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14 results on '"Tristan Weber"'

1. Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars

Author

Shaosui Xu, Janet G. Luhmann, David L. Mitchell, Tristan Weber, David A. Brain, Yingjuan Ma, Shannon M. Curry, Gina A. DiBraccio, Jasper Halekas, Suranga Ruhunusiri, Christian Mazelle, Robert J. Lillis, and Benoit Langlais

Subjects
Mars, Solar-planetary interactions, Magnetic fields, Interplanetary magnetic fields, Magnetic anomalies, Astrophysics, QB460-466
Abstract

Mars’s magnetosphere is hybrid, having contributions from both an induced magnetosphere like Venus and the localized crustal magnetic fields. However, the planetary fields also include large-scale, more global components. In this study, we investigate their role in Mars’s magnetospheric topological responses to the interplanetary magnetic field (IMF) clock angle using observations from the Mars Atmospheric Volatile and EvolutioN mission. We show that the large-scale planetary field has a “dipole-like” influence on the Mars global magnetosphere by examining the open field topology. We find that the “dipole-like” planetary field, as at Earth, results in a more open magnetosphere during southward IMF. The clock angle effects on the twisted magnetotail current sheet are similarly consistent with this analogy. It reinforces the idea that Mars’s magnetosphere and solar wind interaction are more Earth-like than previously thought.

Published
2023
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8. Martian Crustal Field Influence on O+ and O2+ Escape as Measured by MAVEN

Author

David Brain, Bruce M. Jakosky, Christian Mazelle, Jared Espley, Tristan Weber, James P. McFadden, D. L. Mitchell, Shaosui Xu, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Martian, Atmospheric escape, Field (physics), Astrophysics::High Energy Astrophysical Phenomena, Mars, MAVEN, ionosphere, Mars Exploration Program, crustal magnetic fields, ion escape, Astrobiology, Physics::Geophysics, Geophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, atmospheric escape, Geology
Abstract

International audience; Martian crustal magnetic fields influence the solar wind interaction with Mars in a way that is not fully understood. In some locations, crustal magnetic fields act as "mini-magnetospheres," shielding the planet's atmosphere, while in other locations they act as channels for enhanced energy input and particle escape. The net effect of this system is not intuitively clear, but previous modeling studies have suggested that crustal fields likely decrease global ion escape from Mars. In this study, we use data from the Mars Atmosphere and Volatile EvolutioN spacecraft to analyze how crustal magnetic fields influence both global and local ion escape at Mars. We find that crustal fields only increase ion escape if ions are not bound tightly to the magnetic field. Specifically, ion escape is increased only if closed magnetic fields trap 35% or less of energized oxygen ions. In any other case, crustal fields decrease both global and local ion escape by as much as 40% and 80%, respectively. This suggests that the presence of crustal magnetic fields has had a moderate impact on atmospheric ion loss throughout Martian history, potentially influencing the planet's atmospheric evolution and habitability.

Published
2021
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9. Global Ambipolar Potentials and Electric Fields at Mars Inferred From MAVEN Observations

Author

Shaosui Xu, David L. Mitchell, Yingjuan Ma, Tristan Weber, David A. Brain, Jasper Halekas, Suranga Ruhunusiri, Gina DiBraccio, Christian Mazelle, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Sun-Mars interaction, Geophysics, Space and Planetary Science, particle acceleration, solar wind electrons, [SDU]Sciences of the Universe [physics], ambipolar electric field, MAVEN, ion escape
Abstract

International audience; The motion of charged particles is governed by electromagnetic forces at high altitudes at Mars and thus the characterization of electrostatic potential and electric fields is important for understanding ion escape at Mars. In this study, we utilize measurements from the Mars Atmosphere and Volatile EvolutioN mission to derive electrostatic potentials above the collisional atmosphere at Mars. We find averaged potentials to be up to ∼100 V in the magnetosheath and down to ∼-70 V in the tail, with respect to the upstream. We then derive electric fields based on averaged potential maps, ranging ∼0.01-0.1 V/km. These data-derived electric fields are in good agreement with ambipolar electric fields from a multi-fluid magnetohydrodynamic (MHD) model. MHD results also reveal that these large electric fields mainly originate from the electron pressure gradient in the magnetosheath and in the transition region from the hot solar wind flow to the cold ionospheric flow. This work provides the first data-based characterization of global ambipolar electric fields at Mars (outside of the main ionosphere).

