High-resolution 3-μm spectra of Jupiter: Latitudinal spectral variations influenced by molecules, clouds, and haze

Kim, Sang J.; Geballe, T. R.; Kim, J.H.; Jung, Ah Ra; Seo, Hye Sook; Minh, Y. C.

doi:10.1016/j.icarus.2010.03.024

Cited by 10 publications

(4 citation statements)

References 48 publications

(106 reference statements)

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“…Comparisons between our results and a representative set of observations for the depthdependent mixing ratios, for the species CH 4 , C 2 H 2 , C 2 H 4 , C 2 H 6 ,and C 4 H 2 , are shown in Figure 12. The observations for CH 4 are taken from Drossart et al (1999) and Yelle et al (1996), C 2 H 2 observations are from Fouchet et al (2000), Moses et al (2005), and Kim et al (2010), C 2 H 4 observations are from Romani et al (2008) and Moses et al (2005), C 2 H 6 observations are from Fouchet et al 2000, Moses et al (2005), Yelle et al (2001) and Kim et al (2010), and the C 4 H 2 observations are from Fouchet et al (2000) and Moses et al (2005). We also incorporate observations for C 2 H 2 , C 2 H 4 ,and C 2 H 6 from Gladstone et al (1996) and references therein.…”

Section: Jupitermentioning

confidence: 99%

A Chemical Kinetics Network for Lightning and Life in Planetary Atmospheres

Rimmer

Helling

2016

ApJS

127

154

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There are many open questions about prebiotic chemistry in both planetary and exoplanetary environments. The increasing number of known exoplanets and other ultra-cool, substellar objects has propelled the desire to detect life andprebiotic chemistry outside the solar system. We present an ion-neutral chemical network constructed from scratch, STAND2015, that treats hydrogen, nitrogen, carbon, and oxygen chemistry accurately within a temperature range between 100 and 30,000 K. Formation pathways for glycine and other organic molecules are included. The network is complete up to H6C2N2O3. STAND2015 is successfully tested against atmospheric chemistry models for HD 209458b, Jupiter, and the present-day Earth using a simple one-dimensionalphotochemistry/diffusion code. Our results for the early Earth agree with those of Kasting for CO 2 , H 2 , CO, and O 2 , but do not agree for water and atomic oxygen. We use the network to simulate an experiment where varied chemical initial conditions are irradiated by UV light. The result from our simulation is that more glycine is produced when more ammonia and methane is present. Very little glycine is produced in the absence of any molecular nitrogen and oxygen. This suggests that theproduction of glycine is inhibited if a gas is too strongly reducing. Possible applications and limitations of the chemical kinetics network are also discussed.

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Section: Jupitermentioning

confidence: 99%

A Chemical Kinetics Network for Lightning and Life in Planetary Atmospheres

Rimmer

Helling

2016

ApJS

127

154

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“…The absolute intensities presented in Figure 1abcd were obtained from the observed fluxes of the standard stars as well as by cross-checking the previous absolute calibrations of the 3.3-m continuum levels of the non-auroral regions observed by UKIRT/CGS4 (Kim et al 2010), ISO (Kim et al 2014), and Gemini North/GNIRS (Kim et al 2015). A discussion of the uncertainties in the intensities is given below.…”

Section: ) Observations and Data Reductionmentioning

confidence: 99%

Temporal variation of the 3-micron hydrocarbon emissions at the 8-micron north polar hot spot of Jupiter: Comparison with solar wind activity

Kim

Sim

Geballe

et al. 2020

Icarus

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“…We derive temperatures from the rotational lines of the CH 4 bands using the following considerations. Radiative transfer programs that simulate the fluorescent emission of the 3-lm bands of CH 4 have been developed for analysis of jovian spectra (Drossart et al, 1999;Kim et al, 2009Kim et al, , 2010Kim et al, , 2014. For the CH 4 molecular line list, we adopt the HITRAN2012 database (Rothman et al, 2009).…”

Section: Observations and Data Reductionmentioning

confidence: 99%