) the coronal rotation period exhibit an obviously decreasing trend during the considered time interval, implying the solar corona accelerates its global rotation rate in the long run; (3) there exist significant periods of 3.25, 6.13, 9.53, and 11.13 years in the period length of the coronal rotation, providing an evidence that the coronal rotation should be connected with the quasi-biennial oscillation, the eleven-year solar cycle, and the 22-year Hale cycle (or the magnetic activity reversal); and (4) the phase relationship between the coronal rotation period and the solar magnetic activity is not only time-dependent but also frequency-dependent. For a small range around the 11- year cycle band, there is a systematic trend in the phase, and the small mismatch in this band brings out the phase to drift. The possible mechanism for the above analysis results is discussed., Comment: 9 Pages, 12 figures, Accepted by MNRAS

Published
2019
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15. Phase and amplitude asymmetry in the quasi-biennial oscillation of solar Halpha flare activity

Author

Deng, L. H., Zhang, X. J., Li, G. Y., Deng, H., and Wang, F.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Quasi-biennial oscillation (QBO) of solar magnetic activities is intrinsic to dynamo mechanism, but still far from fully understood. In this work, the phase and amplitude asymmetry of solar QBO of Halpha flare activity in the northern and southern hemispheres is studied by the ensemble empirical mode decomposition, the cross-correlation analysis, and the wavelet transform technique. The following results are found: (1) solar QBO of Halpha flare index in the two hemispheres has a complicated phase relationship, but does not show any systematic regularity; (2) the solar cycle mode of solar Halpha flare index in the northern hemisphere generally leads that in the southern one by 9 months for the time interval from 1966 to 2014. The possible origin of these results is discussed.

Published
2019
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16. Magnetotail reconnection onset caused by electron kinetics with a strong external driver.

Author

Lu, San, Wang, Rongsheng, Lu, Quanming, Angelopoulos, V, Nakamura, R, Artemyev, AV, Pritchett, PL, Liu, TZ, Zhang, X-J, Baumjohann, W, Gonzalez, W, Rager, AC, Torbert, RB, Giles, BL, Gershman, DJ, Russell, CT, Strangeway, RJ, Qi, Y, Ergun, RE, Lindqvist, P-A, Burch, JL, and Wang, Shui

Abstract

Magnetotail reconnection plays a crucial role in explosive energy conversion in geospace. Because of the lack of in-situ spacecraft observations, the onset mechanism of magnetotail reconnection, however, has been controversial for decades. The key question is whether magnetotail reconnection is externally driven to occur first on electron scales or spontaneously arising from an unstable configuration on ion scales. Here, we show, using spacecraft observations and particle-in-cell (PIC) simulations, that magnetotail reconnection starts from electron reconnection in the presence of a strong external driver. Our PIC simulations show that this electron reconnection then develops into ion reconnection. These results provide direct evidence for magnetotail reconnection onset caused by electron kinetics with a strong external driver.

Published
2020

18. The ELFIN Mission

Author

Angelopoulos, V, Tsai, E, Bingley, L, Shaffer, C, Turner, DL, Runov, A, Li, W, Liu, J, Artemyev, AV, Zhang, X-J, Strangeway, RJ, Wirz, RE, Shprits, YY, Sergeev, VA, Caron, RP, Chung, M, Cruce, P, Greer, W, Grimes, E, Hector, K, Lawson, MJ, Leneman, D, Masongsong, EV, Russell, CL, Wilkins, C, Hinkley, D, Blake, JB, Adair, N, Allen, M, Anderson, M, Arreola-Zamora, M, Artinger, J, Asher, J, Branchevsky, D, Capitelli, MR, Castro, R, Chao, G, Chung, N, Cliffe, M, Colton, K, Costello, C, Depe, D, Domae, BW, Eldin, S, Fitzgibbon, L, Flemming, A, Fox, I, Frederick, DM, Gilbert, A, Gildemeister, A, Gonzalez, A, Hesford, B, Jha, S, Kang, N, King, J, Krieger, R, Lian, K, Mao, J, McKinney, E, Miller, JP, Norris, A, Nuesca, M, Palla, A, Park, ESY, Pedersen, CE, Qu, Z, Rozario, R, Rye, E, Seaton, R, Subramanian, A, Sundin, SR, Tan, A, Turner, W, Villegas, AJ, Wasden, M, Wing, G, Wong, C, Xie, E, Yamamoto, S, Yap, R, Zarifian, A, and Zhang, GY

