Proxima Centauri b: A Strong Case for including Cosmic-Ray-induced Chemistry in Atmospheric Biosignature Studies

Due to its Earth-like minimum mass of 1.27 M\(_{\text{E}}\) and its close proximity to our Solar system, Proxima Centauri b is one of the most interesting exoplanets for habitability studies. Its host star, Proxima Centauri, is however a strongly flaring star, which is expected to provide a very hos...

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Bibliographic Details
Published in:arXiv.org 2020-03
Main Authors: Scheucher, M, Herbst, K, Schmidt, V, Grenfell, J L, Schreier, F, Banjac, S, Heber, B, Rauer, H, Sinnhuber, M
Format: Article
Language:English
Subjects:
Atmosphere
Bombardment
Cosmic rays
Earth
Energy spectra
Extrasolar planets
Habitability
Ionosphere
Magnetospheres
Planetary atmospheres
Red dwarf stars
Solar system
Stellar flares
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Summary:Due to its Earth-like minimum mass of 1.27 M\(_{\text{E}}\) and its close proximity to our Solar system, Proxima Centauri b is one of the most interesting exoplanets for habitability studies. Its host star, Proxima Centauri, is however a strongly flaring star, which is expected to provide a very hostile environment for potentially habitable planets. We perform a habitability study of Proxima Centauri b assuming an Earth-like atmosphere under high stellar particle bombardment, with a focus on spectral transmission features. We employ our extensive model suite calculating energy spectra of stellar particles, their journey through the planetary magnetosphere, ionosphere, and atmosphere, ultimately providing planetary climate and spectral characteristics, as outlined in Herbst et al. (2019). Our results suggest that together with the incident stellar energy flux, high particle influxes can lead to efficient heating of the planet well into temperate climates, by limiting CH\(_4\) amounts, which would otherwise run into anti-greenhouse for such planets around M-stars. We identify some key spectral features relevant for future spectral observations: First, NO\(_2\) becomes the major absorber in the visible, which greatly impacts the Rayleigh slope. Second, H\(_2\)O features can be masked by CH\(_4\) (near infra-red) and CO\(_2\) (mid to far infra-red), making them non-detectable in transmission. Third, O\(_3\) is destroyed and instead HNO\(_3\) features become clearly visible in the mid to far infra-red. Lastly, assuming a few percent of CO\(_2\) in the atmosphere, CO\(_2\) absorption at 5.3 \(\mu\)m becomes significant (for flare and non-flare cases), strongly overlapping with a flare related NO feature in Earth's atmosphere.
ISSN:2331-8422
DOI:10.48550/arxiv.2003.02036