Properties Of Mars’ Dayside Low-Altitude Induced Magnetic Field And Comparisons With Venus

Properties Of Mars’ Dayside Low-Altitude Induced Magnetic Field And Comparisons With Venus

The variation of Bmax with photo voltaic wind dynamic strain for Venus (left) and Mars (proper). For Venus, values derived from magnetized profiles are plotted as black triangles and values derived from unmagnetized profiles are plotted as blue circles. The crimson strains are energy regulation suits with slopes 0.57±0.13 for Venus (magnetized) and 0.45±0.02 for Mars. — physics.space-ph

Our analysis goal is to characterize Mars’ low-altitude (250 km) induced magnetic fields utilizing knowledge from NASA’s MAVEN (Mars Ambiance and Unstable EvolutioN) Mission.

We intention to evaluate how the induced magnetic fields behave below totally different photo voltaic zenith angles and photo voltaic wind circumstances, and moreover, perceive how planet-specific properties (similar to Mars crustal magnetism) alter the formation and construction of the magnetic fields. We then use knowledge from the Pioneer Venus Orbiter to match induced magnetic fields at Venus with these at Mars.

At Venus, the vertical construction of the magnetic subject tends to exist in one in every of two states (magnetized or unmagnetized) however we discover the induced fields at Mars are extra difficult, and we’re unable to make use of this straightforward classification scheme.

We additionally discover the low-altitude induced subject energy within the ionospheres of each Venus and Mars fluctuate with as cosine of the angle between photo voltaic wind velocity and the magnetic pileup boundary. The low-altitude subject energy at Venus tends to be larger than Mars. Nevertheless, Venus subject strengths are decrease than theoretical predictions assuming strain steadiness and negligible thermal strain.

For Mars, low-altitude subject strengths are larger than anticipated given these assumptions. Induced subject strengths exhibit a pattern with photo voltaic wind dynamic strain that’s per strain steadiness expectations at each planets, nonetheless there’s important uncertainty within the Venus match as a result of lack of upstream photo voltaic wind knowledge. Our outcomes spotlight main variations between the induced magnetic fields at Venus and Mars, suggesting planet-specific properties similar to dimension and the presence of crustal magnetism have an effect on the induced ionospheric magnetic fields at non magnetized planets.

Susanne Byrd, Zachary Girazian

Feedback: 20 pages, 7 figures. To be submitted to AGU Journal
Topics: House Physics (physics.space-ph); Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2311.18217 [physics.space-ph] (or arXiv:2311.18217v1 [physics.space-ph] for this model)
Submission historical past
From: Susanne Byrd
[v1] Thu, 30 Nov 2023 03:21:34 UTC (1,001 KB)
https://arxiv.org/abs/2311.18217
Astrobiology

Explorers Membership Fellow, ex-NASA House Station Payload supervisor/house biologist, Away Groups, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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