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7,013 results on '"Lopez E"'

1. Probing a Magnetar Origin for the population of Extragalactic Fast X-ray Transients detected by Chandra

Author

Quirola-Vásquez, J., Bauer, F. E., Jonker, P. G., Brandt, W. N., Eappachen, D., Levan, A. J., Lopez, E., Luo, B., Ravasio, M. E., Sun, H., Xue, Y. Q., Yang, G., and Zheng, X. C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Twenty-two extragalactic fast X-ray transients (FXTs) have now been discovered from two decades of Chandra data (analyzing ~259 Ms of data), with 17 associated with distant galaxies (>100 Mpc). Different mechanisms and progenitors have been proposed to explain their properties; nevertheless, after analyzing their timing, spectral parameters, host-galaxy properties, luminosity function, and volumetric rates, their nature remains uncertain. We interpret a sub-sample of nine FXTs that show a plateau or a fast-rise light curve within the framework of a binary neutron star (BNS) merger magnetar model. We fit their light curves and derive magnetar (magnetic field and initial rotational period) and ejecta (ejecta mass and opacity) parameters. This model predicts two zones: an orientation-dependent free zone (where the magnetar spin-down X-ray photons escape freely to the observer) and a trapped zone (where the X-ray photons are initially obscured and only escape freely once the ejecta material becomes optically thin). We argue that six FXTs show properties consistent with the free zone and three FXTs with the trapped zone. This sub-sample of FXTs has a similar distribution of magnetic fields and initial rotation periods to those inferred for short gamma-ray bursts (SGRBs), suggesting a possible association. We compare the predicted ejecta emission fed by the magnetar emission (called merger-nova) to the optical and near-infrared upper limits of two FXTs, XRT 141001 and XRT 210423 where contemporaneous optical observations are available. The non-detections place lower limits on the redshifts of XRT 141001 and XRT 210423 of z>1.5 and >0.1, respectively. If the magnetar remnants lose energy via gravitational waves, it should be possible to detect similar objects with the current advanced LIGO detectors out to a redshift z<0.03, while future GW detectors will be able to detect them out to z=0.5., Comment: The paper was accepted for publication in Astronomy & Astrophysics

Published
2024

2. Improving graph-based detection of singular events for photochemical smog agents

Author

Carmona-Cabezas, R., Gomez-Gomez, J., de Rave, E. Gutierrez, Sanchez-Lopez, E., Serrano, J., and Jimenez-Hornero, F. J.

Subjects
Physics - Atmospheric and Oceanic Physics
Abstract

Recently, a set of graph-based tools have been introduced for the identification of singular events of O3, NO2 and temperature time series, as well as description of their dynamics. These are based on the use of the Visibility Graphs (VG). In this work, an improvement of the original approach is proposed, being called Upside-Down Visibility Graph (UDVG). It adds the possibility of investigating the singular lowest episodes, instead of the highest. Results confirm the applicability of the new method for describing the multifractal nature of the underlying O3, NO2, and temperature. Asymmetries in the NO2 degree distribution are observed, possibly due to the interaction with different chemicals. Furthermore, a comparison of VG and UDVG has been performed and the outcomes show that they describe opposite subsets of the time series (low and high values) as expected. The combination of the results from the two networks is proposed and evaluated, with the aim of obtaining all the information at once. It turns out to be a more complete tool for singularity detection in photochemical time series, which could be a valuable asset for future research., Comment: 35 pages, 7 figures

Published
2023
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3. Multifractal fluctuations of the precipitation in Spain (1960-2019)

Author

Gomez-Gomez, J., Carmona-Cabezas, R., Sanchez-Lopez, E., de Rave, E. Gutierrez, and Jimenez-Hornero, F. J.

Subjects
Physics - Atmospheric and Oceanic Physics
Abstract

In this work, an analysis of multifractal parameters of daily precipitation series over the Iberian Peninsula was performed in two 30-year periods to explore whether these properties follow any pattern. Fluctuations of precipitation series show three different scaling regions. Only two distinct regimes for small and large timescales can be confirmed, while intermediate scales are part of a transition region. It is also observed a certain degree of multifractality, which is higher for small timescales. At these scales, there is a high persistence which follows the spatial gradient of the annual precipitation. Moreover, multifractal parameters of the precipitation are modified according to complex spatial and temporal patterns. Only persistence uniformly decreases in the last period. Other relevant findings are the changes in the asymmetry of multifractal spectra in the eastern belt at larger timescales, which might be related to the change in the behavior of the Mediterranean cyclones., Comment: 12 pages, 8 figures

Published
2023
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4. The black widow pulsar J1641+8049 in the optical, radio and X-rays

Author

Kirichenko, A. Yu., Zharikov, S. V., Karpova, A. V., Fonseca, E., Zyuzin, D. A., Shibanov, Yu. A., López, E. A., Gilfanov, M. R., Cabrera-Lavers, A., Geier, S., Dong, F. A., Good, D. C., McKee, J. W., Meyers, B. W., Stairs, I. H., McLaughlin, M. A., and Swiggum, J. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

PSR J1641+8049 is a 2 ms black widow pulsar with the 2.2 h orbital period detected in the radio and $\gamma$-rays. We performed new phase-resolved multi-band photometry of PSR J1641+8049 using the OSIRIS instrument at the Gran Telescopio Canarias. The obtained data were analysed together with the new radio-timing observations from the Canadian Hydrogen Intensity Mapping Experiment (CHIME), the X-ray data from the Spectrum-RG/eROSITA all-sky survey, and all available optical photometric observations. An updated timing solution based on CHIME data is presented, which accounts for secular and periodic modulations in pulse dispersion. The system parameters obtained through the light curve analysis, including the distance to the source 4.6-4.8 kpc and the orbital inclination 56-59 deg, are found to be consistent with previous studies. However, the optical flux of the source at the maximum brightness phase faded by a factor of $\sim$2 as compared to previous observations. Nevertheless, the face of the J1641+8049 companion remains one of the most heated (8000-9500 K) by a pulsar among the known black widow pulsars. We also report a new estimation on the pulsar proper motion of $\approx$2 mas yr$^{-1}$, which yields a spin down luminosity of $\approx$4.87$\times 10^{34}$ ergs s$^{-1}$ and a corresponding heating efficiency of the companion by the pulsar of 0.3-0.7. The pulsar was not detected in X-rays implying its X-ray-luminosity was <3 $\times$ 10$^{31}$ erg s$^{-1}$ at the date of observations., Comment: Accepted for publication in MNRAS

Published
2023
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8. Broad-line Region Clouds orbiting an AGN sample

Author

Armijos-Abendaño, J., López, E., Llerena, M., and Logan, C. H. A.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a spectral and temporal analysis of XMM-Newton data from a sample of six galaxies (NGC 3783, Mrk 279, Mrk 766, NGC 3227, NGC 7314, and NGC 3516). Using the hardness-ratio curves, we identify time-intervals in which clouds are eclipsing the central X-ray source in five of the six sources. We detect three occultations in NGC 3227 and one occultation in NGC 3783, NGC 7314, and NGC 3516, together with the well-known occultations in Mrk 766. We estimate the physical properties of the eclipsing clouds. The derived physical size of the X-ray sources ($\sim$(3-28)$\times$10$^{13}$ cm) is less than that of the eclipsing clouds with column densities of $\sim$10$^{22}$-10$^{23}$ cm$^{-2}$, thus a single cloud may block the X-ray source, leading to notorious temporal variability of the X-ray flux. The eclipsing clouds in Mrk 766, NGC 3227, NGC 7314, and NGC 3516 with distances from the X-ray source of $\sim$(0.3-3.6)$\times$10$^4$ $R_g$ are moving at Keplerian velocities $>$1122 km s$^{-1}$, typical parameters of broad-line region clouds, while the eclipsing cloud in NGC 3783 is likely located in the dusty torus. We also find a good anti-correlation with a slope of -187$\pm$62 between the known masses of the supermassive black hole in the center of the galaxies with the equivalent width (EW) of the 6.4 keV Fe line for the five Seyfert 1 galaxies of our sample, while the Seyfert 2 galaxy NGC 7314 shows an average EW value of 100$\pm$11 eV inconsistent with the above anti-correlation., Comment: 13 pages, 15 figures, accepted for publication in MNRAS

Published
2022
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11. First Proof-of-Concept Prototype of an Additive-Manufactured Radio Frequency Quadrupole

Author

Torims, T., Pikurs, G., Gruber, S., Vretenar, M., Ratkus, A., Vedani, M., Lopez, E., and Bruckner, F.