Published
2021
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10. Inverted-V Electron Acceleration Events Concurring With Localized Auroral Observations at Mars by MAVEN

Author

Sonal Jain, Christopher M. Fowler, Nicholas M. Schneider, Tristan Weber, David Brain, James P. McFadden, Matthew Fillingim, David L. Mitchell, Christian Mazelle, Jared Espley, Robert Lillis, Shaosui Xu, Laila Andersson, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, field-aligned potential, inverted-V electron, Mars, MAVEN, Magnetic reconnection, Mars Exploration Program, Astrophysics, aurora, Geophysics, Electron acceleration, [SDU]Sciences of the Universe [physics], magnetic reconnection, General Earth and Planetary Sciences
Abstract

International audience; From February to March 2019, the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft repeatedly observed aurora near periapsis over Mars' southern strong crustal fields. During these orbits, the Solar Wind Electron Analyzer observed accelerated electrons at similar locations to where the auroras were observed, resembling the inverted-V structure observed near Earth's auroral region. In this study, we present a case study of such an acceleration event, where we estimate a field-aligned electrostatic potential drop of ∼440 V. We determine the field-aligned current from the observed magnetic perturbation reaches 1.1 μA/m2, agreeing reasonably well with the estimated net electron current carried by acceleration electrons with a maximum of 2.5 μA/m2. Similar to Earth, the potential drop develops when the ambient plasma cannot sustain the imposed field-aligned current. We also estimate the potential layer to be located above 750- to 850-km altitude and the associated electric field to be ∼0.6 V/m.

Published
2020
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11. Search for the decay Ds+ ??e+?e

