Photochemistry of a Volcanically Driven Atmosphere on Io: Sulfur and Oxygen Species from a Pele-Type Eruption

Moses, J. I.; Zolotov, M. Yu.; Fegley, B.

doi:10.1006/icar.2001.6758

Cited by 100 publications

(77 citation statements)

References 144 publications

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“…Previous studies which used a larger radius of the planet required a thick water envelope (Demory et al 2011;Winn et al 2011) or a carbon-rich interior ), neither of which are now required but cannot be ruled out either. However, under the assumption of an Earth-like interior, which is also the case for Io, the outgassed products could comprise of gaseous CO2 and sulfur compounds (Moses et al 2002;Schaefer & Fegley 2005) along with particulate matter composed of silicates (Spencer et al 1997;McEwen et al 1998). The steady state composition of the atmosphere can be equally diverse (Miguel et al 2011;Hu & Seager 2014), although the stability of a thick ambient atmosphere is uncertain (Castan & Menou 2011;Heng & Kopparla 2012).…”

Section: Discussionmentioning

confidence: 99%

Variability in the super-Earth 55 Cnc e

Demory

Gillon

Madhusudhan

et al. 2015

Mon. Not. R. Astron. Soc.

158

147

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Considerable progress has been made in recent years in observations of atmospheric signatures of giant exoplanets, but processes in rocky exoplanets remain largely unknown due to major challenges in observing small planets. Numerous efforts to observe spectra of superEarths, exoplanets with masses of 1-10 Earth masses, have thus far revealed only featureless spectra. In this paper we report a 4-σ detection of variability in the dayside thermal emission from the transiting super-Earth 55 Cancri e. Dedicated space-based monitoring of the planet in the mid-infrared over eight eclipses revealed the thermal emission from its dayside atmosphere varying by a factor 3.7 between 2012 and 2013. The amplitude and trend of the variability are not explained by potential influence of star spots or by local thermal or compositional changes in the atmosphere over the short span of the observations. The possibility of large scale surface activity due to strong tidal interactions possibly similar to Io, or the presence of circumstellar/circumplanetary material appear plausible and motivate future long-term monitoring of the planet.

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Section: Discussionmentioning

confidence: 99%

Variability in the super-Earth 55 Cnc e

Demory

Gillon

Madhusudhan

et al. 2015

Mon. Not. R. Astron. Soc.

158

147

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“…The photochemistry of such a sublimation-driven SO 2 atmosphere on Io is relatively straightforward, with SO 2 , SO, O, S, and O 2 being the only important photochemical products (e.g., Kumar 1982, Wong and Johnson 1996a. However, to explain the presence of the photochemically reactive S 2 molecule or alkali and halogen species in Io's atmosphere, photochemical models must also consider sputtering of surface deposits or emission from active volcanoes (e.g., Kumar 1985, Wong and Smyth 2000, Moses et al 2002. Several recent observations indicate that active volcanoes might play a larger role in controlling atmospheric properties than was previously thought.…”

Section: Introductionmentioning

confidence: 99%

Alkali and Chlorine Photochemistry in a Volcanically Driven Atmosphere on Io

Moses

Zolotov

Fegley

2002

Icarus

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102

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“…Besides SO2, millimeter wavelength observations indicate also the presence of Na-, Cl-, and K-bearing volatiles (Schaefer & Fegley 2005). Other elements related to chondritic abundances such as Li, Br, Rb are negligible compared to the above mentioned species (Fegley & Zolotov 2000;Moses et al 2002;Schaefer & Fegley 2005).…”

Section: Io's Volcanic Activitymentioning

confidence: 99%

On the ultraviolet anomalies of the WASP-12 and HD 189733 systems: Trojan satellites as a plasma source

Kislyakova

Pilat-Lohinger

Funk

et al. 2016

Mon. Not. R. Astron. Soc.

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We suggest an additional possible plasma source to explain part of the phenomena observed for the transiting hot Jupiters WASP-12b and HD 189733b in their ultraviolet (UV) light curves. In the proposed scenario, material outgasses from the molten surface of Trojan satellites on tadpole orbits near the Lagrange points L 4 and L 5 . We show that the temperature at the orbital location of WASP-12b is high enough to melt the surface of rocky bodies and to form shallow lava oceans on them. In case of WASP12b, this leads to the release of elements such as Mg and Ca, which are expected to surround the system. The predicted Mg and Ca outgassing rates from two Io-sized WASP-12b Trojans are ≈ 2.2 × 10 27 s −1 and ≈ 2.2 × 10 26 s −1 , respectively. Trojan outgassing can lead to the apparent lack of emission in Mgii h&k and Caii H&K line cores of WASP-12. For HD 189733b, the mechanism is only marginally possible due to the lower temperature. This may be one of the reasons that couldn't explain the early ingress of HD 189733b observed in the far-UV (FUV) Cii doublet due to absence of carbon within elements outgassed by molten lava. We investigate the long-term stability region of WASP-12b and HD 189733b in case of planar and inclined motion of these satellites and show that unlike the classical exomoons orbiting the planet, Io-sized Trojans can be stable for the whole systems life time.

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Photochemistry of a Volcanically Driven Atmosphere on Io: Sulfur and Oxygen Species from a Pele-Type Eruption

Cited by 100 publications

References 144 publications

Variability in the super-Earth 55 Cnc e

Variability in the super-Earth 55 Cnc e

Alkali and Chlorine Photochemistry in a Volcanically Driven Atmosphere on Io

On the ultraviolet anomalies of the WASP-12 and HD 189733 systems: Trojan satellites as a plasma source

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