Subjects
Physics - Accelerator Physics
Abstract

Continuous developments in Additive Manufacturing (AM) technologies are opening opportunities in novel machining, and improving design alternatives for modern particle accelerator components. One of the most critical, complex, and delicate accelerator elements to manufacture and assemble is the Radio Frequency Quadrupole (RFQ) linear accelerator, used as an injector for all large modern proton and ion accelerator systems. For this reason, the RFQ has been selected by a wide European collaboration participating in the AM developments of the I.FAST (Innovation Fostering in Accelerator Science and Technology) Horizon 2020 project. RFQ is as an excellent candidate to show how sophisticated pure-copper accelerator components can be manufactured by AM and how their functionalities can be boosted by this evolving technology. To show the feasibility of the AM process, a prototype RFQ section has been designed, corresponding to one-quarter of a 750 MHz 4-vane RFQ, which was optimised for production with state-of-art Laser Powder Bed Fusion (L-PBF) technology, and then manufactured in pure copper. To the best knowledge of the authors, this is the first RFQ section manufactured in the world by AM. Subsequently, geometrical precision and surface roughness of the prototype were measured. The results obtained are encouraging and confirm the feasibility of AM manufactured high-tech accelerator components. It has been also confirmed that the RFQ geometry, in particular the critical electrode modulation and the complex cooling channels, can be successfully realised thanks to the opportunities provided by the AM technology. Further prototypes will aim to improve surface roughness and to test vacuum properties. In parallel, laboratory measurements will start to test and improve the voltage holding properties of AM manufactured electrode samples.

Published
2021

19. DEVELOPMENT AND CHARACTERIZATION OF AN OPTIMIZED NOVEL DRINK FROM THREE VARIETIES OF SPROUTED QUINOA

Author

Bendezu-Ccanto, J., Contreras-Lopez, E., and Lozada-Urbano, M.

Subjects
Beverages -- Product development -- Nutritional aspects, Quinoa -- Usage -- Varieties -- Nutritional aspects, Agricultural industry, Food/cooking/nutrition, Health
Abstract

Sprouted products are a food alternative that contribute to improving human nutrition. Quinoa has a large amount of natural antioxidants. The dry and hard grains when they undergo a germination process change to tender and slightly acidic sprouts that contain amino acids, minerals, vitamins, enzymes that help digestion and antioxidants. Furthermore, sprouted quinoa has a high protein content and a low concentration of saponins. Previous studies have shown that sprouted quinoa has shown an increase in protein, calcium and ascorbic acid content. Quinoa sprouts improve the organoleptic characteristics of quinoa grains; few studies have used sprouted quinoa in the preparation of beverages. The objective of this study was to prepare a beverage based on sprouted quinoa using a simplex lattice mix design to determine the optimal formula. Three varieties of sprouted quinoa were used: white (Salcedo INIA), red (INIA-415 Pasankalla), and black (INIA 420-Negra Collana). The quinoa was incubated at 30[degrees]C in the dark for 48 hours at a relative humidity of 98%. Ten treatments with different proportions of the three types of sprouted quinoa were used. The antioxidant capacity and consumer satisfaction of the ten treatments were evaluated. The ABTS method was used to measure the antioxidant capacity of each treatment. The optimal drink mix was composed of 81.67% sprouted black quinoa, 18.33% sprouted white quinoa, and 0% sprouted red quinoa. Furthermore, the consumer acceptability results were similar across all treatments (p>0.05). A nutritional analysis revealed significant differences (p Key words: Sprouts, Chenopodium quinoa, ABTS, Design-expert, Mixture design, antioxidant capacity, acceptability, INTRODUCTION Quinoa (Chenopodium quinoa Willd) belongs to the Amarantaceae family and is considered an Andean grain cultivated in the Andes region spanning Peru and Bolivia. Its adaptability to diverse environments, [...]

Published
2023
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22. Satellite data for the offshore renewable energy sector: synergies and innovation opportunities

Author

Medina-Lopez, E., McMillan, D., Lazic, J., Hart, E., Zen, S., Angeloudis, A., Bannon, E., Browell, J., Dorling, S., Dorrell, R. M., Forster, R., Old, C., Payne, G. S., Porter, G., Rabaneda, A. S., Sellar, B., Tapoglou, E., Trifonova, N., Woodhouse, I. H., and Zampollo, A.

Subjects
Physics - Geophysics, Physics - Atmospheric and Oceanic Physics
Abstract

Can satellite data be used to address challenges currently faced by the Offshore Renewable Energy (ORE) sector? What benefit can satellite observations bring to resource assessment and maintenance of ORE farms? Can satellite observations be used to assess the environmental impact of offshore renewables leading towards a more sustainable ORE sector? This review paper faces these questions presenting a holistic view of the current interactions between satellite and ORE sectors, and future needs to make this partnerships grow. The aim of the work is to start the conversation between these sectors by establishing a common ground. We present offshore needs and satellite technology limitations, as well as potential opportunities and areas of growth. To better understand this, the reader is guided through the history, current developments, challenges and future of offshore wind, tidal and wave energy technologies. Then, an overview on satellite observations for ocean applications is given, covering types of instruments and how they are used to provide different metocean variables, satellite performance, and data processing and integration. Past, present and future satellite missions are also discussed. Finally, the paper focuses on innovation opportunities and the potential of synergies between the ORE and satellite sectors. Specifically, we pay attention to improvements that satellite observations could bring to standard measurement techniques: assessing uncertainty, wind, tidal and wave conditions forecast, as well as environmental monitoring from space. Satellite-enabled measurement of ocean physical processes and applications for fisheries, mammals and birds, and habitat change, are also discussed in depth., Comment: Review paper, 53 pages, 19 figures

Published
2021
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23. Tensile Properties of Inconel 718 Produced by LMD-Wire

Author

Cormier, J., Cabeza, S., Burlot, G., Bordas, R., Bordas-Czaplicki, M., Machado Alves da Fonseca, F., Polenz, S., Marquardt, F., Lopez, E., Villechaise, P., Ott, Eric A., editor, Andersson, Joel, editor, Sudbrack, Chantal, editor, Bi, Zhongnan, editor, Bockenstedt, Kevin, editor, Dempster, Ian, editor, Fahrmann, Michael, editor, Jablonski, Paul, editor, Kirka, Michael, editor, Liu, Xingbo, editor, Nagahama, Daisuke, editor, Smith, Tim, editor, Stockinger, Martin, editor, and Wessman, Andrew, editor

Published
2023
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27. An accelerator facility for intermediate energy proton irradiation and testing of nuclear materials

Author

Jepeal, S. J., Danagoulian, A., Kesler, L. A., Korsun, D. A., Lee, H. Y., Schwartz, N., Sorbom, B. N., Lopez, E. Velez, and Hartwig, Z. S.