Author

J. Libby, Y. Fu, Yaquan Fang, M. Greco, Shou-hua Zhu, J. H. Zou, Z. G. Wang, R. Kappert, Y. H. Yan, P. Kiese, Yuan Hou, Q. Q. Song, H. Y. Zhang, S. S. Sun, J. W. Zhao, Y. Ding, R. A. Briere, B. J. Liu, M. M. Ma, J. Chai, G. X. Sun, J. V. Bennett, Li Yan, X. Q. Hao, M. Qi, H. J. Yang, Z. Jiao, D. H. Zhang, E. M. Gersabeck, P. L. Wang, G. F. Chen, G. S. Huang, T. Y. Xing, Y. C. Zhu, G. F. Xu, S. Jin, Y. P. Guo, X. S. Jiang, S. Nakhoul, Tao Luo, H. B. Li, C. L. Luo, Q. Zhou, X. L. Luo, C.-H. Rosner, Jun-Yi Zhang, K. Schoenning, Q. Y. Li, B. S. Zou, W. Kühn, J. Y. Zhang, R. E. Mitchell, M. Kuessner, F. De Mori, Serkant Ali Cetin, P. Larin, R. X. Yang, H. H. Wang, Xiao-Rui Lyu, C. C. Zhang, B. Zhong, L. B. Guo, Q. A. Malik, G. Mezzadri, W. C. Yan, Z. P. Zhang, Yunlong Zhang, Z. Y. You, Z. A. Zhu, H. W. Wen, X. Y. Zhou, B. X. Yu, Zujian Wang, C. Sowa, Y. B. Zhao, Fang Liu, I. B. Nikolaev, Wei Xu, J. H. Yin, W. Shan, M. Shao, Y. T. Gu, D. Bettoni, J. Dong, Zhiqiang Liu, R. Kliemt, Qiang Zhao, Lei Li, S. Nisar, A. Pitka, M.G. Alekseev, A. N. Zhu, Tao Zhang, C. J. Tang, Y. Hu, K. Begzsuren, Y. P. Lu, J. L. Zhang, W. P. Wang, U. Wiedner, H. L. Jiang, I. Denysenko, L. M. Gu, A. Mangoni, M. N. Achasov, L. P. Zhou, A. Guskov, Jie Yu, F. Bianchi, Jianping Zheng, Y. M. Ma, Z. P. Mao, L. H. Wu, M. Richter, Z. Ning, S. Y. Xiao, X. Y. Song, Y. K. Heng, T. Khan, Shulei Zhang, F. Y. Li, Magnus Wolke, Y. F. Liang, D. P. Jin, H. S. Chen, Alperen Yuncu, M. Savrie, N. Hüsken, T. Y. Qi, J. Min, Y. F. Wang, Xu Shan, C. P. Shen, Yi Jin, H. B. Liu, B. Kopf, W. Imoehl, B. Y. Zhang, J. B. Jiao, J. Fang, J. W. Li, R. M. Wang, K. L. He, L. J. Wu, X. L. Ji, T. Held, X. F. Wang, Q. M. Ma, A. Mustafa, S. J. Zhao, T. J. Min, Xujin Yuan, K. J. Zhu, D. Y. Liu, Y. J. Xiao, S. X. Du, K. Y. Liu, H. L. Dai, J. Q. Zhang, T. Hussain, X. Y. Ma, A. Calcaterra, Z. G. Zhao, L. Z. Liao, X. H. Liu, Z. Y. Zhang, Y. J. Mo, S. B. Liu, H. J. Lu, J. G. Lu, N. Qin, Y. X. Xia, F. Feldbauer, Lingxuan Zhang, Yu Bai, W. X. Gong, H. H. Zhang, S. W. Han, Y. Yuan, Y. S. Zhu, G. Cibinetto, X. K. Zhou, A. Sarantsev, Matthew Glenn Kurth, D. H. Wei, P. R. Li, Bibo Ke, J. S. Lange, M. Destefanis, W. B. Yan, Y. Nefedov, X. L. Gao, Z. J. Sun, Jimin Zhao, P. L. Li, P. W. Luo, Q. J. Xu, Z. L. Huang, Y. G. Xie, Xiang-Gan Liu, M. H. Ye, F. E. Maas, T. Hu, S. Maldaner, J. P. Dai, J. C. Chen, Xuanhong Lou, Q. P. Ji, Viktor Thorén, I. R. Boyko, S. Pacetti, S. Leiber, O. Bakina, H. Liang, Ke Wang, H. H. Liu, J. C. Li, X. P. Qin, C. F. Redmer, Li Zhou, M. Ablikim, Liqing Xu, X. Y. Shen, X. Y. Jiang, Q. Ouyang, I. Uman, Nasser Kalantar-Nayestanaki, Y. G. Gao, Q. Liu, Tristan