Subjects
CubeSat, Van Allen radiation belts, EMIC, electromagnetic ion cyclotron waves, Magnetosphere, Particle precipitation, Auroral, Loss cone, Electron, Ionosphere, Pitch angle scattering, Energetic particle detector, Fluxgate magnetometer, UCLA, physics.space-ph, physics.geo-ph, physics.ins-det, physics.plasm-ph, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

The Electron Loss and Fields Investigation with a Spatio-Temporal Ambiguity-Resolving option (ELFIN-STAR, or heretoforth simply: ELFIN) mission comprises two identical 3-Unit (3U) CubeSats on a polar (∼93∘ inclination), nearly circular, low-Earth (∼450 km altitude) orbit. Launched on September 15, 2018, ELFIN is expected to have a >2.5 year lifetime. Its primary science objective is to resolve the mechanism of storm-time relativistic electron precipitation, for which electromagnetic ion cyclotron (EMIC) waves are a prime candidate. From its ionospheric vantage point, ELFIN uses its unique pitch-angle-resolving capability to determine whether measured relativistic electron pitch-angle and energy spectra within the loss cone bear the characteristic signatures of scattering by EMIC waves or whether such scattering may be due to other processes. Pairing identical ELFIN satellites with slowly-variable along-track separation allows disambiguation of spatial and temporal evolution of the precipitation over minutes-to-tens-of-minutes timescales, faster than the orbit period of a single low-altitude satellite (Torbit ∼ 90 min). Each satellite carries an energetic particle detector for electrons (EPDE) that measures 50 keV to 5 MeV electrons with Δ E/E < 40% and a fluxgate magnetometer (FGM) on a ∼72 cm boom that measures magnetic field waves (e.g., EMIC waves) in the range from DC to 5 Hz Nyquist (nominally) with 1 MeV. This broad energy range of precipitation indicates that multiple waves are providing scattering concurrently. Many observed events show significant backscattered fluxes, which in the past were hard to resolve by equatorial spacecraft or non-pitch-angle-resolving ionospheric missions. These observations suggest that the ionosphere plays a significant role in modifying magnetospheric electron fluxes and wave-particle interactions. Routine data captures starting in February 2020 and lasting for at least another year, approximately the remainder of the mission lifetime, are expected to provide a very rich dataset to address questions even beyond the primary mission science objective.

Published
2020

23. Evolution of electron distribution driven by nonlinear resonances with intense field-aligned chorus waves

Author

Vainchtein, D., Zhang, X. -J., Artemyev, A. V., Mourenas, D., Angelopoulos, V., and Thorne, R. M.

Subjects
Physics - Plasma Physics
Abstract

Resonant electron interaction with whistler-mode chorus waves is recognized as one of the main drivers of radiation belt dynamics. For moderate wave intensity, this interaction is well described by quasi-linear theory. However, recent statistics of parallel propagating chorus waves have demonstrated that 5-20% of the observed waves are sufficiently intense to interact nonlinearly with electrons. Such interactions include phase trapping and phase bunching (nonlinear scattering) effects not described by the quasi-linear diffusion. For sufficiently long (large) wave-packets, these nonlinear effects can result in very rapid electron acceleration and scattering. In this paper we introduce a method to include trapping and nonlinear scattering into the kinetic equation describing the evolution of the electron distribution function. We use statistics of Van Allen Probes and Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations to determine the probability distribution of intense, long wave-packets as function of power and frequency. Then we develop an analytical model of particle resonance of an individual particle with an intense chorus wave-packet and derive the main properties of this interaction: probability of electron trapping, energy change due to trapping and nonlinear scattering. These properties are combined in a nonlocal operator acting on the electron distribution function. When multiple waves are present, we average the obtained operator over the observed distributions of waves and examine solutions of the resultant kinetic equation. We also examine energy conservation and its implications in systems with the nonlinear wave-particle interaction.

Published
2018
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24. Generation and Impacts of Whistler‐Mode Waves During Energetic Electron Injections in Jupiter's Outer Radiation Belt.