Subjects
Condensed Matter - Materials Science
Abstract

The bulk irradiation of materials with 10-30 MeV protons promises to advance the study of radiation damage for fission and fusion power plants. Intermediate energy proton beams can now be dedicated to materials irradiation within university-scale laboratories. This paper describes the first such facility, with an Ionetix ION-12SC cyclotron producing 12 MeV proton beams. Samples are mm-scale tensile specimens with thicknesses up to 300 um, mounted to a cooled beam target with control over temperature. A specialized tensile tester for radioactive specimens at high temperature (500+ {\deg}C) and/or vacuum represents the conditions in fission and fusion systems, while a digital image correlation system remotely measures strain. Overall, the facility provides university-scale irradiation and testing capability with intermediate energy protons to complement traditional in-core fission reactor and micro-scale ion irradiation. This facility demonstrates that bulk proton irradiation is a scalable and effective approach for nuclear materials research, down-selection, and qualification., Comment: Submitted to NIM B journal

Published
2020
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28. Vassiliev Invariants for Flows Via Chern-Simons Perturbation Theory

Author

de-la-Cruz-Moreno, J., García-Compeán, H., and López, E.

Subjects
High Energy Physics - Theory, Mathematical Physics
Abstract

The perturbative expansion of Chern-Simons gauge theory leads to invariants of knots and links, the finite type invariants or Vassiliev invariants. It has been proven that at any order in perturbation theory the resulting expression is an invariant of that order. Bott-Taubes integrals on configuration spaces are introduced in the present context to write Feynman diagrams at a given order in perturbation theory in a geometrical and topological setting. One of the consequences of the configuration space formalism is that the resulting amplitudes are given in cohomological terms. This cohomological structure can be used to translate Bott-Taubes integrals into Chern-Simons perturbative amplitudes and vice versa. In this article this program is performed up to third order in the coupling constant. This expands some work previously worked out by Thurston. Finally we take advantage of these results to incorporate in the formalism a smooth and divergenceless vector field on the $3$-manifold. The Bott-Taubes integrals obtained are used for constructing higher-order asymptotic Vassiliev invariants extending the work of Komendarczyk and Voli\'c., Comment: 54 pages, 21 figures, 3 appendices

Published
2020
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29. On the effects of UV photons/X-rays on the chemistry of the Sgr B2 cloud

Author

Armijos-Abendaño, J., Martín-Pintado, J., López, E., Llerena, M., Harada, N., Requena-Torres, M. A., Martín, S., Rivilla, V. M., Riquelme, D., and Aldas, F.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The lines of HOC$^+$, HCO and CO$^+$ are considered good tracers of photon-dominated regions (PDRs) and X-ray dominated regions. We study these tracers towards regions of the Sgr B2 cloud selected to be affected by different heating mechanisms. We find the lowest values of the column density ratios of HCO$^+$ versus HOC$^+$, HCO and CO$^+$ in dense HII gas, where UV photons dominate the heating and chemistry of gas. HOC$^+$, HCO and CO$^+$ abundances and the above ratios are compared with those of chemical modeling, finding that high temperature chemistry, a cosmic-ray ionization rate of 10$^{-16}$ s$^{-1}$ and timescales $>$10$^{5.0}$ years explain well the HOC$^+$ abundances in quiescent Sgr B2 regions, while shocks are also needed to explain the highest HCO abundances derived for these regions. CO$^+$ is mainly formed in PDRs since the highest CO$^+$ abundances of $\sim$(6-10)$\times$10$^{-10}$ are found in HII regions with electron densities $>$540 cm$^{-3}$ and that CO$^+$ emission is undetected in quiescent gas. Between the ratios, the HCO$^+$/HCO ratio is sensitive to the electron density as it shows different values in dense and diffuse HII regions. We compare SiO J=2-1 emission maps of Sgr B2 with X-ray maps from 2004 and 2012. One known spot shown on the 2012 X-ray map is likely associated with molecular gas at velocities of 15-25 km s$^{-1}$. We also derive the X-ray ionization rate of $\sim$10$^{-19}$ s$^{-1}$ for Sgr B2 regions pervaded by X-rays in 2004, which is quite low to affect the chemistry of the molecular gas.

Published
2020
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30. Precise mass and radius of a transiting super-Earth planet orbiting the M dwarf TOI-1235: a planet in the radius gap?

Author

Bluhm, P., Luque, R., Espinoza, N., Palle, E., Caballero, J. A., Dreizler, S., Livingston, J. H., Mathur, S., Quirrenbach, A., Stock, S., Van Eylen, V., Nowak, G., Lopez, E., Csizmadia, Sz., Osorio, M. R. Zapatero, Schoefer, P., Lillo-Box, J., Oshagh, M., Amado, P. J., Barrado, D., Bejar, V. J. S., Cale, B., Chaturvedi, P., Cifuentes, C., Cochran, W. D., Collins, K. A., Collins, K. I., Cortes-Contreras, M., Alonso, E. Diez, Mufti, M. El, Ercolino, A., Fridlund, M., Gaidos, E., Garcia, R. A., Gonzalez-Alvarez, E., Gonzalez-Cuesta, L., Guerra, P., Hatzes, A. P., Henning, T., Herrero, E., Hidalgo, D., Isopi, G., Jeffers, S. V., Jenkins, J. M., Jensen, E. L. N., Kabath, P., Kemmer, J., Korth, J., Kossakowski, D., Kuerster, M., Lafarga, M., Mallia, F., Montes, D., Morales, J. C., Morales-Calderon, M., Murgas, F., Narita, N., Plavchan, P., Passegger, V. M., Pedraz, S., Rauer, H., Redfield, S., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rodriguez-Lopez, C., Santos, A. R. G., Seager, S., Shan, Y., Schlecker, M., Schweitzer, A., Soto, M. G., Subjak, J., Tal-Or, L., Trifonov, T., Vanaverbeke, S., Vanderspek, R., Wittrock, J., Zechmeister, M., and Zohrabi, F.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We report the confirmation of a transiting planet around the bright, inactive M0.5 V star TOI-1235 (TYC 4384-1735-1, V = 11.5 mag), whose transit signal was detected in the photometric time series of Sectors 14, 20, and 21 of the TESS space mission. We confirm the planetary nature of the transit signal, which has a period of 3.44 d, by using precise radial velocity measurements with CARMENES and HARPS-N spectrographs. A comparison of the properties derived for TOI-1235 b's with theoretical models reveals that the planet has a rocky composition, with a bulk density slightly higher than Earth's. In particular, we measure a mass of M_p = 5.9+/-0.6 M_Earth and a radius of R_p = 1.69+/-0.08 R_Earth, which together result in a density of rho_p = 6.7+1.3-1.1 g/cm3. When compared with other well-characterized exoplanetary systems, the particular combination of planetary radius and mass puts our discovery in the radius gap, a transition region between rocky planets and planets with significant atmospheric envelopes, with few known members. While the exact location of the radius gap for M dwarfs is still a matter of debate, our results constrain it to be located at around 1.7 R_Earth or larger at the insolation levels received by TOI-1235 b (~60 S_Earth), which makes it an extremely interesting object for further studies of planet formation and atmospheric evolution., Comment: A&A, in press

Published
2020
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31. Casimir effect in polymer scalar field theory

Author

Escobar, C. A., Chan-López, E., and Martín-Ruiz, A.