Weber, C. Dong, L. L. Ma, L. Gong, Z. L. Dou, S. Sosio, Z. Q. Yang, S. S. Fang, Ke Li, M. Bertani, P. X. Shen, J. Zhuang, J. D. Lu, L. G. Xia, C. H. Li, X. H. Sun, L. Y. Dong, L. Yang, Y. B. Liu, Z. Wu, M. X. Luo, D. V. Dedovich, S. L. Yang, A. Amoroso, G. Y. Tang, C. Morales Morales, F. F. Sui, Yue Pan, X. T. Huang, M. Albrecht, Zhiqing Zhang, J. S. Huang, S. Qian, Q. An, Jialun Ping, Jie Zhao, D. X. Lin, Z. Gao, M. H. Gu, R. Kiuchi, G. Felici, C. X. Liu, K. Zhang, X. Y. Zhang, Alexey Zhemchugov, H. M. Hu, A. Dbeyssi, S. L. Niu, G. Rong, F. H. Liu, H. Y. Sheng, W. D. Li, Z. J. Xiao, R. Poling, Z. X. Meng, F. H. Heinsius, Nicolas Berger, J. B. Liu, X. Q. Li, Y. F. Long, Joachim Pettersson, Ke Liu, X. P. Xu, X. B. Ji, Y. J. Sun, Yifan Yang, E. Boger, J. W. Zhang, X. A. Xiong, C. X. Yu, B. T. Tsednee, Fenfen An, Angelo Rivetti, H. J. Li, Dong E. Liu, P. Patteri, X. H. Li, Q. L. Xiu, Y. T. Tan, B. Zheng, R. G. Ping, K. Goetzen, A. A. Zafar, W. Gradl, X. N. Ma, B. L. Wang, Xingchao Dai, Y. H. Zheng, X. Tang, Xiaozhong Huang, Cong-Feng Qiao, X. H. Mo, T. C. Zhao, Z. A. Liu, L. S. Wang, M. Fritsch, S. Q. Qu, Z. B. Li, W. Ikegami Andersson, X. L. Wang, W. S. Cheng, G. Li, V. Prasad, M. Kavatsyuk, G. R. Liao, Andrzej Kupsc, Y. Ban, P. Weidenkaff, K. H. Rashid, L. L. Wang, H. Cai, T. Johansson, J. F. Chang, N. Yu. Muchnoi, C. D. Fu, S. P. Wen, M. Rolo, C. Q. Feng, X. S. Qin, B. X. Zhang, M. L. Chen, X. S. Kang, L. Koch, A. Khoukaz, X. R. Zhou, Cheng Li, O. B. Kolcu, Z. Y. Deng, M. Ripka, Y. H. Zhang, M. G. Zhao, Y. H. Yang, X. X. Ma, X. Cai, L. Lavezzi, S. L. Olsen, R. Baldini Ferroli, R. P. Guo, J. Zhu, Y. T. Liang, Xingguo Li, S. J. Chen, F. Cossio, Krisztian Peters, Z. Y. Wang, Teresa Lenz, B. Q. Wang, M. Z. Wang, X. N. Li, Haiping Peng, W. G. Li, A. G. Denig, Y. K. Sun, J. F. Sun, S. Spataro, S. Marcello, Y. Zeng, Y. J. Lin, H. M. Liu, J. F. Hu, Zhe Sun, S. Lusso, G. F. Cao, X D Shi, Y. J. Mao, H. X. Yang, I. Garzia, G. A. Chelkov, Y. H. Xie, J. Pellegrino, M. Maggiora, Ling Zhao, Lei Zhao, Z. L. Hou, C. Z. Yuan, N. Cao, B. Garillon, Y. B. Chen, J. G. Messchendorp, Xiaofeng Zhu, J. Z. Zhang, A. Q. Guo, J. J. Song, L. Sun, C. W. Wang, Muhammad Irshad, Z. H. Qin, M. Kuemmel, X. F. Cui, W. J. Zhu, X. D. Shi, F. A. Harris, W. L. Chang, Dan Wang, R. Farinelli, H. Leithoff, F. Li, F. C. Ma, H. L. Ma, D. M. Li, H. Muramatsu, M. Pelizaeus, J. Y. Liu, Q. Gao, Y. N. Gao, Y. Zhang, Feng Yan, J. Z. Fan, T. Liu, J. F. Qiu, M. Papenbrock, S. Ahmed, Y. X. Yang, Kang Li, L. Fava, Y. Z. Sun, I. K. Keshk, F. Nerling, C. X. Lin, Alexander Leon Gilman, M. Rump, Gang Zhao, M. Y. Dong, and İstanbul Arel Üniversitesi