Author

Ma, Q., Li, W., Zhang, X.‐J., Bortnik, J., Shen, X.‐C., Daly, A., Kurth, W. S., Mauk, B. H., Allegrini, F., Connerney, J. E. P., Bagenal, F., and Bolton, S. J.

Subjects
RADIATION belts, JUNO (Space probe), ELECTRONS, RELATIVISTIC electrons, ELECTRON scattering, ELECTRON distribution
Abstract

Energetic particle injections are commonly observed in Jupiter's magnetosphere and have important impacts on the radiation belts. We evaluate the roles of electron injections in the dynamics of whistler‐mode waves and relativistic electrons using Juno measurements and wave‐particle interaction modeling. The Juno spacecraft observed injected electron flux bursts at energies up to 300 keV at M shell ∼11 near the magnetic equator during perijove‐31. The electron injections are related to chorus wave bursts at 0.05–0.5 fce frequencies, where fce is the electron gyrofrequency. The electron pitch angle distributions are anisotropic, peaking near 90° pitch angle, and the fluxes are high during injections. We calculate the whistler‐mode wave growth rates using the observed electron distributions and linear theory. The frequency spectrum of the wave growth rate is consistent with that of the observed chorus magnetic intensity, suggesting that the observed electron injections provide free energy to generate whistler‐mode chorus waves. We further use quasilinear theory to model the impacts of chorus waves on 0.1–10 MeV electrons. Our modeling shows that the chorus waves could cause the pitch angle scattering loss of electrons at <1 MeV energies and accelerate relativistic electrons at multiple MeV energies in Jupiter's outer radiation belt. The electron injections also provide an important seed population at several hundred keV energies to support the acceleration to higher energies. Our wave‐particle interaction modeling demonstrates the energy flow from the electron injections to the relativistic electron population through the medium of whistler‐mode waves in Jupiter's outer radiation belt. Key Points: Chorus wave generation due to electron injections is demonstrated by their correlative occurrence and wave instability analysisWhistler‐mode waves scatter electrons into the loss cone and cause diffuse auroral precipitation with intensities of 60–160 erg/cm2/sChorus waves cause local acceleration of MeV electrons in several days, further aided by the seed electron population from injections [ABSTRACT FROM AUTHOR]

Published
2024
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34. Observation of $\eta^{\prime}\to\omega e^{+} e^{-}$

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, Y. Hu G. M. Huang G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcud, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, C. H., Li, Cheng, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Loue, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Moriya, K., Muchnoia, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaeva, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Weber, T., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Yin, M. H. Ye J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncug, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugovh, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Based on a sample of \etapr mesons produced in the radiative decay $J/\psi\to\gamma\eta^{\prime}$ in $1.31\times 10^9$ $J/\psi$ events collected with the BESIII detector, the decay $\eta^{\prime}\to\omega e^{+} e^{-}$ is observed for the first time, with a statistical significance of $8\sigma$. The branching fraction is measured to be $\mathcal{B}(\eta^{\prime}\to\omega e^{+} e^{-})=(1.97\pm0.34(\text{stat})\pm0.17(\text{syst}))\times10^{-4}$, which is in agreement with theoretical predictions. The branching fraction of $\eta^{\prime}\to\omega\gamma$ is also measured to be $(2.55\pm0.03(\text{stat})\pm0.16(\text{syst}))\times10^{-2}$, which is the most precise measurement to date, and the relative branching fraction $\frac{\mathcal{B}(\eta^{\prime}\to \omega e^{+}e^{-})}{\mathcal{B}(\eta^{\prime}\to \omega \gamma)}$ is determined to be $(7.71\pm1.34(\text{stat})\pm0.54(\text{syst}))\times10^{-3}$., Comment: 8 pages, 10 figures

Published
2015
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35. Study of J/psi->eta phi pi+pi- at BESIII