Subjects
High Energy Physics - Phenomenology
Abstract

In this paper, we study the Casimir effect in the classical geometry of two parallel conducting plates, separated by a distance $L$, due to the presence of a minimal length $\lambda$ arising from a background independent (polymer) quantization scheme. To this end, we polymer-quantize the classical Klein-Gordon Hamiltonian for a massive scalar field confined between the plates and obtain the energy spectrum. The minimal length scale of the theory introduces a natural cutoff for the momenta in the plane parallel to the plates and a maximum number of discrete modes between the plates. The zero-point energy is calculated by summing over the modes, and by assuming $\lambda \ll L$, we expressed it as an expansion in powers of $1/N$, being $N=L/ \lambda$ the number of points between the plates. Closed analytical expressions are obtained for the Casimir energy in the cases of small and large scalar mass limits., Comment: Accepted for publication in Physical Review D

Published
2020
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32. Searching for optical companions to four binary millisecond pulsars with the Gran Telescopio Canarias

Author

Kirichenko, A. Yu., Karpova, A. V., Zyuzin, D. A., Zharikov, S. V., Lopez, E. A., Shibanov, Yu. A., Freire, P. C. C., Fonseca, E., and Cabrera-Lavers, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on multi-band photometric observations of four binary millisecond pulsars with the Gran Telescopio Canarias. The observations led to detection of binary companions to PSRs J1630+3734, J1741+1351 and J2042+0246 in the Sloan g', r' and i' bands. Their magnitudes in the r' band are $\approx$24.4, 24.4 and 24.0, respectively. We also set a 3$\sigma$ upper limit on the brightness of the PSR J0557+1550 companion in the r' band of $\approx$25.6 mag. Combining the optical data with the radio timing measurements and white dwarf cooling models, we show that the detected companions are cool low-mass white dwarfs with temperatures and ages in the respective ranges of (4-7)$\times 10^3$ K and 2-5 Gyr. All the detected white dwarfs are found to likely have either pure hydrogen or mixed helium-hydrogen atmospheres., Comment: Accepted for publication in MNRAS

Published
2020
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41. The impact of stripped cores on the frequency of Earth-size planets in the habitable zone

Author

Pascucci, I., Mulders, G., and Lopez, E.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The frequency of Earth-size planets in the habitable zone of Sun-like stars, hereafter $\eta_\oplus$, is a key parameter to evaluate the yield of nearby Earth analogues that can be detected and characterized by future missions. Yet, this value is poorly constrained as there are no reliable exoplanet candidates in the habitable zone of Sun-like stars in the Kepler field. Here, we show that extrapolations relying on the population of small ($< 1.8\,R_\oplus$) short-period ($< 25\,$days) planets bias $\eta_\oplus$ to large values. As the radius distribution at short orbital periods is strongly affected by atmospheric loss, we re-evaluate $\eta_\oplus$ using exoplanets at larger separations. We find that $\eta_\oplus$ drops considerably, to values of only $\sim 5-10$%. Observations of young ($< 100$ Myr) clusters can probe short-period sub-Neptunes that still retain most of their envelope mass. As such, they can be used to quantify the contamination of sub-Neptunes to the population of Kepler short-period small planets and aid in more reliable estimates of $\eta_\oplus$.

Published
2019
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43. A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

Author

Fontanive, C., Rice, K., Bonavita, M., Lopez, E., Muzic, K., and Biller, B.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Stellar multiplicity is believed to influence planetary formation and evolution, although the precise nature and extent of this role remain ambiguous. We present a study aimed at testing the role of stellar multiplicity in the formation and/or evolution of the most massive, close-in planetary and substellar companions. Using direct imaging observations, as well as the Gaia DR2 catalogue, we searched for wide binary companions to 38 stars hosting massive giant planets or brown dwarfs (M > 7 MJup) on orbits shorter than ~1 AU. We report the discovery of a new component in the WASP-14 system, and present an independent confirmation of a comoving companion to WASP-18. From a robust Bayesian statistical analysis, we derived a binary fraction of 79.0+13.2-14.7% between 20-10,000 AU for our sample, twice as high as for field stars with a 3-{\sigma} significance. This binary frequency was found to be larger than for lower-mass planets on similar orbits, and we observed a marginally higher binary rate for inner companions with periods shorter than 10 days. These results demonstrate that stellar companions greatly influence the formation and/or evolution of these systems, suggesting that the role played by binary companions becomes more important for higher-mass planets, and that this trend may be enhanced for systems with tighter orbits. Our analysis also revealed a peak in binary separation at 250 AU, highlighting a shortfall of close binaries among our sample. This indicates that the mechanisms affecting planet and brown dwarf formation or evolution in binaries must operate from wide separations, although we found that the Kozai-Lidov mechanism is unlikely to be the dominant underlying process. We conclude that binarity plays a crucial role in the existence of very massive short-period giant planets and brown dwarf desert inhabitants, which are almost exclusively observed in multiple systems., Comment: Accepted for publication in MNRAS. 30 pages, 20 figures. Updated to include proof corrections

Published
2019
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44. Toward Complete Characterization: Prospects for Directly Imaging Transiting Exoplanets

Author

Stark, CC, Dressing, C, Dulz, S, Lopez, E, Marley, MS, Plavchan, P, and Sahlmann, J

Subjects
Exoplanet detection methods, Exoplanets, Transits, Direct imaging, Coronagraphic imaging, Radial velocity, Astrometric exoplanet detection, Space telescopes, astro-ph.EP, astro-ph.IM, astro-ph.SR, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

High-contrast direct imaging of exoplanets can provide many important observables, including measurements of the orbit, spectra that probe the lower layers of the atmosphere, and phase variations of the planet, but cannot directly measure planet radius or mass. Our future understanding of directly imaged exoplanets will therefore rely on extrapolated models of planetary atmospheres and bulk composition, which need robust calibration. We estimate the population of extrasolar planets that could serve as calibrators for these models. Critically, this population of "standard planets" must be accessible to both direct imaging and the transit method, allowing for radius measurement. We show that the search volume of a direct imaging mission eventually overcomes the transit probability falloff with semimajor axis, so that as long as cold planets are not exceedingly rare, the population of transiting planets and directly imageable planets overlaps. Using current extrapolations of Kepler occurrence rates, we estimate that ∼8 standard planets could be characterized shortward of 800 nm with an ambitious future direct imaging mission like LUVOIR-A and several dozen could be detected at the V band. We show the design space that would expand the sample size and discuss the extent to which ground-and space-based surveys could detect this small but crucial population of planets.