Subjects
Nuclear physics, Physics, Luminosity (scattering theory), Electron–positron annihilation, Detector, Radiative transfer, High Energy Physics::Experiment, Limit (mathematics), Photon energy, Energy (signal processing)
Abstract

A search for the rare radiative leptonic decay Ds+??e+?e is performed for the first time using electron-positron collision data corresponding to an integrated luminosity of 3.19 fb-1, collected with the BESIII detector at a center-of-mass energy of 4.178 GeV. No evidence for the Ds+??e+?e decay is seen, and an upper limit of B(Ds+??e+?e)0.01 GeV. © 2019 authors. Published by the American Physical Society.

Published
2019

12. Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time

Author

Phillip C. Chamberlin, Jane L. Fox, Jared Espley, Andrew F. Nagy, Daniel Lo, Yuki Harada, Ali Rahmati, Casey L. Flynn, Valeriy Tenishev, Shotaro Sakai, Shannon Curry, Shaosui Xu, Franck Montmessin, Jean-Yves Chaufray, Tristan Weber, Anna Kotova, Michael Mendillo, Christy Lentz, David Brain, Kyle Connour, J. P. McFadden, Nicholas M. Schneider, Roger V. Yelle, Christina O. Lee, Bruce M. Jakosky, F. J. Crary, Matthew Fillingim, Arnaud Stiepen, Michael R. Combi, W. K. Peterson, Thomas E. Cravens, Joseph M. Grebowsky, Jared Bell, Kaori Terada, Anders Eriksson, K. Roeten, Jeffrey Trovato, Frank Eparvier, Zachary Girazian, S. Inui, P. Dunn, Paul Withers, Majd Mayyasi, Scott L. England, Yaxue Dong, Meredith Elrod, Edward Thiemann, David E. Siskind, Paul R. Mahaffy, Robert H. Tolson, François Leblanc, Gina A. DiBraccio, David L. Mitchell, David Andrews, Kirk Olsen, Ronan Modolo, K. Fallows, Dolon Bhattacharyya, Marissa F. Vogt, Masaki Fujimoto, Michael Chaffin, S. Houston, Nicolas André, Mehdi Benna, Chuanfei Dong, Kyle Crabb, Naoki Terada, J. R. Gruesbeck, Takeshi Kuroda, Yingjuan Ma, Yuni Lee, Alexander S. Medvedev, Robert Lillis, Glyn Collinson, Hiromu Nakagawa, Christopher M. Fowler, K. G. Hanley, Richard W. Zurek, R. M. Dewey, Hilary Egan, Robert E. Ergun, S. R. Shaver, Takuya Hara, Sonal Jain, Suranga Ruhunusiri, Jasper Halekas, Morgane Steckiewicz, S. Stone, Stephen W. Bougher, Jacob Hermann, Janet G. Luhmann, Hannes Groeller, Y. I. J. Soobiah, David Pawlowski, Xiaohua Fang, A. Fogle, Davin Larson, Yosuke Matsumoto, T. M. Esman, R. Jolitz, Darren Baird, Karim Meziane, O. Q. Hamil, Clara Narvaez, William E. McClintock, J. Correira, Gabor Toth, John E. P. Connerney, M. Slipski, Melissa L. Marquette, Christopher T. Russell, Kanako Seki, Matteo Crismani, Michael L. Stevens, Greg Holsclaw, John Clarke, Philippe Garnier, Mika Holmberg, Erdal Yiğit, Ian Stewart, Rafael Lugo, G. T. Delory, Laila Andersson, Justin Deighan, C. F. Bowers, Scott Evans, Zachariah Milby, Norberto Romanelli, R. Sharrar, Franck Lefèvre, Christian Mazelle, Daniel N. Baker, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), NASA Johnson Space Center (JSC), NASA, National Institute of Aerospace [Hampton] (NIA), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), Communications and Power Industries (CPI), Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), Princeton University, University of Arizona, Wright State University, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Department of Physics and Astronomy [Ames, Iowa], Iowa State University (ISU), University of Kansas [Kansas City], The University of Tokyo (UTokyo), National Institute of Information and Communications Technology [Tokyo, Japan] (NICT), PLANETO - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Analytical Mechanics Associates, Inc., University of California [Los Angeles] (UCLA), University of California, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, University of New Brunswick (UNB), Tohoku University [Sendai], Eastern Michigan University, University of Michigan System, Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Naval Research Laboratory (NRL), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Graduate School of Information Sciences [Sendai], Lunar and Planetary Laboratory [Tucson] (LPL), Department of Physics and Astronomy [Fairfax], George Mason University [Fairfax], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and California Institute of Technology (CALTECH)-NASA

Subjects
010504 meteorology & atmospheric sciences, Solar wind, Extrapolation, Mars, Present day, Atmospheric sciences, Mars climate, 01 natural sciences, Atmosphere, Mars atmosphere, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, 13. Climate action, Space and Planetary Science, Magnetospheres, Environmental science, business
Abstract

International audience; Observations of the Mars upper atmosphere made from the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft have been used to determine the loss rates of gas from the upper atmosphere to space for a complete Mars year (16 Nov 2014 – 3 Oct 2016). Loss rates for H and O are sufficient to remove ∼2-3 kg/s to space. By itself, this loss would be significant over the history of the planet. In addition, loss rates would have been greater early in history due to the enhanced solar EUV and more-active Sun. Integrated loss, based on current processes whose escape rates in the past are adjusted according to expected solar evolution, would have been as much as 0.8 bar CO2 or 23 m global equivalent layer of H2O; these losses are likely to be lower limits due to the nature of the extrapolation of loss rates to the earliest times. Combined with the lack of surface or subsurface reservoirs for CO2 that could hold remnants of an early, thick atmosphere, these results suggest that loss of gas to space has been the dominant process responsible for changing the climate of Mars from an early, warmer environment to the cold, dry one that we see today.

