Cosmic-ray flux predictions and observations for and with Metis on board Solar Orbiter
C. Grimani, V. Andretta, P. Chioetto, V. Da Deppo, M. Fabi, S. Gissot, G. Naletto, A. Persici, C. Plainaki, M. Romoli, F. Sabbatini, D. Spadaro, M. Stangalini, … 展开作者
C. Grimani, V. Andretta, P. Chioetto, V. Da Deppo, M. Fabi, S. Gissot, G. Naletto, A. Persici, C. Plainaki, M. Romoli, F. Sabbatini, D. Spadaro, M. Stangalini, D. Telloni, M. Uslenghi, E. Antonucci, A. Bemporad, G. Capobianco, G. Capuano, M. Casti, Y. De Leo, S. Fineschi, F. Frassati, F. Frassetto, P. Heinzel, G. Jerse, F. Landini, A. Liberatore, E. Magli, M. Messerotti, D. Moses, G. Nicolini, M. Pancrazzi, M. G. Pelizzo, P. Romano, C. Sasso, U. Schühle, A. Slemer, T. Straus, R. Susino, L. Teriaca, C. A. Volpicelli, J. L. Freiherr von Forstner, P. Zuppella
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11 pages, 7 figures, accepted for publication on Astronomy & Astrophysics
The Metis coronagraph is one of the remote sensing instruments hosted on board the ESA/NASA Solar Orbiter mission. Metis is devoted to carry out the first simultaneous imaging of the solar corona in both visible light (VL) and ultraviolet (UV). High-energy particles penetrate spacecraft materials and may limit the performance of on-board instruments. A study of galactic cosmic-ray (GCR) tracks observed in the first VL images gathered by Metis during the commissioning phase for a total of 60 seconds of exposure time is presented here. A similar analysis is planned for the UV channel. A prediction of the GCR flux up to hundreds of GeV is made here for the first part of the Solar Orbiter mission to study the Metis coronagraph performance. GCR model predictions are compared to observations gathered on board Solar Orbiter by the EPD/HET experiment in the range 10 MeV-100 MeV in the summer 2020 and with previous measurements. Estimated cosmic-ray fluxes above 70 MeV n$^{-1}$ have been also parameterized and used for Monte Carlo simulations aiming at reproducing the cosmic-ray track observations in the Metis coronagraph VL images. The same parameterizations can also be used to study the performance of other detectors. By comparing observations of cosmic-ray tracks in the Metis VL images with FLUKA Monte Carlo simulations of cosmic-ray interactions in the VL detector, it is found that cosmic rays fire a fraction of the order of 10$^{-4}$ of the whole image pixel sample. Therefore, cosmic rays do not affect sensibly the quality of Metis VL images. It is also found that the overall efficiency for cosmic-ray identification in the Metis VL images is approximately equal to the contribution of Z$>$2 particles. As a result, the Metis coronagraph may play the role of a proton monitor for long-term GCR variations during the overall mission duration.
A Point-Spread Function for the Extreme Ultraviolet High-Resolution Imager on board Solar Orbiter
Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学天体物理实验室）；Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium（比利时皇家天文台太阳-地球卓越中心SIDC）；Centre Spatial de Liège, Université de Liège（列日大学空间研究中心）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）；Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale（巴黎萨克雷大学，法国国家科学研究中心，天体物理研究所）
Modelling spacecraft-emitted electrons measured by SWA-EAS experiment on board Solar Orbiter mission
Institute of Atmospheric Physics of the Czech Academy of Sciences（捷克科学院大气物理研究所）；Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）；Czech Technical University in Prague（布拉格捷克理工大学）；Mullard Space Science Laboratory, University College London（伦敦大学学院穆拉德空间科学实验室）；Swedish Institute of Space Physics (IRF)（瑞典空间物理研究所）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Univers（巴黎天文台 LIRA 实验室，PSL 大学，法国国家科学研究中心，索邦大学）
