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Nightside Martian Upper

In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species.

In Situ Heating of the Nightside Martian Upper Atmosphere and Ionosphere: The Role of Solar Wind Electron Precipitation

Nightside Martian Upper

Solar Wind (SW) electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere, potentially exerting an influence on its thermal structure.

Is Solar Wind electron precipitation a source of neutral heating in the nightside Martian upper atmosphere?

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Martian Upper sentence examples within martian upper atmosphere

martian upper atmosphere

In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species.

In Situ Heating of the Nightside Martian Upper Atmosphere and Ionosphere: The Role of Solar Wind Electron Precipitation

martian upper atmosphere

These observations have implications on the ion escape rates from the Martian upper atmosphere.

The impact of a stealth CME on the Martian topside ionosphere

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10.3847/1538-4357/abdbb0

In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species.

In Situ Heating of the Nightside Martian Upper Atmosphere and Ionosphere: The Role of Solar Wind Electron Precipitation

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10.1093/mnras/stab494

These observations have implications on the ion escape rates from the Martian upper atmosphere.

The impact of a stealth CME on the Martian topside ionosphere

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10.26464/epp2021012

Solar Wind (SW) electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere, potentially exerting an influence on its thermal structure.

Is Solar Wind electron precipitation a source of neutral heating in the nightside Martian upper atmosphere?

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10.1016/J.ICARUS.2021.114515

We study the high-altitude occurrence of Auger electrons in the Martian upper atmosphere during four solar flare events occurred on 19 October 2014, 24 March 2015, 04 May 2015, and 10 September 2017.

High altitude occurrence of Auger electrons in the Martian upper atmosphere during solar flares

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10.1016/j.icarus.2019.113498

We have simulated the 3D atomic hydrogen density in the Martian upper atmosphere and associated Jeans escape rate during Martian years 28 and 29.

Study of the hydrogen escape rate at Mars during Martian years 28 and 29 from comparisons between SPICAM/Mars express observations and GCM-LMD simulations

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10.1089/ast.2018.1943

Here, we assess whether aerobic methanotrophy is a potentially viable metabolism in the martian upper regolith, by calculating metabolic energy gain rates under assumed conditions of martian surface temperature, pressure, and atmospheric composition.

Potential for Aerobic Methanotrophic Metabolism on Mars

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Martian Upper - In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species. [1] These observations have implications on the ion escape rates from the Martian upper atmosphere. [2] Solar Wind (SW) electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere, potentially exerting an influence on its thermal structure. [3] We study the high-altitude occurrence of Auger electrons in the Martian upper atmosphere during four solar flare events occurred on 19 October 2014, 24 March 2015, 04 May 2015, and 10 September 2017. [4] We have simulated the 3D atomic hydrogen density in the Martian upper atmosphere and associated Jeans escape rate during Martian years 28 and 29. [5] Here, we assess whether aerobic methanotrophy is a potentially viable metabolism in the martian upper regolith, by calculating metabolic energy gain rates under assumed conditions of martian surface temperature, pressure, and atmospheric composition. [6]

Nightside Martian Upper

In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species. [1] Solar Wind (SW) electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere, potentially exerting an influence on its thermal structure. [2]

martian upper atmosphere

In the absence of solar radiation, precipitating electrons from the solar wind (SW) are generally thought to be the dominant source of energy deposition in the nightside Martian upper atmosphere, creating a patchy ionosphere and possibly also affecting the nightside thermal budget of various neutral and ionized species. [1] These observations have implications on the ion escape rates from the Martian upper atmosphere. [2] Solar Wind (SW) electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere, potentially exerting an influence on its thermal structure. [3] We study the high-altitude occurrence of Auger electrons in the Martian upper atmosphere during four solar flare events occurred on 19 October 2014, 24 March 2015, 04 May 2015, and 10 September 2017. [4] We have simulated the 3D atomic hydrogen density in the Martian upper atmosphere and associated Jeans escape rate during Martian years 28 and 29. [5]