Published
2020

45. Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets

Author

Rice, K., Malavolta, L., Mayo, A., Mortier, A., Buchhave, L. A., Affer, L., Vanderburg, A., Lopez-Morales, M., Poretti, E., Zeng, L., Cameron, A. C., Damasso, M., Coffinet, A., Latham, D. W., Bonomo, A. S., Bouchy, F., Charbonneau, D., Dumusque, X., Figueira, P., Fiorenzano, A. F. Martinez, Haywood, R. D., Johnson, J. Asher, Lopez, E., Lovis, C., Mayor, M., Micela, G., Molinari, E., Nascimbeni, V., Nava, C., Pepe, F., Phillips, D. F., Piotto, G., Sasselov, D., Ségransan, D., Sozzetti, A., Udry, S., and Watson, C.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Super-Earths belong to a class of planet not found in the Solar System, but which appear common in the Galaxy. Given that some super-Earths are rocky, while others retain substantial atmospheres, their study can provide clues as to the formation of both rocky planets and gaseous planets, and - in particular - they can help to constrain the role of photo-evaporation in sculpting the exoplanet population. GJ 9827 is a system already known to host 3 super-Earths with orbital periods of 1.2, 3.6 and 6.2 days. Here we use new HARPS-N radial velocity measurements, together with previously published radial velocities, to better constrain the properties of the GJ 9827 planets. Our analysis can't place a strong constraint on the mass of GJ 9827 c, but does indicate that GJ 9827 b is rocky with a composition that is probably similar to that of the Earth, while GJ 9827 d almost certainly retains a volatile envelope. Therefore, GJ 9827 hosts planets on either side of the radius gap that appears to divide super-Earths into pre-dominantly rocky ones that have radii below $\sim 1.5 R_\oplus$, and ones that still retain a substantial atmosphere and/or volatile components, and have radii above $\sim 2 R_\oplus$. That the less heavily irradiated of the 3 planets still retains an atmosphere, may indicate that photoevaporation has played a key role in the evolution of the planets in this system., Comment: 16 pages, 9 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2018
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47. Goodbye Hartmann trial: a prospective, international, multicenter, observational study on the current use of a surgical procedure developed a century ago

