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The Day the Solar Wind Disappeared at Mars.

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Title: The Day the Solar Wind Disappeared at Mars.
Authors: Halekas, J. S.1 (AUTHOR) jasper-halekas@uiowa.edu, Shaver, S.2 (AUTHOR), Azari, A. R.3 (AUTHOR), Fowler, C. M.4 (AUTHOR), Ma, Y.5 (AUTHOR), Xu, S.3 (AUTHOR), Andersson, L.2 (AUTHOR), Bertucci, C.6 (AUTHOR), Curry, S. M.3 (AUTHOR), Dong, C.7 (AUTHOR), Dong, Y.2 (AUTHOR), Fang, X.2 (AUTHOR), Garnier, P.8 (AUTHOR), Hanley, K. G.3 (AUTHOR), Hara, T.3 (AUTHOR), Howard, S. K.9,10 (AUTHOR), Hughes, A.9 (AUTHOR), Lillis, R. J.3 (AUTHOR), Lee, C. O.3 (AUTHOR), Luhmann, J. G.3 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Dec2023, Vol. 128 Issue 12, p1-14. 14p.
Subject Terms: Solar wind, Mars (Planet), Mach number, Plasma instabilities, Supersonic flow, Solar system
Abstract: In December 2022, an extremely low‐density solar wind stream encountered first the Earth and then Mars, shortly after the radial alignment of the two planets (i.e., Mars opposition). As the low‐density stream passed Mars, the properties of the Mars‐solar wind interaction changed dramatically in response to the low solar wind Alfvénic Mach number and dynamic pressure. The Martian magnetosphere and its boundaries expanded by thousands of kilometers, extending outside of the nominal average bow shock location. The low upstream Mach number resulted in a low ratio of plasma to magnetic field pressure in the magnetosheath, allowing the formation of a very high but stable ion temperature anisotropy, together with a very low level of electromagnetic instabilities. Meanwhile, the decrease in solar wind dynamic pressure caused the Martian upper ionosphere at the terminator to transition from a magnetized state to an unmagnetized state. This event provides an opportunity to study a unique end‐member state of the Mars‐solar wind interaction. Plain Language Summary: The solar wind consists of a supersonic flow of hot ionized gas (plasma) from the Sun that flows outward through the solar system. The solar wind interacts with planetary atmospheres and magnetic fields, which form shielded regions known as magnetospheres. The characteristics of the solar wind, including its density and speed, vary over a wide range. The shape, extent, and physical characteristics of planetary magnetospheres in turn respond to these changes in the solar wind. In this work, we study the response of the Martian magnetosphere to an extremely low‐density solar wind stream. During the passage of this stream, the Martian magnetosphere expanded by thousands of kilometers, and its physical characteristics changed dramatically. This event reveals a unique outlier state for the Mars‐solar wind interaction. Key Points: An extremely low‐density solar wind stream encountered the Earth and Mars just after Mars opposition in December 2022The Martian magnetosheath developed very unusual properties, with a low level of plasma instabilities and a high ion anisotropyThe Martian magnetosphere and its boundaries expanded by thousands of km, extending outside of the location of the nominal bow shock [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: The Day the Solar Wind Disappeared at Mars.
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  Data: <searchLink fieldCode="AR" term="%22Halekas%2C+J%2E+S%2E%22">Halekas, J. S.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> jasper-halekas@uiowa.edu</i><br /><searchLink fieldCode="AR" term="%22Shaver%2C+S%2E%22">Shaver, S.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Azari%2C+A%2E+R%2E%22">Azari, A. R.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Fowler%2C+C%2E+M%2E%22">Fowler, C. M.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ma%2C+Y%2E%22">Ma, Y.</searchLink><relatesTo>5</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Xu%2C+S%2E%22">Xu, S.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Andersson%2C+L%2E%22">Andersson, L.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Bertucci%2C+C%2E%22">Bertucci, C.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Curry%2C+S%2E+M%2E%22">Curry, S. M.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Dong%2C+C%2E%22">Dong, C.</searchLink><relatesTo>7</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Dong%2C+Y%2E%22">Dong, Y.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Fang%2C+X%2E%22">Fang, X.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Garnier%2C+P%2E%22">Garnier, P.</searchLink><relatesTo>8</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Hanley%2C+K%2E+G%2E%22">Hanley, K. G.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Hara%2C+T%2E%22">Hara, T.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Howard%2C+S%2E+K%2E%22">Howard, S. K.</searchLink><relatesTo>9,10</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Hughes%2C+A%2E%22">Hughes, A.</searchLink><relatesTo>9</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Lillis%2C+R%2E+J%2E%22">Lillis, R. J.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Lee%2C+C%2E+O%2E%22">Lee, C. O.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Luhmann%2C+J%2E+G%2E%22">Luhmann, J. G.</searchLink><relatesTo>3</relatesTo> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Space+Physics%22">Journal of Geophysical Research. Space Physics</searchLink>. Dec2023, Vol. 128 Issue 12, p1-14. 14p.
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  Data: In December 2022, an extremely low‐density solar wind stream encountered first the Earth and then Mars, shortly after the radial alignment of the two planets (i.e., Mars opposition). As the low‐density stream passed Mars, the properties of the Mars‐solar wind interaction changed dramatically in response to the low solar wind Alfvénic Mach number and dynamic pressure. The Martian magnetosphere and its boundaries expanded by thousands of kilometers, extending outside of the nominal average bow shock location. The low upstream Mach number resulted in a low ratio of plasma to magnetic field pressure in the magnetosheath, allowing the formation of a very high but stable ion temperature anisotropy, together with a very low level of electromagnetic instabilities. Meanwhile, the decrease in solar wind dynamic pressure caused the Martian upper ionosphere at the terminator to transition from a magnetized state to an unmagnetized state. This event provides an opportunity to study a unique end‐member state of the Mars‐solar wind interaction. Plain Language Summary: The solar wind consists of a supersonic flow of hot ionized gas (plasma) from the Sun that flows outward through the solar system. The solar wind interacts with planetary atmospheres and magnetic fields, which form shielded regions known as magnetospheres. The characteristics of the solar wind, including its density and speed, vary over a wide range. The shape, extent, and physical characteristics of planetary magnetospheres in turn respond to these changes in the solar wind. In this work, we study the response of the Martian magnetosphere to an extremely low‐density solar wind stream. During the passage of this stream, the Martian magnetosphere expanded by thousands of kilometers, and its physical characteristics changed dramatically. This event reveals a unique outlier state for the Mars‐solar wind interaction. Key Points: An extremely low‐density solar wind stream encountered the Earth and Mars just after Mars opposition in December 2022The Martian magnetosheath developed very unusual properties, with a low level of plasma instabilities and a high ion anisotropyThe Martian magnetosphere and its boundaries expanded by thousands of km, extending outside of the location of the nominal bow shock [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
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  Data: <i>Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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      – SubjectFull: Mach number
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