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, Y. Hu G. M. Huang G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcud, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, C. H., Li, Cheng, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Loue, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Moriya, K., Muchnoia, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaeva, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Weber, T., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Yin, M. H. Ye J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncug, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugovh, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Based on a sample of $2.25\times 10^{8} J/\psi$ events taken with the BESIII detector at the BEPCII collider, we present the results of a study of the decay $J/\psi\to \eta \phi\pi^{+}\pi^{-}$. The $Y(2175)$ resonance is observed in the invariant mass spectrum of $\phi f_{0}(980)$ with a statistical significance of greater than $10\sigma$. The corresponding mass and width are determined to be $M=2200\pm 6 \mathrm{(stat.)} \pm 5\mathrm{(syst.)} \mathrm{MeV}/c^{2}$ and $\Gamma=104\pm 15\mathrm{(stat.)}\pm 15\mathrm{(syst.)}$ MeV, respectively, and the product branching fraction is measured to be $\mathcal{B}(J/\psi\to\eta Y(2175)$, $Y(2175)\to \phi f_{0}(980)$, $f_{0}(980)\to \pi^{+}\pi^{-})= (1.20\pm 0.14\mathrm{(stat.)}\pm 0.37 \mathrm{(syst.)})\times 10^{-4}$. The results are consistent within errors with those of previous experiments. We also measure the branching fraction of $J/\psi\to \phi f_1(1285)$ with $f_1(1285)\to \eta\pi^{+}\pi^{-}$ and set upper limits on the branching fractions for $J/\psi\to \phi\eta(1405)$/$\phi X(1835)$/$\phi X(1870)$ with $\eta(1405)$/$X(1835)$/$X(1870)\to \eta\pi^{+}\pi^{-}$ at the 90\% confidence level., Comment: 11 pages, 11 figures

Published
2014
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36. Search for the $Y(4140)$ via $e^{+} e^{-} \to \gamma \phi J/\psi$ at $\sqrt{s}=$ 4.23, 4.26 and 4.36 GeV

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, Y. Hu G. M. Huang G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcud, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, C. H., Li, Cheng, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Loue, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Moriya, K., Muchnoia, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaeva, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Weber, T., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Yin, M. H. Ye J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncug, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugovh, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using data samples collected at center-of-mass energies $\sqrt{s} = 4.23$, 4.26, and 4.36 GeV with the BESIII detector operating at the BEPCII storage ring, we search for the production of the charmoniumlike state $Y(4140)$ through a radiative transition followed by its decay to $\phi J/\psi$. No significant signal is observed and upper limits on $\sigma[e^{+} e^{-} \rightarrow \gamma Y(4140)] \cdot \mathcal{B}(Y(4140)\rightarrow \phi J/\psi)$ at the $90\%$ confidence level are estimated as 0.35, 0.28, and 0.33 pb at $\sqrt{s} = 4.23$, 4.26, and 4.36 GeV, respectively.

Published
2014
Full Text
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37. Evidence for $e^+e^-\to\gamma\chi_{c1, 2}$ at center-of-mass energies from 4.009 to 4.360 GeV

Author

BESIII Collaboration, Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcu, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, Cheng, Li, C. H., Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yin, J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using data samples collected at center-of-mass energies of $\sqrt{s}$ = 4.009, 4.230, 4.260, and 4.360 GeV with the BESIII detector operating at the BEPCII collider, we perform a search for the process $e^+e^-\to\gamma\chi_{cJ}$ $(J = 0, 1, 2)$ and find evidence for $e^+e^-\to\gamma\chi_{c1}$ and $e^+e^-\to\gamma\chi_{c2}$ with statistical significances of 3.0$\sigma$ and 3.4$\sigma$, respectively. The Born cross sections $\sigma^{B}(e^+e^-\to\gamma\chi_{cJ})$, as well as their upper limits at the 90% confidence level are determined at each center-of-mass energy., Comment: 8 pages, 7 figures, 3 tables

Published
2014
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38. Search for the weak decays $J/\psi \to D^{(*)}_{s}e\nu_{e}$

Author

BESIII collaboration, Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcu, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, C. H., Li, Cheng, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yin, J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using a sample of $2.25\times 10^8$ $J/\psi$ events collected with the BESIII detector at the BEPCII collider, we search for the $J/\psi$ semi-leptonic weak decay $J/\psi \to D^{-}_{s} e^{+}\nu_{e}+c.c.$ with a much higher sensitivity than previous searches. We also perform the first search for $J/\psi \to D^{*-}_{s} e^{+}\nu_{e}+c.c.$ No significant excess of a signal above background is observed in either channel. At the $90\%$ confidence level, the upper limits are determined to be $\mathcal{B}(J/\psi \to D^{-}_{s}e^{+}\nu_{e}+c.c.)<1.3\times10^{-6}$ and $\mathcal{B}(J/\psi \to {D^{*}_{s}}^{-}e^{+}\nu_{e}+c.c.)<1.8\times10^{-6}$, respectively. Both are consistent with Standard Model predictions., Comment: 9 pages, 4 figures