Author

Perrone, G, Giuffrida, M, Abu-Zidan, F, Kruger, V, Livrini, M, Petracca, G, Rossi, G, Tarasconi, A, Tian, B, Bonati, E, Mentz, R, Mazzini, F, Campana, J, Gasser, E, Kafka-Ritsch, R, Felsenreich, D, Dawoud, C, Riss, S, Gomes, C, Gomes, F, Gonzaga, R, Canton, C, Pereira, B, Fraga, G, Zem, L, Cordeiro-Fonseca, V, de Mesquita Tauil, R, Atanasov, B, Belev, N, Kovachev, N, Melendez, L, Dimova, A, Dimov, S, Zelic, Z, Augustin, G, Bogdanic, B, Moric, T, Chouillard, E, Bajul, M, De Simone, B, Panis, Y, Esposito, F, Notarnicola, M, Lauka, L, Fabbri, A, Hentati, H, Fnaiech, I, Aurelien, V, Bougard, M, Roulet, M, Demetrashvili, Z, Pipia, I, Merabishvili, G, Bouliaris, K, Koukoulis, G, Doudakmanis, C, Xenaki, S, Chrysos, E, Kokkinakis, S, Vassiliu, P, Michalopoulos, N, Margaris, I, Kechagias, A, Avgerinos, K, Katunin, J, Lostoridis, E, Nagorni, E, Pujante, A, Mulita, F, Maroulis, I, Vailas, M, Marinis, A, Siannis, I, Bourbouteli, E, Manatakis, D, Tasis, N, Acheimastos, V, Maria, S, Stylianos, K, Kuzeridis, H, Korkolis, D, Fradelos, E, Kavalieratos, G, Petropoulou, T, Polydorou, A, Papacostantinou, I, Triantafyllou, T, Kimpizi, D, Theodorou, D, Toutouzas, K, Chamzin, A, Frountzas, M, Schizas, D, Karavokyros, I, Syllaios, A, Charalabopoulos, A, Boura, M, Baili, E, Ioannidis, O, Loutzidou, L, Anestiadou, E, Tsouknidas, I, Petrakis, G, Polenta, E, Bains, L, Gupta, R, Singh, S, Khanduri, A, Bala, M, Kedar, A, Pisano, M, Podda, M, Pisanu, A, Martines, G, Trigiante, G, Lantone, G, Agrusa, A, Di Buono, G, Buscemi, S, Veroux, M, Gioco, R, Veroux, G, Oragano, L, Zonta, S, Lovisetto, F, Feo, C, Pesce, A, Fabbri, N, Marino, F, Perrone, F, Vincenti, L, Papagni, V, Picciariello, A, Rossi, S, Picardi, B, Del Monte, S, Visconti, D, Osella, G, Petruzzelli, L, Pignata, G, Andreuccetti, J, D'Alessio, R, Buonfantino, M, Guaitoli, E, Spinelli, S, Sampietro, G, Corbellini, C, Lorusso, L, Frontali, A, Pezzoli, I, Bonomi, A, Chierici, A, Cotsoglou, C, Manca, G, Delvecchio, A, Musa, N, Casati, M, Letizia, L, Abate, E, Ercolani, G, D'Acapito, F, Solaini, L, Guercioni, G, Cicconi, S, Sasia, D, Borghi, F, Giraudo, G, Sena, G, Castaldo, P, Cardamone, E, Portale, G, Zuin, M, Spolverato, Y, Esposito, M, Isernia, R, Di Salvo, M, Manunza, R, Esposito, G, Agus, M, Asti, E, Bernardi, D, Tonucci, T, Luppi, D, Casadei, M, Bonilauri, S, Pezzolla, A, Panebianco, A, Laforgia, R, De Luca, M, Zese, M, Parini, D, Jovine, E, De Sario, G, Lombardi, R, Aprea, G, Palomba, G, Capuano, M, Argenio, G, Orio, G, Armellino, M, Troian, M, Guerra, M, Nagliati, C, Biloslavo, A, Germani, P, Aizza, G, Monsellato, I, Chahrour, A, Anania, G, Bombardini, C, Bagolini, F, Sganga, G, Fransvea, P, Bianchi, V, Boati, P, Ferrara, F, Palmieri, F, Cianci, P, Gattulli, D, Restini, E, Cillara, N, Cannavera, A, Nita, G, Sarnari, J, Roscio, F, Clerici, F, Scandroglio, I, Berti, S, Cadeo, A, Filippelli, A, Conti, L, Grassi, C, Cattaneo, G, Pighin, M, Papis, D, Gambino, G, Bertino, V, Schifano, D, Prando, D, Fogato, L, Cavallo, F, Ansaloni, L, Picheo, R, Pontarolo, N, Depalma, N, Spampinato, M, D'Ugo, S, Lepre, L, Capponi, M, Campa, R, Sarro, G, Dinuzzi, V, Olmi, S, Uccelli, M, Ferrari, D, Inama, M, Moretto, G, Fontana, M, Favi, F, Picariello, E, Rampini, A, Barberis, A, Azzinnaro, A, Oliva, A, Totaro, L, Benzoni, I, Ranieri, V, Capolupo, G, Carannante, F, Caricato, M, Ronconi, M, Casiraghi, S, Casole, G, Pantalone, D, Alemanno, G, Scheiterle, M, Ceresoli, M, Cereda, M, Fumagalli, C, Zanzi, F, Bolzon, S, Guerra, E, Lecchi, F, Cellerino, P, Ardito, A, Scaramuzzo, R, Balla, A, Lepiane, P, Tartaglia, N, Ambrosi, A, Pavone, G, Palini, G, Veneroni, S, Garulli, G, Ricci, C, Torre, B, Russo, I, Rottoli, M, Tanzanu, M, Belvedere, A, Milone, M, Manigrasso, M, De Palma, G, Piccoli, M, Pattacini, G, Magnone, S, Bertoli, P, Massucco, P, Palisi, M, Luzzi, A, Fleres, F, Clarizia, G, Spolini, A, Kobe, Y, Toma, T, Shimamura, F, Parker, R, Ranketi, S, Mitei, M, Svagzdys, S, Pauzas, H, Zilinskas, J, Poskus, T, Kryzauskas, M, Jakubauskas, M, Zakaria, A, Zakaria, Z, Wong, M, Jusoh, A, Zakaria, M, Cruz, D, Elizalde, A, Reynaud, A, Hernandez, E, Monroy, J, Hinojosa-Ugarte, D, Quiodettis, M, Du Bois, M, Latorraca, J, Major, P, Pedziwiatr, M, Pisarska-Adamczyk, M, Waledziak, M, Kwiatkowski, A, Czyzykowski, L, da Costa, S, Ferreira, A, Almeida, F, Rocha, R, Carneiro, C, Perez, D, Carvas, J, Rocha, C, Ferreira, C, Marques, R, Fernandes, U, Leao, P, Goulart, A, Pereira, R, Patrocinio, S, de Mendonca, N, Manso, M, Morais, H, Cardoso, P, Calu, V, Miron, A, Toma, E, Gachabayov, M, Abdullaev, A, Litvin, A, Nechay, T, Tyagunov, A, Yuldashev, A, Bradley, A, Wilson, M, Panyko, A, Lateckova, Z, Lacko, V, Lesko, D, Soltes, M, Radonak, J, Turrado-Rodriguez, V, Termes-Serra, R, Morales-Sevillano, X, Lapolla, P, Mingoli, A, Brachini, G, Degiuli, M, Sofia, S, Reddavid, R, de Manzoni Garberini, A, Buffone, A, del Pozo, E, Aparicio-Sanchez, D, Dos Barbeito, S, Estaire-Gomez, M, Viton-Herrero, R, de los Angeles Gil Olarte-Marquez, M, Gil-Martinez, J, Alconchel, F, Nicolas-Lopez, T, Rahy-Martin, A, Pelloni, M, Banolas-Suarez, R, Mendoza-Moreno, F, Nisa, F, Diez-Alonso, M, Rodas, M, Agundez, M, Andres, M, Moreira, C, Perez, A, Ponce, I, Gonzalez-Castillo, A, Membrilla-Fernandez, E, Salvans, S, Serradilla-Martin, M, Pardo, P, Rivera-Alonso, D, Dziakova, J, Huguet, J, Valle, N, Ruiz, E, Valcarcel, C, Moreno, C, Salazar, Y, Garcia, J, Mico, S, Lopez, J, Farre, S, Gomez, M, Petit, N, Titos-Garcia, A, Aranda-Narvaez, J, Romacho-Lopez, L, Sanchez-Guillen, L, Aranaz-Ostariz, V, Bosch-Ramirez, M, Martinez-Perez, A, Martinez-Lopez, E, Sebastian-Tomas, J, Jimenez-Riera, G, Jimenez-Vega, J, Cuellar, J, Campos-Serra, A, Munoz-Campana, A, Gracia-Roman, R, Alegre, J, Pinto, F, O'Sullivan, S, Antona, F, Jimenez, B, Lopez-Sanchez, J, Carmona, Z, Fernandez, R, Sierra, I, de Leon, L, Moreno, V, Iglesias, E, Cumplido, P, Bravo, A, Simo, I, Dominguez, C, Caamano, A, Lozano, R, Martinez, M, Torres, A, de Quiros, J, Pellino, G, Cloquell, M, Moller, E, Jalal-Eldin, S, Abdoun, A, Hamid, H, Lohsiriwat, V, Mongkhonsupphawan, A, Baraket, O, Ayed, K, Abbassi, I, Ali, A, Ammar, H, Kchaou, A, Tlili, A, Zribi, I, Colak, E, Polat, S, Koylu, Z, Guner, A, Usta, M, Reis, M, Mantoglu, B, Gonullu, E, Akin, E, Altintoprak, F, Bayhan, Z, Firat, N, Isik, A, Memis, U, Bayrak, M, Altintas, Y, Kara, Y, Bozkurt, M, Kocatas, A, Das, K, Seker, A, Ozer, N, Atici, S, Tuncer, K, Kaya, T, Ozkan, Z, Ilhan, O, Agackiran, I, Uzunoglu, M, Demirbas, E, Altinel, Y, Meric, S, Hacim, N, Uymaz, D, Omarov, N, Balik, E, Tebala, G, Khalil, H, Rana, M, Khan, M, Florence, C, Swaminathan, C, Leo, C, Liasis, L, Watfah, J, Trostchansky, I, Delgado, E, Pontillo, M, Latifi, R, Coimbra, R, Edwards, S, Lopez, A, Velmahos, G, Dorken, A, Gebran, A, Palmer, A, Oury, J, Bardes, J, Seng, S, Coffua, L, Ratnasekera, A, Egodage, T, Echeverria-Rosario, K, Armento, I, Napolitano, L, Sangji, N, Hemmila, M, Quick, J, Austin, T, Hyman, T, Curtiss, W, Mcclure, A, Cairl, N, Biffl, W, Truong, H, Schaffer, K, Reames, S, Banchini, F, Capelli, P, Coccolini, F, Sartelli, M, Bravi, F, Vallicelli, C, Agnoletti, V, Baiocchi, G, Catena, F, Perrone G., Giuffrida M., Abu-Zidan F., Kruger V. F., Livrini M., Petracca G. L., Rossi G., Tarasconi A., Tian B. W. C. A., Bonati E., Mentz R., Mazzini F. N., Campana J. P., Gasser E., Kafka-Ritsch R., Felsenreich D. M., Dawoud C., Riss S., Gomes C. A., Gomes F. C., Gonzaga R. A. T., Canton C. A. B., Pereira B. M., Fraga G. P., Zem L. G., Cordeiro-Fonseca V., de Mesquita Tauil R., Atanasov B., Belev N., Kovachev N., Melendez L. J. J., Dimova A., Dimov S., Zelic Z., Augustin G., Bogdanic B., Moric T., Chouillard E., Bajul M., De Simone B., Panis Y., Esposito F., Notarnicola M., Lauka L., Fabbri A., Hentati H., Fnaiech I., Aurelien V., Bougard M., Roulet M., Demetrashvili Z., Pipia I., Merabishvili G., Bouliaris K., Koukoulis G., Doudakmanis C., Xenaki S., Chrysos E., Kokkinakis S., Vassiliu P., Michalopoulos N., Margaris I., Kechagias A., Avgerinos K., Katunin J., Lostoridis E., Nagorni E. -A., Pujante A., Mulita F., Maroulis I., Vailas M., Marinis A., Siannis I., Bourbouteli E., Manatakis D. K., Tasis N., Acheimastos V., Maria S., Stylianos K., Kuzeridis H., Korkolis D., Fradelos E., Kavalieratos G., Petropoulou T., Polydorou A., Papacostantinou I., Triantafyllou T., Kimpizi D., Theodorou D., Toutouzas K., Chamzin A., Frountzas M., Schizas D., Karavokyros I., Syllaios A., Charalabopoulos A., Boura M., Baili E., Ioannidis O., Loutzidou L., Anestiadou E., Tsouknidas I., Petrakis G., Polenta E., Bains L., Gupta R., Singh S. K., Khanduri A., Bala M., Kedar A., Pisano M., Podda M., Pisanu A., Martines G., Trigiante G., Lantone G., Agrusa A., Di Buono G., Buscemi S., Veroux M., Gioco R., Veroux G., Oragano L., Zonta S., Lovisetto F., Feo C. V., Pesce A., Fabbri N., Marino F., Perrone F., Vincenti L., Papagni V., Picciariello A., Rossi S., Picardi B., Del Monte S. R., Visconti D., Osella G., Petruzzelli L., Pignata G., Andreuccetti J., D'Alessio R., Buonfantino M., Guaitoli E., Spinelli S., Sampietro G. M., Corbellini C., Lorusso L., Frontali A., Pezzoli I., Bonomi A., Chierici A., Cotsoglou C., Manca G., Delvecchio A., Musa N., Casati M., Letizia L., Abate E., Ercolani G., D'Acapito F., Solaini L., Guercioni G., Cicconi S., Sasia D., Borghi F., Giraudo G., Sena G., Castaldo P., Cardamone E., Portale G., Zuin M., Spolverato Y., Esposito M., Isernia R. M., Di Salvo M., Manunza R., Esposito G., Agus M., Asti E. L. G., Bernardi D. T., Tonucci T. P., Luppi D., Casadei M., Bonilauri S., Pezzolla A., Panebianco A., Laforgia R., De Luca M., Zese M., Parini D., Jovine E., De Sario G., Lombardi R., Aprea G., Palomba G., Capuano M., Argenio G., Orio G., Armellino M. F., Troian M., Guerra M., Nagliati C., Biloslavo A., Germani P., Aizza G., Monsellato I., Chahrour A. C., Anania G., Bombardini C., Bagolini F., Sganga G., Fransvea P., Bianchi V., Boati P., Ferrara F., Palmieri F., Cianci P., Gattulli D., Restini E., Cillara N., Cannavera A., Nita G. E., Sarnari J., Roscio F., Clerici F., Scandroglio I., Berti S., Cadeo A., Filippelli A., Conti L., Grassi C., Cattaneo G. M., Pighin M., Papis D., Gambino G., Bertino V., Schifano D., Prando D., Fogato L., Cavallo F., Ansaloni L., Picheo R., Pontarolo N., Depalma N., Spampinato M., D'Ugo S., Lepre L., Capponi M. G., Campa R. D., Sarro G., Dinuzzi V. P., Olmi S., Uccelli M., Ferrari D., Inama M., Moretto G., Fontana M., Favi F., Picariello E., Rampini A., Barberis A., Azzinnaro A., Oliva A., Totaro L., Benzoni I., Ranieri V., Capolupo G. T., Carannante F., Caricato M., Ronconi M., Casiraghi S., Casole G., Pantalone D., Alemanno G., Scheiterle M., Ceresoli M., Cereda M., Fumagalli C., Zanzi F., Bolzon S., Guerra E., Lecchi F., Cellerino P., Ardito A., Scaramuzzo R., Balla A., Lepiane P., Tartaglia N., Ambrosi A., Pavone G., Palini G. M., Veneroni S., Garulli G., Ricci C., Torre B., Russo I. S., Rottoli M., Tanzanu M., Belvedere A., Milone M., Manigrasso M., De Palma G. D., Piccoli M., Pattacini G. C., Magnone S., Bertoli P., Massucco P., Palisi M., Luzzi A. -P., Fleres F., Clarizia G., Spolini A., Kobe Y., Toma T., Shimamura F., Parker R., Ranketi S., Mitei M., Svagzdys S., Pauzas H., Zilinskas J., Poskus T., Kryzauskas M., Jakubauskas M., Zakaria A. D., Zakaria Z., Wong M. P. -K., Jusoh A. C., Zakaria M. N., Cruz D. R., Elizalde A. B. R., Reynaud A. B., Hernandez E. E. L., Monroy J. M. V. P., Hinojosa-Ugarte D., Quiodettis M., Du Bois M. E., Latorraca J., Major P., Pedziwiatr M., Pisarska-Adamczyk M., Waledziak M., Kwiatkowski A., Czyzykowski L., da Costa S. D., Pereira B., Ferreira A. R. O., Almeida F., Rocha R., Carneiro C., Perez D. P., Carvas J., Rocha C., Ferreira C., Marques R., Fernandes U., Leao P., Goulart A., Pereira R. G., Patrocinio S. D. D., de Mendonca N. G. G., Manso M. I. C., Morais H. M. C., Cardoso P. S., Calu V., Miron A., Toma E. A., Gachabayov M., Abdullaev A., Litvin A., Nechay T., Tyagunov A., Yuldashev A., Bradley A., Wilson M., Panyko A., Lateckova Z., Lacko V., Lesko D., Soltes M., Radonak J., Turrado-Rodriguez V., Termes-Serra R., Morales-Sevillano X., Lapolla P., Mingoli A., Brachini G., Degiuli M., Sofia S., Reddavid R., de Manzoni Garberini A., Buffone A., del Pozo E. P., Aparicio-Sanchez D., Dos Barbeito S., Estaire-Gomez M., Viton-Herrero R., de los Angeles Gil Olarte-Marquez M. a., Gil-Martinez J., Alconchel F., Nicolas-Lopez T., Rahy-Martin A. C., Pelloni M., Banolas-Suarez R., Mendoza-Moreno F., Nisa F. G. -M., Diez-Alonso M., Rodas M. E. V., Agundez M. C., Andres M. I. P., Moreira C. C. L., Perez A. L., Ponce I. A., Gonzalez-Castillo A. M., Membrilla-Fernandez E., Salvans S., Serradilla-Martin M., Pardo P. S., Rivera-Alonso D., Dziakova J., Huguet J. M., Valle N. P., Ruiz E. C., Valcarcel C. R., Moreno C. R., Salazar Y. T. M., Garcia J. J. R., Mico S. S., Lopez J. R., Farre S. P., Gomez M. S., Petit N. M., Titos-Garcia A., Aranda-Narvaez J. M., Romacho-Lopez L., Sanchez-Guillen L., Aranaz-Ostariz V., Bosch-Ramirez M., Martinez-Perez A., Martinez-Lopez E., Sebastian-Tomas J. C., Jimenez-Riera G., Jimenez-Vega J., Cuellar J. A. N., Campos-Serra A., Munoz-Campana A., Gracia-Roman R., Alegre J. M., Pinto F. L., O'Sullivan S. N., Antona F. B., Jimenez B. M., Lopez-Sanchez J., Carmona Z. G., Fernandez R. T., Sierra I. B., de Leon L. R. G., Moreno V. P., Iglesias E., Cumplido P. L., Bravo A. A., Simo I. R., Dominguez C. L., Caamano A. G., Lozano R. C., Martinez M. D., Torres A. N., de Quiros J. T. M. B., Pellino G., Cloquell M. M., Moller E. G., Jalal-Eldin S., Abdoun A. K., Hamid H. K. S., Lohsiriwat V., Mongkhonsupphawan A., Baraket O., Ayed K., Abbassi I., Ali A. B., Ammar H., Kchaou A., Tlili A., Zribi I., Colak E., Polat S., Koylu Z. A., Guner A., Usta M. A., Reis M. E., Mantoglu B., Gonullu E., Akin E., Altintoprak F., Bayhan Z., Firat N., Isik A., Memis U., Bayrak M., Altintas Y., Kara Y., Bozkurt M. A., Kocatas A., Das K., Seker A., Ozer N., Atici S. D., Tuncer K., Kaya T., Ozkan Z., Ilhan O., Agackiran I., Uzunoglu M. Y., Demirbas E., Altinel Y., Meric S., Hacim N. A., Uymaz D. S., Omarov N., Balik E., Tebala G. D., Khalil H., Rana M., Khan M., Florence C., Swaminathan C., Leo C. A., Liasis L., Watfah J., Trostchansky I., Delgado E., Pontillo M., Latifi R., Coimbra R., Edwards S., Lopez A., Velmahos G., Dorken A., Gebran A., Palmer A., Oury J., Bardes J. M., Seng S. S., Coffua L. S., Ratnasekera A., Egodage T., Echeverria-Rosario K., Armento I., Napolitano L. M., Sangji N. F., Hemmila M., Quick J. A., Austin T. R., Hyman T. S., Curtiss W., McClure A., Cairl N., Biffl W. L., Truong H. P., Schaffer K., Reames S., Banchini F., Capelli P., Coccolini F., Sartelli M., Bravi F., Vallicelli C., Agnoletti V., Baiocchi G. L., Catena F., Perrone, G, Giuffrida, M, Abu-Zidan, F, Kruger, V, Livrini, M, Petracca, G, Rossi, G, Tarasconi, A, Tian, B, Bonati, E, Mentz, R, Mazzini, F, Campana, J, Gasser, E, Kafka-Ritsch, R, Felsenreich, D, Dawoud, C, Riss, S, Gomes, C, Gomes, F, Gonzaga, R, Canton, C, Pereira, B, Fraga, G, Zem, L, Cordeiro-Fonseca, V, de Mesquita Tauil, R, Atanasov, B, Belev, N, Kovachev, N, Melendez, L, Dimova, A, Dimov, S, Zelic, Z, Augustin, G, Bogdanic, B, Moric, T, Chouillard, E, Bajul, M, De Simone, B, Panis, Y, Esposito, F, Notarnicola, M, Lauka, L, Fabbri, A, Hentati, H, Fnaiech, I, Aurelien, V, Bougard, M, Roulet, M, Demetrashvili, Z, Pipia, I, Merabishvili, G, Bouliaris, K, Koukoulis, G, Doudakmanis, C, Xenaki, S, Chrysos, E, Kokkinakis, S, Vassiliu, P, Michalopoulos, N, Margaris, I, Kechagias, A, Avgerinos, K, Katunin, J, Lostoridis, E, Nagorni, E, Pujante, A, Mulita, F, Maroulis, I, Vailas, M, Marinis, A, Siannis, I, Bourbouteli, E, Manatakis, D, Tasis, N, Acheimastos, V, Maria, S, Stylianos, K, Kuzeridis, H, Korkolis, D, Fradelos, E, Kavalieratos, G, Petropoulou, T, Polydorou, A, Papacostantinou, I, Triantafyllou, T, Kimpizi, D, Theodorou, D, Toutouzas, K, Chamzin, A, Frountzas, M, Schizas, D, Karavokyros, I, Syllaios, A, Charalabopoulos, A, Boura, M, Baili, E, Ioannidis, O, Loutzidou, L, Anestiadou, E, Tsouknidas, I, Petrakis, G, Polenta, E, Bains, L, Gupta, R, Singh, S, Khanduri, A, Bala, M, Kedar, A, Pisano, M, Podda, M, Pisanu, A, Martines, G, Trigiante, G, Lantone, G, Agrusa, A, Di Buono, G, Buscemi, S, Veroux, M, Gioco, R, Veroux, G, Oragano, L, Zonta, S, Lovisetto, F, Feo, C, Pesce, A, Fabbri, N, Marino, F, Perrone, F, Vincenti, L, Papagni, V, Picciariello, A, Rossi, S, Picardi, B, Del Monte, S, Visconti, D, Osella, G, Petruzzelli, L, Pignata, G, Andreuccetti, J, D'Alessio, R, Buonfantino, M, Guaitoli, E, Spinelli, S, Sampietro, G, Corbellini, C, Lorusso, L, Frontali, A, Pezzoli, I, Bonomi, A, Chierici, A, Cotsoglou, C, Manca, G, Delvecchio, A, Musa, N, 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M., Corbellini C., Lorusso L., Frontali A., Pezzoli I., Bonomi A., Chierici A., Cotsoglou C., Manca G., Delvecchio A., Musa N., Casati M., Letizia L., Abate E., Ercolani G., D'Acapito F., Solaini L., Guercioni G., Cicconi S., Sasia D., Borghi F., Giraudo G., Sena G., Castaldo P., Cardamone E., Portale G., Zuin M., Spolverato Y., Esposito M., Isernia R. M., Di Salvo M., Manunza R., Esposito G., Agus M., Asti E. L. G., Bernardi D. T., Tonucci T. P., Luppi D., Casadei M., Bonilauri S., Pezzolla A., Panebianco A., Laforgia R., De Luca M., Zese M., Parini D., Jovine E., De Sario G., Lombardi R., Aprea G., Palomba G., Capuano M., Argenio G., Orio G., Armellino M. F., Troian M., Guerra M., Nagliati C., Biloslavo A., Germani P., Aizza G., Monsellato I., Chahrour A. C., Anania G., Bombardini C., Bagolini F., Sganga G., Fransvea P., Bianchi V., Boati P., Ferrara F., Palmieri F., Cianci P., Gattulli D., Restini E., Cillara N., Cannavera A., Nita G. 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Abstract

