The role of photochemical processes in evolution of the isotopic composition of the atmosphere of Titan

Berezhnoi, A. A.

doi:10.1134/s0038094610060031

Cited by 8 publications

(4 citation statements)

References 30 publications

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“…Figure 10 places the measurements of Titan's H, C, N, and O isotopes into solar system context. Conversion of NH 3 to N 2 by photolysis [Atreya et al, 1978], shock chemistry [McKay et al, 1988], and thermal decomposition in the interior [Glein et al, 2009] do not significantly alter the 14 N/ 15 N ratio [Berezhnoi, 2010]. Sekine et al [2011] also suggested that impacts into ammonium hydrate in the crust could convert NH 3 into N 2 ; however, Marounina et al [2015] showed that impact erosion of Titan's atmosphere would be very efficient.…”

Section: The Age and Origin Of Titan's Atmospherementioning

confidence: 99%

Titan's atmosphere and climate

2017

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Titan is the only moon with a substantial atmosphere, the only other thick N2 atmosphere besides Earth's, the site of extraordinarily complex atmospheric chemistry that far surpasses any other solar system atmosphere, and the only other solar system body with stable liquid currently on its surface. The connection between Titan's surface and atmosphere is also unique in our solar system; atmospheric chemistry produces materials that are deposited on the surface and subsequently altered by surface‐atmosphere interactions such as aeolian and fluvial processes resulting in the formation of extensive dune fields and expansive lakes and seas. Titan's atmosphere is favorable for organic haze formation, which combined with the presence of some oxygen‐bearing molecules indicates that Titan's atmosphere may produce molecules of prebiotic interest. The combination of organics and liquid, in the form of water in a subsurface ocean and methane/ethane in the surface lakes and seas, means that Titan may be the ideal place in the solar system to test ideas about habitability, prebiotic chemistry, and the ubiquity and diversity of life in the universe. The Cassini‐Huygens mission to the Saturn system has provided a wealth of new information allowing for study of Titan as a complex system. Here I review our current understanding of Titan's atmosphere and climate forged from the powerful combination of Earth‐based observations, remote sensing and in situ spacecraft measurements, laboratory experiments, and models. I conclude with some of our remaining unanswered questions as the incredible era of exploration with Cassini‐Huygens comes to an end.

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Section: The Age and Origin Of Titan's Atmospherementioning

confidence: 99%

Titan's atmosphere and climate

2017

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“…Soon after Titan's formation, the conversion of ammonia into nitrogen may have been induced by photolysis (Atreya et al 1978) or shock chemistry (McKay et al 1988) in the satellite's atmosphere, or resulted from its thermal decomposition in the interior (Glein et al 2009). It has already been shown that none of these conversion processes could have significantly changed the 14 N/ 15 N ratio (Berezhnoi 2010).…”

Section: Introductionmentioning

confidence: 99%

“…We first explore whether it is possible for Titan's primordial ratio to fractionate from 272 to its current value of 167.7 and then discuss the implications for the origin of Titan's nitrogen. It has already been demonstrated that the conversion of NH 3 into N 2 by photolysis (Atreya et al 1978) or shock chemistry (McKay et al 1988) could not have significantly changed the 14 N/ 15 N ratio (Berezhnoi 2010) nor could thermal decomposition in the interior (Glein et al 2009). However, these studies did not consider escape, which is one of the most efficient mechanisms known to substantially fractionate the planetary atmospheres (Pepin 2006).…”

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confidence: 99%

PROTOSOLAR AMMONIA AS THE UNIQUE SOURCE OF TITAN's NITROGEN

Mandt

Mousis

Lunine

et al. 2014

ApJ

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The origin of Titan's nitrogen-rich atmosphere is thought to be ammonia ice, but this has not yet been confirmed. Furthermore, it is uncertain whether the building blocks of Titan formed within the Saturnian subnebula or in the colder protosolar nebula (PSN). Recent measurements of the nitrogen isotope ratio in cometary ammonia, combined with evolutionary constraints on the nitrogen isotopes in Titan's atmosphere provide firm evidence that the nitrogen in Titan's atmosphere must have originated as ammonia ice formed in the PSN under conditions similar to that of cometary formation. This result has important implications for the projected D/H ratio in cometary methane, nitrogen isotopic fractionation in the PSN and the source of nitrogen for Earth's atmosphere.

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“…and thermal decomposition in the interior do not significantly alter the 14 N/ 15 N ratio [Berezhnoi , 2010]. Sekine et al [2011] also suggested that impacts into ammonium hydrate in the crust could convert NH 3 into N 2 ; however, Marounina et al [2015] showed that impact erosion of Titan's atmosphere would be very efficient.…”

Section: Cryovolcanismmentioning

confidence: 99%

Titan's Atmosphere and Climate

Hörst

2017

Preprint

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Titan is the only moon with a substantial atmosphere, the only other thick N 2 atmosphere besides Earth's, the site of extraordinarily complex atmospheric chemistry that far surpasses any other solar system atmosphere, and the only other solar system body with stable liquid currently on its surface. The connection between Titan's surface and atmosphere is also unique in our Solar system; atmospheric chemistry produces materials that are deposited on the surface and subsequently altered by surface-atmosphere interactions such as aeolian and fluvial processes resulting in the formation of extensive dune fields and expansive lakes and seas. Titan's atmosphere is favorable for organic haze formation, which combined with the presence of some oxygen bearing molecules indicates that Titan's atmosphere may produce molecules of prebiotic interest. The combination of organics and liquid, in the form of water in a subsurface ocean and methane/ethane in the surface lakes and seas, means that Titan may be the ideal place in the solar system to test ideas about habitability, prebiotic chemistry, and the ubiquity and diversity of life in the Universe. The Cassini-Huygens mission to the Saturn system has provided a wealth of new information allowing for study of Titan as a complex system. Here I review our current understanding of Titan's atmosphere and climate forgedThe thermal structure of the upper atmosphere is more variable and complex than expected and there are still a number of outstanding questions regarding its variability.On average the night side is warmer than the day side [

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The role of photochemical processes in evolution of the isotopic composition of the atmosphere of Titan

Cited by 8 publications

References 30 publications

Titan's atmosphere and climate

Titan's atmosphere and climate

PROTOSOLAR AMMONIA AS THE UNIQUE SOURCE OF TITAN's NITROGEN

Titan's Atmosphere and Climate

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