Publications

2024

• Structure and dynamics of the Hermean magnetosphere revealed by electron observations from the Mercury electron analyzer after the first three Mercury flybys of BepiColombo
  
  • Rojo M.
  • André N.
  • Aizawa S.
  • Sauvaud J.-A.
  • Saito Y.
  • Harada Y.
  • Fedorov A.
  • Penou E.
  • Barthe A.
  • Persson M.
  • Yokota S.
  • Mazelle C.
  • Hadid L. Z.
  • Delcourt D.
  • Fontaine D.
  • Fränz M.
  • Katra B.
  • Krupp N.
  • Murakami G.
  Astronomy & Astrophysics - A&A, EDP Sciences, 2024, 687, pp.A243. Context. The Mercury electron analyzer (MEA) obtained new electron observations during the first three Mercury flybys by BepiColombo on October 1, 2021 (MFB1), June 23 , 2022 (MFB2), and June 19, 2023 (MFB3). BepiColombo entered the dusk side magnetotail from the flank magnetosheath in the northern hemisphere, crossed the Mercury solar orbital equator around midnight in the magnetotail, traveled from midnight to dawn in the southern hemisphere near the closest approach, and exited from the post-dawn magnetosphere into the dayside magnetosheath.Aims. We aim to identify the magnetospheric boundaries and describe the structure and dynamics of the electron populations observed in the various regions explored along the flyby trajectories.Methods. We derive 4s time resolution electron densities and temperatures from MEA observations. We compare and contrast our new BepiColombo electron observations with those obtained from the Mariner 10 scanning electron spectrometer (SES) 49 yr ago.Results. A comparison to the averaged magnetospheric boundary crossings of MESSENGER indicates that the magnetosphere of Mercury was compressed during MFB1, close to its average state during MFB2, and highly compressed during MFB3. Our new MEA observations reveal the presence of a wake effect very close behind Mercury when BepiColombo entered the shadow region, a significant dusk-dawn asymmetry in electron fluxes in the nightside magnetosphere, and strongly fluctuating electrons with energies above 100s eV in the dawnside magnetosphere. Magnetospheric electron densities and temperatures are in the range of 10–30 cm−3 and above a few 100s eV in the pre-midnight-sector, and in the range of 1–100 cm−3 and well below 100 eV in the post-midnight sector, respectively.Conclusions. The MEA electron observations of different solar wind properties encountered during the first three Mercury flybys reveal the highly dynamic response and variability of the solar wind-magnetosphere interactions at Mercury. A good match is found between the electron plasma parameters derived by MEA in the various regions of the Hermean environment and similar ones derived in a few cases from other instruments on board BepiColombo. (10.1051/0004-6361/202449450)
  DOI : 10.1051/0004-6361/202449450
• Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys
  
  • Edberg Niklas
  • Andrews David
  • Boldú J. Jordi
  • Dimmock Andrew
  • Khotyaintsev Yuri
  • Kim Konstantin
  • Persson Moa
  • Auster Uli
  • Constantinescu Dragos
  • Heyner Daniel
  • Mieth Johannes
  • Richter Ingo
  • Curry Shannon
  • Hadid Lina
  • Pisa David
  • Sorriso-Valvo Luca
  • Lester Mark
  • Sánchez-Cano Beatriz
  • Stergiopoulou Katerina
  • Romanelli Norberto
  • Fischer David
  • Schmid Daniel
  • Volwerk Martin
  Journal of Geophysical Research Space Physics, American Geophysical Union/Wiley, 2024, 129 (10), pp.e2024JA032603. We analyze data from multiple flybys by the Solar Orbiter, BepiColombo, and Parker Solar Probe (PSP) missions to study the interaction between Venus' plasma environment and the solar wind forming the induced magnetosphere. Through examination of magnetic field and plasma density signatures we characterize the spatial extent and dynamics of Venus' magnetotail, focusing mainly on boundary crossings. Notably, we observe significant differences in boundary crossing location and appearance between flybys, highlighting the dynamic nature of Venus' magnetotail. In particular, during Solar Orbiter's third flyby, extreme solar wind conditions led to significant variations in the magnetosheath plasma density and magnetic field properties, but the increased dynamic pressure did not compress the magnetotail. Instead, it is possible that the increased EUV flux at this time rather caused it to expand in size. Key findings also include the identification of several far downstream bow shock (BS), or bow wave, crossings to at least 60 (1 = 6,052 km is the radius of Venus), and the induced magnetospheric boundary to at least 20 . These crossings provide insight into the extent of the induced magnetosphere. Pre‐existing models from Venus Express were only constrained to within 5 of the planet, and we provide modifications to better fit the far‐downstream crossings. The new model BS is now significantly closer to the central tail than previously suggested, by about 10 at 60 downstream. (10.1029/2024JA032603)
  DOI : 10.1029/2024JA032603
• Occurrence rate of equatorial Spread F and GPS ROTI in the ionospheric anomaly region over Vietnam
  
  • Pham Thi Thu Hong
  • Christine Amory Mazaudier
  • Le Huy Minh
  • Saito Susumu
  • Nguyen Thanh Dung
  • Luong Thi Ngoc
  • Luu Viet Hung
  • Nguyen Chien Thang
  • Nguyen Ha Thanh
  • Michi Nishioka
  • Septi Perwitasari
  Vietnam Journal of Earth Sciences, Vietnam Academy of Science and Technology (VAST), 2024, 46 (4), pp.553-569. This paper presents the first observations of the occurrence rates of Spread F and GPS total electron content (TEC) index (ROTI) over Vietnam at the equatorial trough and the northern tropical crest of ionization anomaly in the Asian sector. The data have been examined for the monthly and nighttime variations in the occurrence of these two data at Bac Lieu (9.28°N, 105.73°E, dip: 1.73°N) and Phu Thuy (21.03°N, 105.95°E, dip: 14.49°N) during 2023. For Bac Lieu, the monthly variation in the occurrence of the range Spread F (RSF) has the maxima in the February, May, and September months, while the mixed Spread-F (MSF) and ROTI occurrences exhibit a semiannual asymmetry with peaks in March/April and October. For the nighttime variation, occurrence peaks at 1915-1930 LT for RSF, at about 1945-2100 LT for MSF, and between 2030-2330 LT for ROTI. Regarding the frequency Spread F (FSF) occurrence, the maximum values in the monthly variation are in April, and the nighttime variation peaks at about 2115-2315 LT. For Phu Thuy, the monthly variation of RSF, MSF, and ROTI occurrences also exhibit a semiannual asymmetry with peaks in March/April and October. These peak magnitudes are largest for ROTI, moderate for MSF, and smallest for RSF. The nighttime variation of RSF, MSF, and ROTI occurrence peaks show intense season changes from winter to autumn at pre-midnight, spring at post-midnight, and summer at postmidnight. The FSF occurrences are more significant in summer than in other seasons, mainly after midnight. The time order appearance of the Spread F types at Bac Lieu and Phu Thuy is first of RSF, then MSF, and finally FSF. This could reflect that the formation mechanisms of Spread F types are different and require further research. Our observations also showed that the post-midnight occurrence of Spread F is much larger than ROTI at Bac Lieu and Phu Thuy. The monthly variations in occurrence rates of Spread F and ROTI at Bac Lieu and Phu Thuy are similar, but these occurrence rates at Bac Lieu are usually larger than at Phu Thuy. (10.15625/2615-9783/21368)
  DOI : 10.15625/2615-9783/21368