Solar System Ionospheres

Witasse, Olivier; Cravens, T. E.; Mendillo, M.; Moses, J. I.; Kliore, A. J.; Nagy, Andrew F.; Бреус, Т. К.

doi:10.1007/s11214-008-9395-3

“…Witasse et al, 2008). The maximum density of this layer is typically located between 125-140 km altitude with a characteristic electron density range between 0.4•10 11 and 2•10 11 electrons per m -3 , and is dependent on solar zenith angle (SZA) and solar activity conditions (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The maximum density of this layer is typically located between 125-140 km altitude with a characteristic electron density range between 0.4•10 11 and 2•10 11 electrons per m -3 , and is dependent on solar zenith angle (SZA) and solar activity conditions (e.g. Gurnett et al, 2005;Witasse et al, 2008;Peter et al, 2014;Sánchez-Cano, 2014). Since EUV photons are greatly attenuated at lower atmospheric altitudes, soft X-ray solar photons of 10 nm are the dominant flux able to ionize the lower atmosphere, with a significant contribution due to secondary electrons and photoelectrons.…”

Section: Introductionmentioning

confidence: 99%

An observational study of the response of the upper atmosphere of Mars to lower atmospheric dust storms

Withers

¹

,

Pratt

²

2013

Icarus

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Solar cycle variations in solar radiation create notable changes in the Martian ionosphere, which have been analysed with Mars Express plasma datasets in this paper. In general, lower densities and temperatures of the ionosphere are found during the low solar activity phase, while higher densities and temperatures are found during the high solar activity phase. In this paper, we assess the degree of influence of the long term solar flux variations in the ionosphere of Mars. Key words: solar cycle; ionosphere of Mars; TEC. Variaciones de la ionosfera de Marte debidas al ciclo solarResumen La radiación solar en cada fase del ciclo solar crea importantes variaciones en la ionosfera de Marte, las cuales son analizadas en este artículo con datos de la sonda Mars Express. En general, las densidades y temperaturas más bajas de la ionosfera se encuentran durante la fase de baja actividad solar, mientras que las densidades y temperaturas más elevadas se encuentran durante la fase de alta actividad solar. Este artículo evalúa el efecto que las variaciones del flujo solar tienen a largo plazo en la ionosfera. Palabras clave: ciclo solar; ionosfera de Marte; TEC.

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“…In many situations, photoionization by solar UV photons is the dominant source of atmospheric ions, but energetic particle radiation also plays a major role (notably for the nightside ionosphere and bodies at a greater distance from the Sun). Ionization can be caused by charged particles trapped in a planet's dipolar magnetic field precipitating into the upper atmosphere around the poles (e.g., Earth; reviewed by Lyons, 1997), or a moon if it is embedded in its parent planetary magnetosphere (e.g., Titan), as well as GCR and SEP cosmic rays arriving from beyond the magnetosphere (Kivelson and Russell, 1995; also see a recent review of solar system ionospheres by Witasse et al, 2008). Atmospheric ionization is very dynamic and variable over both space and time, being influenced in the short term and longer term by solar UV output and flares; CR variability; gamma-ray, X-ray, and energetic particle influx from supernovae in the stellar neighborhood; and passage of the Solar System through dense molecular clouds (Vasilyev et al, 2008).…”

Section: Interaction Of Cosmic Rays With Atmospherementioning

confidence: 99%

Ionizing Radiation and Life

Dartnell

¹

2011

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Ionizing radiation is a ubiquitous feature of the Cosmos, from exogenous cosmic rays (CR) to the intrinsic mineral radioactivity of a habitable world, and its influences on the emergence and persistence of life are wideranging and profound. Much attention has already been focused on the deleterious effects of ionizing radiation on organisms and the complex molecules of life, but ionizing radiation also performs many crucial functions in the generation of habitable planetary environments and the origins of life. This review surveys the role of CR and mineral radioactivity in star formation, generation of biogenic elements, and the synthesis of organic molecules and driving of prebiotic chemistry. Another major theme is the multiple layers of shielding of planetary surfaces from the flux of cosmic radiation and the various effects on a biosphere of violent but rare astrophysical events such as supernovae and gamma-ray bursts. The influences of CR can also be duplicitous, such as limiting the survival of surface life on Mars while potentially supporting a subsurface biosphere in the ocean of Europa. This review highlights the common thread that ionizing radiation forms between the disparate component disciplines of astrobiology.

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“…Witasse et al, 2008). The maximum density of this layer is typically located between 125-140 km altitude with a characteristic electron density range between 0.4•10 , and is dependent on solar zenith angle (SZA) and solar activity conditions (e.g.…”

Section: Introductionmentioning

confidence: 99%

Variaciones de la ionosfera de Marte debidas al ciclo solar

Sánchez–Cano

¹

,

Lester

²

,

Witasse

³

et al. 2016

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Solar cycle variations in solar radiation create notable changes in the Martian ionosphere, which have been analysed with Mars Express plasma datasets in this paper. In general, lower densities and temperatures of the ionosphere are found during the low solar activity phase, while higher densities and temperatures are found during the high solar activity phase. In this paper, we assess the degree of influence of the long term solar flux variations in the ionosphere of Mars. Key words: solar cycle; ionosphere of Mars; TEC. Variaciones de la ionosfera de Marte debidas al ciclo solarResumen La radiación solar en cada fase del ciclo solar crea importantes variaciones en la ionosfera de Marte, las cuales son analizadas en este artículo con datos de la sonda Mars Express. En general, las densidades y temperaturas más bajas de la ionosfera se encuentran durante la fase de baja actividad solar, mientras que las densidades y temperaturas más elevadas se encuentran durante la fase de alta actividad solar. Este artículo evalúa el efecto que las variaciones del flujo solar tienen a largo plazo en la ionosfera. Palabras clave: ciclo solar; ionosfera de Marte; TEC.

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Solar System Ionospheres

Cited by 56 publications

References 180 publications

An observational study of the response of the upper atmosphere of Mars to lower atmospheric dust storms

An observational study of the response of the upper atmosphere of Mars to lower atmospheric dust storms

Ionizing Radiation and Life

Variaciones de la ionosfera de Marte debidas al ciclo solar

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