Background: Literature suggests colonic resection and primary anastomosis (RPA) instead of Hartmann’s procedure (HP) for the treatment of left-sided colonic emergencies. We aim to evaluate the surgical options globally used to treat patients with acute left-sided colonic emergencies and the factors that leading to the choice of treatment, comparing HP and RPA. Methods: This is a prospective, international, multicenter, observational study registered on ClinicalTrials.gov. A total 1215 patients with left-sided colonic emergencies who required surgery were included from 204 centers during the period of March 1, 2020, to May 31, 2020. with a 1-year follow-up. Results: 564 patients (43.1%) were females. The mean age was 65.9 ± 15.6 years. HP was performed in 697 (57.3%) patients and RPA in 384 (31.6%) cases. Complicated acute diverticulitis was the most common cause of left-sided colonic emergencies (40.2%), followed by colorectal malignancy (36.6%). Severe complications (Clavien-Dindo ≥ 3b) were higher in the HP group (P < 0.001). 30-day mortality was higher in HP patients (13.7%), especially in case of bowel perforation and diffused peritonitis. 1-year follow-up showed no differences on ostomy reversal rate between HP and RPA. (P = 0.127). A backward likelihood logistic regression model showed that RPA was preferred in younger patients, having low ASA score (≤ 3), in case of large bowel obstruction, absence of colonic ischemia, longer time from admission to surgery, operating early at the day working hours, by a surgeon who performed more than 50 colorectal resections. Conclusions: After 100 years since the first Hartmann’s procedure, HP remains the most common treatment for left-sided colorectal emergencies. Treatment’s choice depends on patient characteristics, the time of surgery and the experience of the surgeon. RPA should be considered as the gold standard for surgery, with HP being an exception.

