Closed magnetic topology in the Venusian magnetotail and ion escape at Venus

Shaosui Xu (), David L. Mitchell, Phyllis Whittlesey, Ali Rahmati, Roberto Livi, Davin Larson, Janet G. Luhmann, Jasper S. Halekas, Takuya Hara, James P. McFadden, Marc Pulupa, Stuart D. Bale, Shannon M. Curry and Moa Persson
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Shaosui Xu: University of California Berkeley
David L. Mitchell: University of California Berkeley
Phyllis Whittlesey: University of California Berkeley
Ali Rahmati: University of California Berkeley
Roberto Livi: University of California Berkeley
Davin Larson: University of California Berkeley
Janet G. Luhmann: University of California Berkeley
Jasper S. Halekas: University of Iowa
Takuya Hara: University of California Berkeley
James P. McFadden: University of California Berkeley
Marc Pulupa: University of California Berkeley
Stuart D. Bale: University of California Berkeley
Shannon M. Curry: University of California Berkeley
Moa Persson: Swedish Institute of Space Physics

Nature Communications, 2024, vol. 15, issue 1, 1-9

Abstract: Abstract Venus, lacking an intrinsic global dipole magnetic field, serves as a textbook example of an induced magnetosphere, formed by interplanetary magnetic fields (IMF) enveloping the planet. Yet, various aspects of its magnetospheric dynamics and planetary ion outflows are complex and not well understood. Here we analyze plasma and magnetic field data acquired during the fourth Venus flyby of the Parker Solar Probe (PSP) mission and show evidence for closed topology in the nightside and downstream portion of the Venus magnetosphere (i.e., the magnetotail). The formation of the closed topology involves magnetic reconnection—a process rarely observed at non-magnetized planets. In addition, our study provides an evidence linking the cold Venusian ion flow in the magnetotail directly to magnetic connectivity to the ionosphere, akin to observations at Mars. These findings not only help the understanding of the complex ion flow patterns at Venus but also suggest that magnetic topology is one piece of key information for resolving ion escape mechanisms and thus the atmospheric evolution across various planetary environments and exoplanets.

Date: 2024
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DOI: 10.1038/s41467-024-50480-0

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