Oxygen Atom Escape from the Martian Atmosphere during Proton Auroral Events

Shematovich, V. I.; Kalinicheva, E. S.

doi:10.1134/s1063772920080089

Cited by 8 publications

(4 citation statements)

References 28 publications

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“…When numerous H‐ENAs and solar wind protons precipitate into the Martian ionosphere, in combination with an enhanced solar wind electric field (deduced from the enhanced IMF B T ) and inward compression of Martian boundaries (i.e., bow shock, magnetic pileup boundary, and photoelectron boundary) under high P dyn , the most obvious effect is to cause ions to escape through ionization, energization/acceleration, sputtering and/or pick‐up processes (Jakosky, Grebowsky, et al., 2015, 2017; Lundin et al., 2004; Rahmati et al., 2017; Shematovich, 2021; Shematovich & Kalinicheva, 2020). This in turn causes large amounts of ions to be stripped away from the Martian ionosphere to space.…”

Section: Response Of Martian Atmosphere/ionospherementioning

confidence: 99%

Martian Proton Aurora Brightening Reveals Atmospheric Ion Loss Intensifying

Fan

Hughes

et al. 2023

Geophysical Research Letters

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The Martian proton aurora is a distinct aurora phenomenon resulting from the direct deposition of solar wind energy into Mars' dayside atmosphere. What solar wind parameters influence the aurora activity in the short term is yet unknown, as are the associated repercussions in the Martian atmospheric ion loss. Here we present observational evidence of synchronized proton aurora brightening and atmospheric ion loss intensifying on Mars, controlled by solar wind dynamic pressure, using observations by the Mars Atmosphere and Volatile Evolution spacecraft. The solar wind dynamic pressure possibly has a saturation effect on brightening proton aurora. Significant erosion of the Martian ionosphere during periods of high dynamic pressure indicates at least five‐to‐tenfold increase in atmospheric ion loss. An empirical relationship between ion escape rate and auroral emission enhancement is established, providing a new proxy of Mars' atmospheric ion loss with optical imaging that may be used remotely and with greater flexibility.

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Section: Response Of Martian Atmosphere/ionospherementioning

confidence: 99%

Martian Proton Aurora Brightening Reveals Atmospheric Ion Loss Intensifying

Fan

Hughes

et al. 2023

Geophysical Research Letters

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“…The behavior of ENAs in the Martian environment has been modeled by various groups over the past two decades (Holmström et al., 2002; Kallio & Barabash, 2001; Kallio et al., 1997; Shematovich et al., 2011; Shematovich & Kalinicheva, 2020; Wang et al., 2018). Kallio et al.…”

Section: Introductionmentioning

confidence: 99%

“…The behavior of ENAs in the Martian environment has been modeled by various groups over the past two decades (Holmström et al, 2002;Kallio & Barabash, 2001;Kallio et al, 1997;Shematovich et al, 2011;Shematovich & Kalinicheva, 2020;Wang et al, 2018). Kallio et al (1997) were the first group to develop a comprehensive model of charge exchange between solar wind protons and neutral atoms in the atmosphere of Mars based on Phobos 2 measurements.…”

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confidence: 99%

Precipitating Solar Wind Hydrogen as Observed by the MAVEN Spacecraft: Distribution as a Function of Column Density, Altitude, and Solar Zenith Angle

Henderson¹,

Halekas

Lillis

et al. 2021

JGR Planets

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Because it lacks a global magnetic field, Mars's atmosphere is subject to direct interaction with the solar wind, which can provide energy for atmospheric constituents to escape the planet's gravitational pull through a variety of processes, including photochemical escape, sputtering, and pick up ion escape Lillis et al., 2015). Evidence suggests that this solar wind interaction has played a major role in changing Mars from a warm, water rich environment to the cold, dry planet we observe today (Jakosky et al., 2018). Mars's atmosphere is comprised primarily of CO 2 but also exhibits a hydrogen corona that extends past the planet's bow shock (Anderson, 1974;Anderson & Hord, 1971). This hydrogen corona is subject to direct interaction with the solar wind by means of charge exchange, providing us with a unique laboratory to observe and characterize various phenomena within the upper Martian atmosphere.As solar wind protons propagate toward Mars, they can charge exchange with neutral hydrogen atoms in the planet's corona, resulting in energetic neutral atoms (ENAs) with the solar wind speed (Kallio et al., 1997). These ENAs can then travel toward the planet without being affected by electromagnetic forces and thus

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“…In addition, the appearance and the intensity of proton polar aurorae can indirectly indicate variations occurring in objects mentioned above and follow the changes occurring in the dynamics of underlying atmospheric layers (such as the neutral CO 2 atmosphere and the dust activity). Studying Martian proton aurorae can also supply an additional understanding of the loss and evolution of the atmosphere, since the processes responsible for the formation of Martian polar aurorae (for example, interactions between the solar wind and the extended hydrogen corona) are also responsible for the loss of the atmosphere [5].…”

Section: Introductionmentioning

confidence: 99%

Kinetic Calculations of the Charge Exchange Efficiency for Solar Wind Protons in the Extended Martian Hydrogen Corona

Shematovich

Bisikalo

2020

Astron. Rep.

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Model calculations of the charge exchange efficiency for solar wind protons colliding with hydrogen atoms of the extensive Martian corona are presented. It is shown that the energy spectrum of hydrogen atoms penetrating in the Martian atmosphere is identical to the spectrum of protons of the unperturbed solar wind. The charge exchange efficiency varies from 2 to 4% depending on the boundary location of the Martian induced magnetosphere. The presented calculations, combined with the kinetic model of proton precipitation proposed earlier, enable us to follow all proton penetration stages of the unperturbed solar wind into denser atmospheric layers and to estimate the characteristics of proton aurorae observed on the Mars.

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Oxygen Atom Escape from the Martian Atmosphere during Proton Auroral Events

Cited by 8 publications

References 28 publications

Martian Proton Aurora Brightening Reveals Atmospheric Ion Loss Intensifying

Martian Proton Aurora Brightening Reveals Atmospheric Ion Loss Intensifying

Precipitating Solar Wind Hydrogen as Observed by the MAVEN Spacecraft: Distribution as a Function of Column Density, Altitude, and Solar Zenith Angle

Kinetic Calculations of the Charge Exchange Efficiency for Solar Wind Protons in the Extended Martian Hydrogen Corona

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