Published
2018
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13. Observation of pseudoscalar and tensor resonances in J /ψ →γφφ

Author

H. H. Liu, H. R. Qi, Y. P. Guo, Serkant Ali Cetin, J. C. Li, J. B. Jiao, Xiang-Zhou Cai, H. Liang, J. Zhuang, Q. P. Ji, M. X. Luo, Jian Wei, D. V. Dedovich, S. Qian, Q. An, Jialun Ping, K. Zhang, X. Y. Zhang, J. B. Liu, I. Uman, X. L. Ji, Y. J. Sun, E. Boger, C. Hu, Y. P. Lu, H. B. Li, B. Kloss, A. G. Denig, C. L. Luo, G. A. Chelkov, X. Tang, C. C. Zhang, H. J. Lu, J. G. Lu, B. Zhong, L. B. Guo, J. Min, Lei Li, F. E. Maas, T. Hu, E. H. Thorndike, R. Baldini Ferroli, Z. Y. Zhang, T. Ma, X. L. Li, Yanping Huang, W. L. Yuan, X. H. Liu, L. Q. Qin, H. B. Liu, Q. Ouyang, S. S. Fang, P. X. Shen, Z. Wu, Krisztian Peters, M. Ullrich, Z. J. Xiao, L. W. Jiang, M. Z. Wang, Zhiqing Zhang, Y. G. Xie, B. Kopf, Y. B. Liu, C. Leng, X. N. Li, A. Calcaterra, Z. G. Zhao, K. L. He, Z. L. Dou, D. W. Bennett, Zujian Wang, H. H. Zhang, Haiping Peng, S. W. Han, Z. J. Sun, H. Loehner, Z. A. Liu, Z. Gao, M. Maggiora, Ling Zhao, Jiaxi Liu, S. L. Niu, L. G. Xia, X. H. Mo, L. S. Wang, M. H. Ye, X. Q. Li, Lei Zhao, V. Prasad, Y. Ban, P. Weidenkaff, J. Q. Zhang, K. J. Zhu, Z. L. Hou, S. P. Wen, Jimin Zhao, Y. B. Chen, Y. H. Zheng, Cong-Feng Qiao, O. Albayrak, X. S. Qin, X. R. Zhou, L. L. Wang, H. Cai, Cheng Li, K. Y. Liu, N. Yu. Muchnoi, X. S. Kang, Z. B. Li, Y. H. Zhang, G. Li, Y. F. Wang, S. L. Olsen, C. Z. Yuan, C. F. Redmer, Xichao Ruan, Andrzej Kupsc, C. D. Fu, Z. Y. Wang, C. Q. Feng, X. R. Chen, M. H. Gu, Z. Y. Deng, M. Ripka, Y. X. Xia, Y. H. Guan, T. Hussain, X. Y. Ma, W. X. Gong, L. Y. Dong, J. M. Bian, H. Y. Sheng, S. J. Zhao, X. K. Zhou, C. X. Yu, Yaquan Fang, M. Greco, P. L. Wang, C. H. Li, Shou-hua Zhu, S. B. Liu, B. Zheng, Q. J. Xu, R. G. Ping, Y. Nefedov, W. J. Zheng, X. L. Luo, G. X. Sun, J. V. Bennett, Li Yan, M. Y. Dong, J. C. Chen, Xuanhong Lou, Cen Zhang, Z. Jiao, D. H. Zhang, X. K. Chu, Nasser Kalantar-Nayestanaki, Ke Wang, I. B. Nikolaev, C. Morales Morales, K. Schoenning, Q. Y. Li, B. S. Zou, M. Qi, Yue Pan, J. H. Yin, H. J. Yang, J. Z. Bai, M. Shao, Y. T. Gu, W. P. Wang, F. Bianchi, R. Poling, P. F. Duan, Peilian Liu, Fenfen An, Lingxuan Zhang, B. L. Wang, W. C. Yan, Magnus Wolke, Y. F. Liang, T. C. Zhao, E. Fioravanti, D. P. Jin, O. Fedorov, Tao