SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo

Orsini, S.; Livi, S.; Lichtenegger, Herbert; Barabash, S.; Milillo, A.; Angelis, E. De; Phillips, Mark L. F.; Laky, G.; Wieser, Martin; Olivieri, A.; Plainaki, C.; Ho, G. C.; Killen, R. M.; Slavin, J. A.; Würz, Peter; Berthelier, J. J.; Dandouras, I.; Kallio, Esa; McKenna‐Lawlor, S.; Szalai, Sándor; Torkar, K.; Вайсберг, О. Л.; Allegrini, F.; Daglis, Ioannis A.; Dong, Chuanfei; Escoubet, C. P.; Fatemi, Shahab; Fränz, M.; Ivanovski, S.; Krupp, N.; Lämmer, H.; Leblanc, François; Mangano, V.; Mura, A.; Nilsson, Hans; Raines, J. M.; Rispoli, Rosanna; Sarantos, M.; Smith, H. T.; Szegö, K.; Aronica, A.; Camozzi, Fabio; Lellis, A. M. Di; Fremuth, G.; Giner, F.; Gurnee, R. S.; Hayes, J. R.; Jeszenszky, H.; Tominetti, F.; Trantham, Bradley J.; Baláž, J.; Baumjohann, W.; Brienza, Daniele; Bührke, U.; Bush, M. D.; Cantatore, M.; Cibella, Sara; Colasanti, L.; Cremonese, Gabriele; Cremonesi, L.; D’Alessandro, Marco; Delcourt, Dominique; Delva, M.; Desai, M. I.; Famá, M.; Ferris, Monty J.; Fischer, Henning; Gaggero, A.; Gamborino, Diana; Garnier, Philippe; Gibson, William C.; Goldstein, R.; Grandé, M.; Гришин, В.А.; Haggerty, D. K.; Holmström, Mats; Horváth, I.; Hsieh, K. C.; Jacques, A. D.; Johnson, R. E.; Kazakov, Adrian; Kecskeméty, K.; Krüger, Harald; Kürbisch, C.; Lazzarotto, F.; Leblanc, Frédéric; Leichtfried, M.; Leoni, R.; Loose, Alexander; Maschietti, D.; Massetti, S.; Mattioli, F.; Miller, G.; Moissenko, D.; Morbidini, Alfredo; Noschese, R.; Nuccilli, F.; Nunez, C.; Paschalidis, N.; Persyn, S.; Piazza, Daniele; Oja, Magnus; Rynö, J.; Schmidt, W.; Scheer, J.; Shestakov, A.; Шувалов, С. Д.; Seki, K.; Selci, S.; Smith, K. D.; Sordini, R.; Svensson, Johan; Szalai, L.; Toublanc, D.; Urdiales, C.; Varsani, A.; Vertolli, N.; Wallner, R.; Wahlstroem, P.; Wilson, Paul; Zampieri, S.

doi:10.1007/s11214-020-00787-3

Cited by 27 publications

(24 citation statements)

References 105 publications

(183 reference statements)

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“…On magnetosphere-planet's surface coupling. MPO/Search for Exosphere Refilling and Emitted Neutral Abundances (SERENA) [Orsini et al, 2021], provide comprehensive measurements of low-energy (~ eV) and high-energy (up to 5 keV) neutrals and their elemental compositions in the exosphere near the planet. The comprehensive measurements of temperature profile and spatial distribution can help to identify the different releasing processes of exospheric particles and the dynamics of planetary exosphere.…”

Section: Future Bepicolombo Opportunitiesmentioning

confidence: 99%

Review of Mercury’s dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres

Sun

Dewey

Aizawa

et al. 2021

Sci. China Earth Sci.

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This review paper summarizes the research of Mercury’s magnetosphere in the Post-MESSENGER era and compares its dynamics to those in other planetary magnetospheres, especially to those in Earth’s magnetosphere. This review starts by introducing the planet Mercury, including its interplanetary environment, magnetosphere, exosphere, and conducting core. The frequent and intense magnetic reconnection on the dayside magnetopause, which is represented by the flux transfer event “shower”, is reviewed on how they depend on magnetosheath plasma β and magnetic shear angle across the magnetopause, following by how it contributes to the flux circulation and magnetosphere-surface-exosphere coupling. In the next, Mercury’s magnetosphere under extreme solar events, including the core induction and the reconnection erosion on the dayside magnetosphere, the responses of the nightside magnetosphere, are reviewed. Then, the dawn-dusk properties of the plasma sheet, including the features of the ions, the structure of the current sheet, and the dynamics of magnetic reconnection, are summarized. The last topic is devoted to the particle energization in Mercury’s magnetosphere, which includes the energization of the Kelvin-Helmholtz waves on the magnetopause boundaries, reconnection-generated magnetic structures, and the cross-tail electric field. In each chapter, the last section discusses the open questions related to each topic, which can be considered by the simulations and the future spacecraft mission. We end this paper by summarizing the future BepiColombo opportunities, which is a joint mission of ESA and JAXA and is en route to Mercury.