Published
2014
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39. Study of $e^+e^-\to\omega\chi_{cJ}$ at center-of-mass energies from 4.21 to 4.42 GeV

Author

BESIII Collaboration, Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcu, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Li, Cheng, Li, C. H., Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yin, J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Based on data samples collected with the BESIII detector at the BEPCII collider at 9 center-of-mass energies from 4.21 to 4.42 GeV, we search for the production of $e^+e^-\to \omega\chi_{cJ}$ ($J$=0, 1, 2). The process $e^+e^-\to \omega\chi_{c0}$ is observed for the first time, and the Born cross sections at $\sqrt{s}$=4.23 and 4.26 GeV are measured to be $(55.4\pm 6.0\pm 5.9)$ and $(23.7\pm 5.3\pm 3.5)$ pb, respectively, where the first uncertainties are statistical and the second are systematic. The $\omega\chi_{c0}$ signals at the other 7 energies and $e^+e^-\to \omega\chi_{c1}$ and $\omega\chi_{c2}$ signals are not significant, and the upper limits on the cross sections are determined. By examining the $\omega\chi_{c0}$ cross section as a function of center-of-mass energy, we find that it is inconsistent with the line shape of the $Y(4260)$ observed in $e^+ e^-\to\pi^+\pi^-J/\psi$. Assuming the $\omega\chi_{c0}$ signals come from a single resonance, we extract mass and width of the resonance to be $(4230\pm8\pm6)$ MeV/$c^2$ and $(38\pm12\pm2)$ MeV, respectively, and the statistical significance is more than $9\sigma$., Comment: 7 pages, 5 figures

Published
2014
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40. Observation of $e^+e^-\to \pi^0\pi^0 h_c$ and a neutral charmoniumlike structure $Z_c(4020)^0$

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, H. Y., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, X., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y., Guo, Y. P., Haddadi, Z., Hafner, A., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kliemt, R., Kloss, B., Kolcu, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Leyhe, M., Li, Cheng, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, Q. J., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. M., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, J. Y., Liu, K., Liu, K. Y., Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. N., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Xue, Z., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yin, J. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. T., Zhang, H. Y., Zhang, J. J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, S., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using data collected with the BESIII detector operating at the Beijing Electron Positron Collider at center-of-mass energies of $\sqrt{s}=4.23$, 4.26, and 4.36~GeV, we observe $\EE\to \pphc$ for the first time. The Born cross sections are measured and found to be about half of those of $\EE\to \pi^+\pi^-h_c$ within less than 2$\sigma$. In the $\pi^0h_c$ mass spectrum, a structure at 4.02~GeV/$c^2$ is found. It is most likely to be the neutral isospin partner of the $\zcp^{\pm}$ observed in the process of $\EE\to \pi^+\pi^-h_c$ is found. A fit to the $\pi^0 h_c$ invariant mass spectrum, with the width of the $\zcpn$ fixed to that of its charged isospin partner and possible interferences with non-$\zcpn$ amplitudes neglected, gives a mass of ($4023.9\pm 2.2 \pm 3.8$)~MeV/$c^2$ for the $\zcpn$, where the first error is statistical and the second systematic., Comment: 7 pages, 2 figures

Published
2014
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41. Search for C-parity violation in $J/ \psi \to \gamma\gamma$ and $ \gamma \phi$