Luo, L. P. Zhou, J. H. Zou, X. L. Kang, A. Sarantsev, D. H. Wei, P. R. Li, D. Y. Liu, J. S. Lange, S. Schumann, B. X. Yu, X. P. Xu, X. B. Ji, M. Tiemens, Zhi Zeng, Y. M. Ma, Q. W. Zhao, N. Qin, Yunlong Zhang, Z. P. Mao, J. F. Chang, Yao Wang, P. Patteri, D. Bettoni, F. Y. Li, H. S. Chen, Alperen Yuncu, P. Kiese, Jin Li, Igor Boyko, J. L. Zhang, H. P. Cheng, J. Fang, Tao Li, R. A. Briere, Jianping Zheng, R. Kliemt, S. Zhu, S. S. Sun, Z. G. Wang, Shan Wang, H. Y. Zhang, X. S. Jiang, Ch. Rosner, Jie Yu, Xiao-Rui Lyu, S. X. Du, Y. J. Mo, X. Q. Hao, G. F. Chen, J. Y. Zhang, J. J. Zhang, Y. B. Zhao, W. Shan, M. Destefanis, G. S. Varner, O. Cakir, P. Larin, J. Dong, G. Cibinetto, M. Bertani, Z. Haddadi, L. Yang, S. Nisar, C. J. Tang, Y. Hu, Y. K. Heng, Manuel Lara, D. Xiao, Liqing Xu, Jie Zhao, D. X. Lin, X. N. Ma, Alexey Zhemchugov, H. M. Hu, X. Y. Shen, W. Gradl, V. Santoro, A. Zallo, F. H. Liu, J. W. Zhang, Y. Ding, D. Y. Wang, B. Wang, B. J. Liu, A. A. Zafar, M. G. Zhao, M. Fritsch, G. Felici, M. Kavatsyuk, Y. N. Zhang, W. Kühn, Q. Liu, Tristan Weber, Z. A. Zhu, Y. X. Yang, X. T. Chen, L. L. Ma, L. Gong, B. X. Zhang, K. H. Rashid, A. Amoroso, C. P. Shen, Q. L. Xiu, X. Fang, R. E. Mitchell, A. Dbeyssi, F. Feldbauer, Feng Liu, M. Ablikim, X. Y. Jiang, M. Kornicer, Y. T. Liang, A. Julin, S. J. Chen, F. De Mori, X. L. Gao, X. Y. Zhou, C. Dong, S. Sosio, K. J. Li, X. F. Wang, Q. M. Ma, Joachim Pettersson, Y. N. Guo, A. Hafner, Q. Zhao, Y. Z. Sun, X. Y. Niu, Y. Yuan, Y. S. Zhu, Yu Zhang, Z. H. Wang, G. S. Huang, Xiaocong Ai, K. Goetzen, Dan Wang, Y. Q. Wang, M. L. Chen, X. T. Huang, H. L. Dai, G. Rong, G. R. Liao, J. F. Sun, Gang Zhao, S. Marcello, Y. Zeng, Zhe Sun, L. H. Wu, M. Savrie, Xiaofeng Zhu, J. Z. Zhang, X. Y. Gao, R. Farinelli, L. D. Liu, F. A. Harris, H. L. Ma, D. M. Li, H. Muramatsu, M. Pelizaeus, J. Y. Liu, Q. Gao, Y. N. Gao, Y. Zhang, J. Z. Fan, J. S. Huang, Z. P. Zhang, C. X. Liu, G. F. Xu, S. Jin, X. Y. Song, F. Li, F. C. Ma, L. Zotti, J. F. Qiu, L. Fava, F. Nerling, Z. Ning, Y. J. Mao, H. X. Yang, I. Garzia, J. P. Liu, I. Tapan, Y. H. Yan, J. W. Zhao, J. G. Messchendorp, J. P. Dai, Zhiqing Liu, T. Johansson, Qiunan Xu, Y. C. Zhu, O. B. Kolcu, H. Xiao, T. Held, W. G. Li, S. Spataro, H. M. Liu, J. F. Hu, G. F. Cao, A. Q. Guo, W. M. Song, Z. H. Qin, D. J. Ambrose, M. Albrecht, W. D. Li, Bibo Ke, W. B. Yan, M. N. Achasov, S. Pacetti, Fang Liu, U. Wiedner, I. Denysenko, and B. Y. Zhang