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Section: Future Bepicolombo Opportunitiesmentioning

confidence: 99%

Review of Mercury’s dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres

Sun

Dewey

Aizawa

et al. 2021

Sci. China Earth Sci.

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“…While this is coincidentally comparable to the production rate for Ca neutrals in the dawn source (10 23 s −1 ) measured by Burger et al (2014), this is not a like-for-like comparison and the production rate of neutrals by ESD is likely to be much lower. Precipitating electrons could plausibly slightly enhance the production of ions in spatially organized regions, and joint observations (Milillo et al, 2020) between Bepi-Colombo's suite of exospheric instruments (PHEBUS (Quémerais et al, 2020), SERENA (Orsini et al, 2021), MSASI (Yoshikawa et al, 2010)) as well as XRS' counterpart MIXS (Bunce et al, 2020), are needed to be able to separate any contribution from ESD.…”

Section: Exospherementioning

confidence: 99%

MESSENGER X‐Ray Observations of Electron Precipitation on the Dayside of Mercury

et al. 2022

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The cruise phase involved six planetary gravity assist maneuvers, three of which involved Mercury. After an extremely successful, twice-extended four-year mission, producing many ground-breaking results (see for example Solomon et al., 2018), the probe was de-orbited and impacted the planetary surface on 30 April 2015.In order to study the planet's magnetosphere as well as its surface, MESSENGER's orbit was highly elliptical and near-polar, with a periapsis altitude of 200-500 km over the northern pole and an apoapsis of 15,000 or 10,000 km (before and after an orbit adjustment on 20 April 2012) above the southern hemisphere. The orbit plane was fixed with respect to the line of apsides of the Mercury orbit, and as such the planet rotated underneath the spacecraft approximately every 118 spacecraft orbits (McAdams et al., 2007) -one Mercury sidereal dayproviding global coverage.The X-Ray Spectrometer, XRS (Schlemm et al., 2007), was part of the MESSENGER surface geochemistry suite of instruments. It was a gas proportional counter-based X-ray fluorescence spectrometer with a 12° hexagonal field of view, using three cylinders (GPCs 1, 2 and 3) filled with an Ar/CH 4 mixture, two of which (GPCs 1 and 2) were equipped with elemental filters to allow separation of the Mg/Al/Si peaks in the range 1.2-1.8 keV. XRS was paired with the Solar Assembly for X-rays (SAX), a Si PIN diode operating as a solar X-ray monitor. SAX was mounted in the spacecraft sunshield and as such was always pointing within 12° of the spacecraft-Sun

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“…Similarly, whereas a high mass resolution would enable some potential ambiguities to be resolved if the molecules happened to overlap in mass space, a mass resolution (M/ΔM) of ∼100 is reasonable for a small NMS. Finally, the sensitivity of the NMS needs to be high, of order one count per second at density of 10 cm −3 (Orsini et al 2021). The analog used for this mission concept study is Strofio on the BepiColombo mission (Orsini et al 2021).…”

Section: Neutral Mass Spectrometer (Nms)mentioning

confidence: 99%

Science Goals and Mission Concept for a Landed Investigation of Mercury

et al. 2022

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Mercury holds valuable clues to the distribution of elements at the birth of the solar system and how planets form and evolve in close proximity to their host stars. This Mercury Lander mission concept returns in situ measurements that address fundamental science questions raised by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission’s pioneering exploration of Mercury. Such measurements are needed to understand Mercury's unique mineralogy and geochemistry, characterize the proportionally massive core's structure, measure the planet's active and ancient magnetic fields at the surface, investigate the processes that alter the surface and produce the exosphere, and provide ground truth for remote data sets. The mission concept achieves one full Mercury year (∼88 Earth days) of surface operations with an 11-instrument, high-heritage payload delivered to a landing site within Mercury's widely distributed low-reflectance material, and it addresses science goals encompassing geochemistry, geophysics, the Mercury space environment, and geology. The spacecraft launches in 2035, and the four-stage flight system uses a solar electric propulsion cruise stage to reach Mercury in 2045. Landing is at dusk to meet thermal requirements, permitting ∼30 hr of sunlight for initial observations. The radioisotope-powered lander continues operations through the Mercury night. Direct-to-Earth communication is possible for the initial 3 weeks of landed operations, drops out for 6 weeks, and resumes for the final month. Thermal conditions exceed lander operating temperatures shortly after sunrise, ending operations. Approximately 11 GB of data are returned to Earth. The cost estimate demonstrates that a Mercury Lander mission is feasible and compelling as a New Frontiers–class mission.

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SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo

Cited by 27 publications

References 105 publications

Review of Mercury’s dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres

Review of Mercury’s dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres

MESSENGER X‐Ray Observations of Electron Precipitation on the Dayside of Mercury

Science Goals and Mission Concept for a Landed Investigation of Mercury

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