ExoMol molecular line lists – XX. A comprehensive line list for H3+

Mizus, Irina I.; Alijah, Alexander; Zobov, Nikolai F.; Lodi, Lorenzo; Kyuberis, Aleksandra A.; Yurchenko, Sergei N.; Tennyson, Jonathan; Polyansky, Oleg L.

doi:10.1093/mnras/stx502

Cited by 44 publications

(37 citation statements)

References 114 publications

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“…For robust identification, absorption cross-sections valid for the extreme temperatures of these sub-stellar objects are needed. The ExoMol team already provides the needed H3 + line-lists (Mizus et al 2017), but updated line-lists for H3O + will be needed if this molecule is to be positively identified in a brown dwarf atmosphere.…”

Section: Resultsmentioning

confidence: 99%

Lightning and charge processes in brown dwarf and exoplanet atmospheres

Helling

Rimmer

2019

Phil. Trans. R. Soc. A.

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The study of the composition of brown dwarf atmospheres helped to understand their formation and evolution. Similarly, the study of exoplanet atmospheres is expected to constrain their formation and evolutionary states. We use results from three-dimensional simulations, kinetic cloud formation and kinetic ion-neutral chemistry to investigate ionization processes that will affect their atmosphere chemistry: the dayside of super-hot Jupiters is dominated by atomic hydrogen, and not H 2 O. Such planetary atmospheres exhibit a substantial degree of thermal ionization and clouds only form on the nightside where lightning leaves chemical tracers (e.g. HCN) for possibly long enough to be detectable. External radiation may cause exoplanets to be enshrouded in a shell of highly ionized, H 3 + -forming gas and a weather-driven aurora may emerge. Brown dwarfs enable us to study the role of electron beams for the emergence of an extrasolar, weather system-driven aurora-like chemistry, and the effect of strong magnetic fields on cold atmospheric gases. Electron beams trigger the formation of H 3 + in the upper atmosphere of a brown dwarf (e.g. LSR-J1835), which may react with it to form hydronium, H 3 O + , as a longer lived chemical tracer. Brown dwarfs and super-hot gas giants may be excellent candidates to search for H 3 O + as an H 3 + product. This article is part of a discussion meeting issue ‘Advances in hydrogen molecular ions: H 3 + , H 5 + and beyond’.

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Section: Resultsmentioning

confidence: 99%

Lightning and charge processes in brown dwarf and exoplanet atmospheres

Helling

Rimmer

2019

Phil. Trans. R. Soc. A.

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“…1 computed from the 10to10 line list for CH 4 . Examples of ExoMol lifetimes and cooling functions can be found in Tennyson et al (2016a); Melnikov et al (2016) and Mizus et al (2017).…”

Section: Radiative Lifetimementioning

confidence: 99%

EXOCROSS: a general program for generating spectra from molecular line lists

Yurchenko

Al-Refaie

Tennyson

2018

A&A

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187

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ExoCross is a Fortran code for generating spectra (emission, absorption) and thermodynamic properties (partition function, specific heat etc.) from molecular line lists. Input is taken in several formats, including ExoMol and HITRAN formats. ExoCross is efficiently parallelized showing also a high degree of vectorization. It can work with several line profiles such as Doppler, Lorentzian and Voigt and support several broadening schemes. Voigt profiles are handled by several methods allowing fast and accurate simulations. Two of these methods are new. ExoCross is also capable of working with the recently proposed method of super-lines. It supports calculations of lifetimes, cooling functions, specific heats and other properties. ExoCross can be used to convert between different formats, such as HITRAN, ExoMol and Phoenix. It is capable of simulating non-LTE spectra using a simple two-temperature approach. Different electronic, vibronic or vibrational bands can be simulated separately using an efficient filtering scheme based on the quantum numbers.

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“…Thus, for example, both the TheoReTS and ExoMol groups pointed out that the 2012 edition of the HITRAN database [104] contained a spurious feature due to methane near 11 µm [105,106], which led to its removal in the 2016 release of HITRAN [107]. procedure is well established [10] in that for all but a small number of systems with very few electrons [109,110,111], the PES used is spectroscopically determined. That is, an initial high-accuracy ab initio PES is systematically adjusted until it reproduces observed spectra as accurately as possible.…”

Section: Dipole Momentsmentioning

confidence: 99%

Laboratory spectra of hot molecules: Data needs for hot super-Earth exoplanets

Tennyson

Yurchenko

2017

Molecular Astrophysics

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The majority of stars are now thought to support exoplanets. Many of those exoplanets discovered thus far are categorized as rocky objects with an atmosphere. Most of these objects are however hot due to their short orbital period. Models suggest that water is the dominant species in their atmospheres. The hot temperatures are expected to turn these atmospheres into a (high pressure) steam bath containing remains of melted rock. The spectroscopy of these hot rocky objects will be very different from that of cooler objects or hot gas giants. Molecules suggested to be important for the spectroscopy of these objects are reviewed together with the current status of the corresponding spectroscopic data. Perspectives of building a comprehensive database of linelist/cross sections applicable for atmospheric models of rocky super-Earths as part of the ExoMol project are discussed.The quantum-mechanical approaches used in linelist productions and their challenges are summarized. ), key hot exoplanets with masses and radii in the rocky-planet range includeCoRoT-7b, Kepler-10b, Kepler-78b, Kepler-97b, Kepler-99b, Kepler-102b, Kepler-93b being slightly cooler than 1673 K [21,22,30,31,32,33,34,35,36] Most of the rocky exoplanets that have so far been studied are characterized by the high temperature of their atmospheres, e.g., about 1500 K in Kepler-36b and Kepler-93b, 2474 ± 71 K in CoRoT-7b [37], 2360 ± 300 K in 55 Cnc

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ExoMol molecular line lists – XX. A comprehensive line list for H3+

Cited by 44 publications

References 114 publications

Lightning and charge processes in brown dwarf and exoplanet atmospheres

Lightning and charge processes in brown dwarf and exoplanet atmospheres

EXOCROSS: a general program for generating spectra from molecular line lists

Laboratory spectra of hot molecules: Data needs for hot super-Earth exoplanets

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