Author

BESIII Collaboration, Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Braun, S., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Gao, Q., Gao, Y., Garzia, I., Geng, C., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y. P., Haddadi, Z., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, X. T., Huang, Y., Hussain, T., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kloss, B., Kolcu, O. B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Leyhe, M., Li, Cheng, Li, Cui, Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, Q. J., Li, T., Li, W. D., Li, W. G., Li, X. H., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, K., Liu, K. Y., Liu, Q., Liu, S. B., Liu, X., Liu, X. X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, J. G., Lu, R. Q., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Pu, Y. N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ren, H. L., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Sosio, S., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Werner, M., Wiedner, U., Wolke, M., Wu, L. H., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Xue, Z., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zang, S. L., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, L., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using $1.06\times10^8$ $\psi(3686)$ events recorded in $e^{+}e^{-}$ collisions at $\sqrt{s}=$ 3.686 GeV with the BESIII at the BEPCII collider, we present searches for C-parity violation in $J/\psi \to \gamma\gamma$ and $ \gamma \phi$ decays via $\psi(3686) \to J/\psi \pi^+\pi^-$. No significant signals are observed in either channel. Upper limits on the branching fractions are set to be $\mathcal{B}(J/\psi \to \gamma\gamma) < 2.7 \times 10^{-7}$ and $\mathcal{B}(J/\psi \to \gamma\phi) < 1.4 \times 10^{-6}$ at the 90\% confidence level. The former is one order of magnitude more stringent than the previous upper limit, and the latter represents the first limit on this decay channel., Comment: 7 pages, 2 figures

Published
2014
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43. Blood cell count-derived inflammation indices as predictors of the osteoporotic risk of postmenopausal women.

Author

ZHANG, X. J., ZHAO, H., ZHANG, D., YE, D. D., QIN, J., ZHOU, Y. R., and ZHANG, Y. Z.

Abstract

OBJECTIVE: We investigated the associations between osteoporosis (OP) and systemic immune inflammation index (SII), neutrophil- to-lymphocyte ratio (NLR), monocyte-to-lymphocyte ratio (MLR), and platelet-to-lymphocyte ratio (PLR) in postmenopausal women. PATIENTS AND METHODS: This retrospective study included 966 postmenopausal women. Logistic regression and receiver operating characteristic curve (ROC) analyses were applied to explore the relationships between SII, NLR, MLR, and PLR with the bone mineral density (BMD) and risk of OP. RESULTS: Logistic regression analyses showed that SII, PLR, NLR, and MLR had independent negative associations with the OP risk. The ROC curve analysis showed that SII, NLR, and MLR predicted a low BMD, with NLR having the highest predictive value (area under the curve = 0.624). SII > 504.09, PLR > 131.87, NLR > 2.02, and MLR > 0.12 correlated with a particularly high OP risk. CONCLUSIONS: High levels of SII, PLR, NLR, and MLR were associated with a high OP risk. In particular, NLR > 2.02 strongly predicted the risk of OP, thereby representing a valuable and convenient inflammatory marker of the OP risk. [ABSTRACT FROM AUTHOR]

Published
2024

46. Observation of $J/\psi \rightarrow p\bar{p}a_{0}(980)$ at BESIII

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Bondarenko, O., Boyko, I., Braun, S., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cibinetto, G., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Fava, L., Felici, G., Feng, C. Q., Fioravanti, E., Fu, C. D., Fuks, O., Gao, Q., Gao, Y., Garzia, I., Geng, C., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, L. B., Guo, T., Guo, Y. P., Haddadi, Z., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, M., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, L., Huang, X. T., Huang, Y., Hussain, T., Ji, C. S., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Ke, B. C., Kloss, B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Leyhe, M., Li, C. H., Li, Cheng, Li, Cui, Li, D., Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, Q. J., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, K., Liu, K. Y., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, H. J., Lu, H. L., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Marcello, S., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ripka, M., Rong, G., Ruan, X. D., Santoro, V., Sarantsev, A., Savrié, M., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Werner, M., Wiedner, U., Wolke, M., Wu, L. H., Wu, N., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Xue, Z., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yu, S. P., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zang, S. L., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. B., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

Using $2.25\times10^{8}$ $J/\psi$ events collected with the BESIII detector at the BEPCII storage rings, we observe for the first time the process $J/\psi\rightarrow p\bar{p}a_{0}(980)$, $a_{0}(980)\rightarrow \pi^{0}\eta$ with a significance of $6.5\sigma$ ($3.2\sigma$ including systematic uncertainties). The product branching fraction of $J/\psi\rightarrow p\bar{p}a_{0}(980)\rightarrow p\bar{p}\pi^{0}\eta$ is measured to be $(6.8\pm1.2\pm1.3)\times 10^{-5}$, where the first error is statistical and the second is systematic. This measurement provides information on the $a_{0}$ production near threshold coupling to $p\bar{p}$ and improves the understanding of the dynamics of $J/\psi$ decays to four body processes., Comment: 8 pages, 7 figures