Subjects
Physics, Pseudoscalar, Nuclear physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Electron–positron annihilation, Partial wave analysis, 0103 physical sciences, Analytical chemistry, Resonance, 010306 general physics, 01 natural sciences, NO
Abstract

Based on a sample of (1310.6 +/- 10.5) x 10(6) J/psi events collected with the BESIII detector operating at the BEPCII storage ring, a partial wave analysis of the decay J/psi -> gamma phi phi is performed in order to study the intermediate states. Results of the partial wave analysis show that the structures are predominantly 0(-+) states. The existence of the eta(2225) is confirmed, and its resonance parameters are measured. Two additional pseudoscalar states, the eta(2100) with a mass of 2050(-24-26)(+30+75) MeV/c(2) and a width of 250(-30-164)(+36+181) MeV/c(2) and the X(2500) with a mass of 2470(-19-23)(+15+101) MeV/c(2) and a width of 230(-35-33)(+64+56) MeV/c(2), are observed. In addition to these three pseudoscalar states, the scalar state f(0)(2100), and three tensor states, the f(2)(2010), f(2)(2300) and f(2)(2340), are observed in the process J/psi -> gamma phi phi The product branching fractions B(J/psi -> gamma X) x B(X -> phi phi) are reported.

Published
2016

14. Early MAVEN Deep Dip campaign reveals thermosphere and ionosphere variability

Author

J. M. Grebowsky, F. Leblanc, Suranga Ruhunusiri, John E. P. Connerney, Xiaohua Fang, Ronan Modolo, Scott D. Guzewich, Richard W. Zurek, Arnaud Stiepen, Michael R. Combi, Davin Larson, Christopher T. Russell, Anders Eriksson, M. Steckiewicz, Yaxue Dong, Franck Lefèvre, Christian Mazelle, J. A. Sauvaud, P. Dunn, Jane L. Fox, Shotaro Sakai, Chuanfei Dong, Yingjuan Ma, S. W. Bougher, S. Stone, R. Jolitz, Gregory M. Holsclaw, T. McEnulty, William E. McClintock, Kirk Olsen, Yuki Harada, A. F. Nagy, Robert Lillis, Thomas N. Woods, Michael L. Stevens, Sonal Jain, Jasper Halekas, Hannes Gröller, Shannon Curry, Franck Montmessin, D. W. Curtis, Tristan Weber, Kanako Seki, Christina O. Lee, Glyn Collinson, Takuya Hara, Paul Mahaffy, D. Baird, Scott L. England, D. Toublanc, Matteo Crismani, Roger V. Yelle, Gina A. DiBraccio, W. K. Peterson, R. M. Dewey, J. P. McFadden, Jared Bell, F. J. Crary, David Brain, Ali Rahmati, Matthew Fillingim, Janet G. Luhmann, John Clarke, Meredith Elrod, Bruce M. Jakosky, Nicholas M. Schneider, A. I. F. Stewart, Paul Withers, Majd Mayyasi, Thomas E. Cravens, Marissa F. Vogt, Edward Thiemann, Michael Chaffin, Phillip C. Chamberlin, Jean-Yves Chaufray, Daniel N. Baker, G. T. Delory, Laila Andersson, Jared Espley, Justin Deighan, Daniel Lo, Christopher M. Fowler, Valeriy Tenishev, Robert E. Ergun, Roberto Livi, Robert H. Tolson, David L. Mitchell, Scott Evans, Michiko Morooka, K. Fortier, Mehdi Benna, Frank Eparvier, David Andrews, Yuni Lee, Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Department of Physics and Astronomy [Ames, Iowa], Iowa State University (ISU), NASA Goddard Space Flight Center (GSFC), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), NASA Johnson Space Center (JSC), NASA, National Institute of Aerospace [Hampton] (NIA), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Boston], Boston University [Boston] (BU), Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), Computational Physics, Inc., Department of Physics [Dayton], Wright State University, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, PLANETO - LATMOS, Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), Solar-Terrestrial Environment Laboratory [Nagoya] (STEL), Nagoya University, Naval Research Laboratory (NRL), University of California [Berkeley], University of California-University of California, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Martian, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Multidisciplinary, 010504 meteorology & atmospheric sciences, Atmospheric escape, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Atmosphere of Mars, Atmospheric sciences, 01 natural sciences, Physics::Geophysics, Atmosphere, Altitude, 13. Climate action, Extreme ultraviolet, 0103 physical sciences, Physics::Space Physics, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Thermosphere, Ionosphere, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences
Abstract

International audience; The Mars Atmosphere and Volatile Evolution (MAVEN) mission, during the second of its Deep Dip campaigns, made comprehensive measurements of martian thermosphere and ionosphere composition, structure, and variability at altitudes down to ~130 kilometers in the subsolar region. This altitude range contains the diffusively separated upper atmosphere just above the well-mixed atmosphere, the layer of peak extreme ultraviolet heating and primary reservoir for atmospheric escape. In situ measurements of the upper atmosphere reveal previously unmeasured populations of neutral and charged particles, the homopause altitude at approximately 130 kilometers, and an unexpected level of variability both on an orbit-to-orbit basis and within individual orbits. These observations help constrain volatile escape processes controlled by thermosphere and ionosphere structure and variability.

Published
2015
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