Dayglow on Mars: Kinetic modelling with SPICAM UV limb data

Simon, Cyril; Witasse, Olivier; Leblanc, François; Gronoff, Guillaume; Bertaux, Jean-Loup

doi:10.1016/j.pss.2008.08.012

Cited by 52 publications

(86 citation statements)

References 103 publications

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“…It has been adapted to several planets, becoming successively transsolo (Lummerzheim & Lilensten 1994), transcar (Lilensten & Blelly 2002), tran4 ) in the case of Earth, and, for orther planets, transTitan (Lilensten et al 2005a,b), transMars (Witasse et al 2003(Witasse et al , 2002Simon et al 2008), transVenus (Gronoff et al 2007. The transTitan code used here consists of primary production through photoabsorption and secondary production through electron impacts.…”

Section: The Transtitan Modelmentioning

confidence: 99%

Ionization processes in the atmosphere of Titan

Gronoff¹,

Lilensten²,

Desorgher

et al. 2009

A&A

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Context. The Cassini probe regularly passes in the vicinity of Titan, revealing new insights into particle precipitation thanks to the electron and proton spectrometer. Moreover, the Huygens probe has revealed an ionized layer at 65 km induced by cosmic rays. The impact of these different particles on the chemistry of Titan is probably very strong. Aims. In this article, we compute the whole ionization in the atmosphere of Titan: from the cosmic rays near the ground to the EUV in the upper atmosphere. The meteoritic layer is not taken into account. Methods. We used the transTitan model to compute the electron and EUV impact, and the planetocosmics code to compute the influence of protons and oxygen ions. We coupled the two models to study the influence of the secondary electrons obtained by planetocosmics through the transTitan code. The resulting model improves the accuracy of the calculation through the transport of electrons in the atmosphere. Results. The whole ionization is computed and studied in details. During the day, the cosmic ray ionization peak is as strong as the UV-EUV one. Electrons and protons are very important depending the precipitation conditions. Protons can create a layer at 500 km, while electrons tend to ionize near 800 km. The oxygen ion impact is near 900 km. The results shows few differences to precedent models for the nightside T5 fly-by of Cassini, and can highlight the sources of the different ion layers detected by radio measurements. Conclusions. The new model successfully computes the ion production in the atmosphere of Titan. For the first time, a full electron and ion profile has been computed from 0 to 1600 km, which compares qualitatively with measurements. This result can be used by chemical models.

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Section: The Transtitan Modelmentioning

confidence: 99%

Ionization processes in the atmosphere of Titan

Gronoff¹,

Lilensten²,

Desorgher

et al. 2009

A&A

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“…We see that for 13.4 eV photoexcitation, unity optical depth is reached at 137 km 359 for Venus and 131 km for Mars. Therefore, for the case of Mars, the CO triplet band4/5/12 emission generated by CO 2 photodissociation for 1/e absorption will lie only 11 km 361 higher than the 120 km Cameron band peak seen by SPICAM [Simon et al, 2009]. 362…”

Section: Altitude Of the Co Triplet Band Emission In Venus And Mars 340mentioning

confidence: 92%

“…The crux of the matter is that 13.4 eV photons are blocked by CO 2 at 344 relatively high altitudes. Above such altitudes, the Cameron and triplet bands will have 345 comparable intensities, but at the altitude where the Cameron band profile peaks, 346 typically near 120 km in the Mars dayglow [Simon et al, 2009], the unity optical depth 347…”

Section: Altitude Of the Co Triplet Band Emission In Venus And Mars 340mentioning

confidence: 99%

CO prompt emission as a CO2 marker in comets and planetary atmospheres

Kalogerakis

Romanescu

Ahmed

et al. 2012

Icarus

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“…In nightglow, chemistry and/or transport of dayside-excited species to the nightside may be involved in the observed emissions (Simon et al 2009). Auroral emissions constitute a very important feature in terrestrial space weather, and are an important part of planetary space weather as well.…”

Section: Airglow and Auroraementioning

confidence: 99%

What characterizes planetary space weather?

Lilensten

Coates

Déhant

et al. 2014

Astron Astrophys Rev

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Space weather has become a mature discipline for the Earth space environment. With increasing efforts in space exploration, it is becoming more and more necessary to understand the space environments of bodies other than Earth. This is the background for an emerging aspect of the space weather discipline: planetary space weather. In this article, we explore what characterizes planetary space weather, using some examples throughout the solar system. We consider energy sources and timescales, the characteristics of solar system objects and interaction processes. We

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Dayglow on Mars: Kinetic modelling with SPICAM UV limb data

Cited by 52 publications

References 103 publications

Ionization processes in the atmosphere of Titan

Ionization processes in the atmosphere of Titan

CO prompt emission as a CO2 marker in comets and planetary atmospheres

What characterizes planetary space weather?

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