Published
2014
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49. Study of e$^+$e$^-$ $\rightarrow \text{p} \overline{\text{p}}\pi^0$ in the Vicinity of the $\psi\text{(3770)}$

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, J. V., Bertani, M., Bian, J. M., Boger, E., Bondarenko, O., Boyko, I., Braun, S., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., Ding, W. M., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Fava, L., Feng, C. Q., Fu, C. D., Fuks, O., Gao, Q., Gao, Y., Geng, C., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, A. Q., Guo, L. B., Guo, T., Guo, Y. P., Han, Y. L., Harris, F. A., He, K. L., He, M., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, L., Huang, X. T., Huang, Y., Hussain, T., Ji, C. S., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Kloss, B., Kopf, B., Kornicer, M., Kühn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Leyhe, M., Li, C. H., Li, Cheng, Li, Cui, Li, D., Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, K., Li, Lei, Li, P. R., Li, Q. J., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, K., Liu, K. Y., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, G. R., Lu, H. J., Lu, H. L., Lu, J. G., Lu, X. R., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Ma, F. C., Ma, H. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Q., N., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ripka, M., Rong, G., Ruan, X. D., Sarantsev, A., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Werner, M., Wiedner, U., Wolke, M., Wu, L. H., Wu, N., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Xue, Z., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yu, S. P., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zang, S. L., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. B., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, X. H., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

The process $e^+e^-\rightarrow p\overline{p}\pi^0$ has been studied by analyzing data collected at $\sqrt{s}=3.773$ GeV, at $\sqrt{s}=3.650$ GeV, and during a $\psi(3770)$ line shape scan with the BESIII detector at the BEPCII collider. The Born cross section of $p \overline{p} \pi^0$ in the vicinity of the $\psi(3770)$ is measured and the Born cross section of $\psi(3770)\rightarrow p \overline{p} \pi^0$ is extracted considering interference between resonant and continuum production amplitudes. Two solutions with the same probability and a significance of 1.5$\sigma$ are found, and the Born cross section of $\psi(3770)\rightarrow p \overline{p} \pi^0$ is determined to be less than 0.22 pb at 90% confidence level and $33.8\pm1.8\pm2.1$ pb, respectively. Using the estimated cross section and a constant decay amplitude approximation, the cross section $\sigma(p\overline{p} \rightarrow \psi(3770) \pi^0)$ is calculated for the kinematic situation of the planned $\overline{\text{P}}\text{ANDA}$ experiment. The maximum cross section corresponding to the two solutions is expected to be less than $0.79$ nb at 90% confidence level and $122\pm10$ nb at a center of mass energy of 5.26 GeV.

Published
2014
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50. Search for the radiative transitions $\psi(3770)\to\gamma\eta_c$ and $\gamma\eta_c(2S)$

