Two‐Spacecraft Observations of Asymmetric Martian Bow Shock: Conjunctions of Tianwen‐1 and MAVEN

Long Cheng; Yuming Wang; Robert Lillis; Jasper Halekas; Benoit Langlais; Tielong Zhang; Jacob R. Gruesbeck; David L. Mitchell; Shannon Curry

doi:10.1029/2024JA033185

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Two‐Spacecraft Observations of Asymmetric Martian Bow Shock: Conjunctions of Tianwen‐1 and MAVEN

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Two‐Spacecraft Observations of Asymmetric Martian Bow Shock: Conjunctions of Tianwen‐1 and MAVEN

Long Cheng, Yuming Wang, Robert Lillis, Jasper Halekas, Benoit Langlais, Tielong Zhang, Jacob R. Gruesbeck, David L. Mitchell and Shannon Curry

Journal of geophysical research. Space physics, Vol.129(9), e2024JA033185

09/2024

DOI: 10.1029/2024JA033185

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Abstract

Abstract The Martian bow shock has been extensively studied through magnetic field and plasma instrument observations from various Mars space missions. However, prior investigations primarily involve statistical analyses based on single spacecraft crossings, leaving the asymmetry of the Martian bow shock unstudied through simultaneous two‐spacecraft observations. In this study, utilizing simultaneous observations from Tianwen‐1 and MAVEN, we examine the instantaneous asymmetry of the Martian bow shock. We present the asymmetry of the Martian bow shock in the Mars‐Solar‐Electric and Mars‐Solar‐Orbital reference frames, possibly influenced by the solar wind motional electric field and Martian crustal magnetic field, respectively. Moreover, we suggest that the bow shock exhibits increased asymmetry under stronger solar wind motional electric field conditions. This study highlights how a two‐point observation approach offers valuable insights into the dynamic behavior of the Martian induced magnetosphere. Plain Language Summary Scientists have been studying the Martian bow shock, which slows down the solar wind from supersonic to subsonic, using instruments on different Mars missions. But most studies only use data from one spacecraft, so we don't know much about how the bow shock varies in different places at the same time. In this study, we looked at data from two spacecraft, Tianwen‐1 and MAVEN, at the same time to see if we could find any differences. We found that the bow shock is different in the northern and southern parts of Mars in different reference frames, and this might be because of the solar wind electric field and the Martian crustal field. We also noticed that the bow shock is more different when the solar wind electric field is stronger. Such two‐spacecraft observations helps us understand more about how the magnetic environment around Mars works. Key Points We investigated the asymmetry of Martian bow shock utilizing two‐spacecraft observations at distinct locations The dayside Martian crustal field may induce the north‐south asymmetry of the bow shock The solar wind electric field may cause bow shock asymmetry in the Mars‐Solar‐Electric frame, with stronger fields increasing the effect

Mars

magnetosphere

bow shock

crustal magnetic field

Tianwen-1

MAVEN

Details

Title: Subtitle: Two‐Spacecraft Observations of Asymmetric Martian Bow Shock: Conjunctions of Tianwen‐1 and MAVEN
Creators: Long Cheng - University of California, Berkeley
Yuming Wang - University of Science and Technology of China
Robert Lillis - University of California, Berkeley
Jasper Halekas - Department of Physics and Astronomy University of Iowa Iowa City IA USA
Benoit Langlais - Laboratoire de Planétologie et Géosciences
Tielong Zhang - University of Science and Technology of China
Jacob R. Gruesbeck - Goddard Space Flight Center
David L. Mitchell - University of California, Berkeley
Shannon Curry - University of Colorado Boulder
Resource Type: Journal article
Publication Details: Journal of geophysical research. Space physics, Vol.129(9), e2024JA033185
DOI: 10.1029/2024JA033185
ISSN: 2169-9380
eISSN: 2169-9402
Publisher: AMER GEOPHYSICAL UNION
Grant note: University of Science and Technology of China: 42130204, 42188101, 42404164 NSFC: XDB41000000 Strategic Priority Program of CAS: GZC20241624
We thank all the individuals who contribute to the science data used in this work. The authors from USTC are supported by the grants from NSFC (42130204, 42188101 and 42404164), the Strategic Priority Program of CAS (XDB41000000) and the Postdoctoral Fellowship Program of CPSF (GZC20241624). LC thanks the support of the Excellent Doctoral Overseas Study Program of USTC. YW is particularly grateful for the support of the New Cornerstone Science Foundation through the Xplorer prize. RL's effort was supported by the Emirates Mars Mission.
Language: English
Date published: 09/2024
Academic Unit: Physics and Astronomy
Record Identifier: 9984719270302771

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