Direct Observations of Magnetic Reconnection in the Solar Wind Current Sheets near Mars

Authors:
  • CZChi Zhang
    Chi Zhang
  • CDChuanfei Dong
    Chuanfei Dong
  • XLXinmin Li
    Xinmin Li
  • HSHan-Wen Shen
    Han-Wen Shen
  • JHJasper Halekas
    Jasper Halekas
  • TPTai Phan
    Tai Phan
  • CMChristian Mazelle
    Christian Mazelle
  • YHYuki Harada
    Yuki Harada
  • HZHongyang Zhou
    Hongyang Zhou
  • JGJiawei Gao
    Jiawei Gao
  • LWLiang Wang
    Liang Wang
  • SCShannon Curry
    Shannon Curry
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Abstract
Magnetic reconnection is a fundamental and ubiquitous process in astrophysical plasmas that converts magnetic energy into plasma kinetic and thermal energy. Throughout the heliosphere, the solar wind is permeated with current sheets (CSs), providing a natural laboratory for investigating this process. Using measurements from NASA's Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft, we report the first direct observations of magnetic reconnection occurring within the solar wind CSs near Mars. Specifically, MAVEN observed the classic Petschek-type reconnection exhaust regions, evidenced by bifurcated magnetic field signatures and Alfvenic ion outflows. Notably, the observed exhaust region appears to be large-scale, significantly exceeding the typical thickness of solar wind CSs near Mars. This suggests that magnetic reconnection may significantly broaden the CS. Our results underscore the ubiquity of magnetic reconnection across heliocentric distances and may provide new insights into the large-scale evolution of the solar wind and the development of turbulence within it.
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