Author

Ablikim, M., Achasov, M. N., Ai, X. C., Albayrak, O., Albrecht, M., Ambrose, D. J., An, F. F., An, Q., Bai, J. Z., Ferroli, R. Baldini, Ban, Y., Bennett, D. W., Bennett, J. V., Bertani, M., Bian, J. M., Boger, E., Bondarenko, O., Boyko, I., Braun, S., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X., Chen, X. R., Chen, Y. B., Cheng, H. P., Chu, X. K., Chu, Y. P., Cronin-Hennessy, D., Dai, H. L., Dai, J. P., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., Ding, W. M., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Fava, L., Feng, C. Q., Fu, C. D., Fuks, O., Gao, Q., Gao, Y., Geng, C., Goetzen, K., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guan, Y. H., Guo, L. B., Guo, T., Guo, Y. P., Haddadi, Z., Han, S., Han, Y. L., Harris, F. A., He, K. L., He, M., He, Z. Y., Held, T., Heng, Y. K., Hou, Z. L., Hu, C., Hu, H. M., Hu, J. F., Hu, T., Huang, G. M., Huang, G. S., Huang, H. P., Huang, J. S., Huang, L., Huang, X. T., Huang, Y., Hussain, T., Ji, C. S., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, L. L., Jiang, L. W., Jiang, X. S., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. L., Kang, X. S., Kavatsyuk, M., Kloss, B., Kopf, B., Kornicer, M., Kuehn, W., Kupsc, A., Lai, W., Lange, J. S., Lara, M., Larin, P., Leyhe, M., Li, C. H., Li, Cheng, Li, Cui, Li, D., Li, D. M., Li, F., Li, G., Li, H. B., Li, J. C., Li, Jin, Li, K., Li, P. R., Li, Q. J., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Lin, D. X., Liu, B. J., Liu, C. L., Liu, C. X., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. H., Liu, H. M., Liu, J., Liu, J. P., Liu, K., Liu, K. Y., Liu, P. L., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqiang, Liu, Zhiqing, Loehner, H., Lou, X. C., Lu, G. R., Lu, H. J., Lu, H. L., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lv, M., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, Q. M., Ma, S., Ma, T., Ma, X. Y., Maas, F. E., Maggiora, M., Malik, Q. A., Mao, Y. J., Mao, Z. P., Messchendorp, J. G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Moeini, H., Morales, C. Morales, Moriya, K., Muchnoi, N. Yu., Muramatsu, H., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pelizaeus, M., Peng, H. P., Peters, K., Ping, J. L., Ping, R. G., Poling, R., Qi, M., Qian, S., Qiao, C. F., Qin, L. Q., Qin, N., Qin, X. S., Qin, Y., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Ripka, M., Rong, G., Ruan, X. D., Sarantsev, A., Schoenning, K., Schumann, S., Shan, W., Shao, M., Shen, C. P., Shen, X. Y., Sheng, H. Y., Shepherd, M. R., Song, W. M., Song, X. Y., Spataro, S., Spruck, B., Sun, G. X., Sun, J. F., Sun, S. S., Sun, Y. J., Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tang, C. J., Tang, X., Tapan, I., Thorndike, E. H., Tiemens, M., Toth, D., Ullrich, M., Uman, I., Varner, G. S., Wang, B., Wang, D., Wang, D. Y., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, Q. J., Wang, S. G., Wang, W., Wang, X. F., Wang, Y. D., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. H., Wang, Z. Y., Wei, D. H., Wei, J. B., Weidenkaff, P., Wen, S. P., Werner, M., Wiedner, U., Wolke, M., Wu, L. H., Wu, N., Wu, Z., Xia, L. G., Xia, Y., Xiao, D., Xiao, Z. J., Xie, Y. G., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Xue, Z., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. X., Yang, L., Yang, Y., Yang, Y. X., Ye, H., Ye, M., Ye, M. H., Yu, B. X., Yu, C. X., Yu, H. W., Yu, J. S., Yu, S. P., Yuan, C. Z., Yuan, W. L., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zang, S. L., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C., Zhang, C. B., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J. J., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, S. H., Zhang, X. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, Q. W., Zhao, S. J., Zhao, T. C., Zhao, X. H., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Li, Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, K., Zhu, K. J., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.

Subjects
High Energy Physics - Experiment
Abstract

By using a 2.92 fb$^{-1}$ data sample taken at $\sqrt{s} = 3.773$ GeV with the BESIII detector operating at the BEPCII collider, we search for the radiative transitions $\psi(3770)\to\gamma\eta_c$ and $\gamma\eta_c(2S)$ through the hadronic decays $\eta_c(\eta_c(2S))\to K^0_SK^\pm\pi^\mp$. No significant excess of signal events above background is observed. We set upper limits at a 90% confidence level for the product branching fractions to be $\mathcal{B}(\psi(3770)\to\gamma\eta_c)\times \mathcal{B}(\eta_c\to K^0_SK^\pm\pi^\mp) < 1.6\times10^{-5}$ and $\mathcal{B}(\psi(3770)\to\gamma\eta_c(2S))\times \mathcal{B}(\eta_c(2S)\to K^0_SK^\pm\pi^\mp) < 5.6\times10^{-6}$. Combining our result with world-average values of $\mathcal{B}(\eta_c(\eta_c(2S))\to K^0_SK^\pm\pi^\mp)$, we find the branching fractions $\mathcal{B}(\psi(3770)\to\gamma\eta_c) < 6.8\times10^{-4}$ and $\mathcal{B}(\psi(3770)\to\gamma\eta_c(2S)) < 2.0\times10^{-3}$ at a 90% confidence level., Comment: 10 pages, 4 figures

Published
2014
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