Новые результаты исследования радиации на борту TGO Экзомарс в 2018–2023 г.

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Abstract

В статье дано краткое описание дозиметра Liulin-MO, который входит в состав прибора FREND (Fine Resolution Epithermal Neutron Detector), установленного на космическом аппарате TGO (Trace Gas Orbiter) миссии ExoMars-2016. С апреля 2018 г. TGO работает на орбите вокруг Марса. Представлены данные о радиационной обстановке на орбите Марса на фазе спада 24-го цикла солнечной активности и фазе роста 25-го цикла. В рассматриваемый период наблюдался максимум потока и мощности дозы, обусловленный галактическими космическими лучами (ГКЛ). В период с июля 2021 г. по март 2023 г. дозиметром Люлин-МО зарегистрировано восемь возрастаний потоков частиц и мощности дозы от солнечных протонных событий (СПС). Представлены данные о радиационной обстановке во время СПС на орбите Марса в июле 2021 г. – марте 2022 г., когда Марс находился на противоположной по отношению к Земле стороне от Солнца. Проведено сравнение потоков частиц, измеренных на орбитах около Земли и Марса.

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About the authors

Й. Семкова

Институт космических исследований и технологии Болгарской академии наук

Author for correspondence.
Email: jsemkova@stil.bas.bg
Bulgaria, София

В. Бенгин

Государственный научный центр Российской Федерации Институт медико-биологических проблем РАН

Email: v_benghin@mail.ru
Russian Federation, Москва

Р. Колева

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

К. Крастев

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

Ю. Матвейчук

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

Б. Томов

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

Н. Банков

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

С. Малчев

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

Ц. Дачев

Институт космических исследований и технологии Болгарской академии наук

Email: jsemkova@stil.bas.bg
Bulgaria, София

В. Шуршаков

Государственный научный центр Российской Федерации Институт медико-биологических проблем РАН

Email: v_benghin@mail.ru
Russian Federation, Москва

С. Дробышев

Государственный научный центр Российской Федерации Институт медико-биологических проблем РАН

Email: v_benghin@mail.ru
Russian Federation, Москва

И. Митрофанов

Институт космических исследований РАН

Email: mitrofanov@np.cosmos.ru
Russian Federation, Москва

Д. Головин

Институт космических исследований РАН

Email: mitrofanov@np.cosmos.ru
Russian Federation, Москва

А. Козырев

Институт космических исследований РАН

Email: mitrofanov@np.cosmos.ru
Russian Federation, Москва

М. Литвак

Институт космических исследований РАН

Email: mitrofanov@np.cosmos.ru
Russian Federation, Москва

М. Мокроусов

Институт космических исследований РАН

Email: mitrofanov@np.cosmos.ru
Russian Federation, Москва

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Supplementary files

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2. Fig. 1. Schematic representation of the arrangement of detectors in the Liulin-MO device (Semkova et al., 2021).

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3. Fig. 2. Location of the Liulin-MO dosimeter on the FREND device.

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4. Fig. 3. Detector shielding functions (left panel) and the corresponding dependences of the effective proton detection area on their energy (right panel).

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5. Fig. 4. Solar activity during the periods of measurements by the Liulin-MO instrument. The shaded areas show the periods of Liulin-MO measurements: on the flight path, MCO1 and MCO2 – the left rectangle, and on the scientific, circular orbit of Mars – the right rectangle.

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6. Fig. 5. Graphs of average daily values ​​of particle fluxes and radiation dose rates measured by the Liulin-MO device.

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7. Fig. 6. Relative positions of the Sun, Earth, Mars and model lines of force of the interplanetary magnetic field connecting the Earth and Mars with the Sun on October 28, 2021.

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8. Fig. 7. Time dependence of the proton flux near the Earth and the particle flux measured near Mars. The curve is the flux of protons with energies greater than 50 MeV, registered near the Earth by the GOES-16 spacecraft. The dots are the particle flux measured by the pair of detectors A and B of the Liulin-MO instrument near Mars.

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9. Fig. 8. Dose rates to silicon (upper panel) and accumulated doses to water from solar energetic particles (lower panel) measured at different locations in the Solar System during the SPE on October 28, 2021. The data are taken from (Guo et al., 2023). The notations from bottom to top correspond to: RAD instrument operating on the surface of Mars, Liulin-MO instrument in orbit around Mars, RAMIS instrument operating in polar orbit near Earth, LND instrument operating on the lunar surface, CRaTER instrument in lunar orbit.

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10. Fig. 9. Relative positions of the Sun, Earth, Mars and model lines of force of the interplanetary magnetic field connecting the Earth and Mars with the Sun on February 15, 2022.

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11. Fig. 10. Comparison of particle fluxes recorded by the GOES and ExoMars spacecraft during the SPE on February 15, 2022. The curve is the flux of protons with energies greater than 50 MeV recorded near Earth by the GOES-16 spacecraft. The dots are the flux of particles measured by the pair of detectors A and B of the Liulin-MO instrument near Mars.

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12. Fig. 11. Mutual arrangement of the Sun, Earth, Mars and model lines of force of the interplanetary magnetic field connecting the Earth and Mars with the Sun on February 24 and 25, 2023.

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13. Fig. 12. Comparison of particle fluxes recorded by the GOES-16 and ExoMars spacecraft during the SPE on February 24–25, 2023. Curves are fluxes of protons with energies greater than 50 MeV and greater than 100 MeV, respectively, recorded near Earth by the GOES-16 spacecraft. Dots are the particle fluxes measured by the pair of detectors A and B of the Liulin-MO instrument near Mars.

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