Published
2024

50. Sun flux variation due to the effects of orbiting planets. Case of study of a non-compact planetary system

Author

Barbier, H., López, E. D., Tipán, B., and Vásconez, C. L.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We study the phase curves for the planets of our Solar System; which, is considered as a non-compact planetary system. We focus on modeling the small variations of the light curve, based on the three photometric effects: reflection, ellipsoidal, and Doppler beaming. Theoretical predictions for these photometric variations are proposed, as if a hypothetical external observer would measure them. In contrast to similar studies of multi-planetary systems, the physical and geometrical parameters for each planet of the Solar System are well-known. Therefore, we can evaluate with accuracy the mathematical relations that shape the planetary light curves for an external fictitious observer. Our results suggest that in all the planets of study the ellipsoidal effect is very weak, while the Doppler beaming effect is in general dominant. In fact, the latter effect seems to be confirmed as the principal cause of variations of the light curves for the planets. This affirmation could not be definitive in Mercury or Venus where the Doppler beaming and the reflection effects have similar amplitudes. The obtained phase curves for the Solar System planets show interesting new features that have not been presented before, so the results presented here are relevant in their application to other non-compact systems, since they allow us to have an idea of what it is expected to find in their light curves., Comment: 12 pages. 3 figures, 3 tables

Published
2018

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