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dc.contributor.authorRugheimer, S.
dc.contributor.authorKaltenegger, L.
dc.contributor.authorSegura, A.
dc.contributor.authorLinsky, J.
dc.contributor.authorMohanty, S.
dc.date.accessioned2016-10-04T11:30:17Z
dc.date.available2016-10-04T11:30:17Z
dc.date.issued2015-08-10
dc.identifier.citationRugheimer , S , Kaltenegger , L , Segura , A , Linsky , J & Mohanty , S 2015 , ' Effect of UV radiation on the spectral fingerprints of Earth-like planets orbiting M stars ' , Astrophysical Journal , vol. 809 , no. 1 . https://doi.org/10.1088/0004-637X/809/1/57en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 246493034
dc.identifier.otherPURE UUID: ad3c3c4b-1f63-4901-80d2-29fc8f2dc03a
dc.identifier.otherScopus: 84945315052
dc.identifier.otherORCID: /0000-0003-1620-7658/work/27164116
dc.identifier.urihttp://hdl.handle.net/10023/9604
dc.descriptionThe authors acknowledge support from DFG funding ENP KA 3142/1-1 and the Simons Foundation (290357, Kaltenegger).en
dc.description.abstractWe model the atmospheres and spectra of Earth-like planets orbiting the entire grid of M dwarfs for active and inactive stellar models with Teff = 2300 K to Teff = 3800 K and for six observed MUSCLES M dwarfs with UV radiation data. We set the Earth-like planets at the 1 AU equivalent distance and show spectra from the visible to IR (0.4-20 μm) to compare detectability of features in different wavelength ranges with the James Webb Space Telescope and other future ground- and spaced-based missions to characterize exo-Earths. We focus on the effect of UV activity levels on detectable atmospheric features that indicate habitability on Earth, namely, H2O, O3, CH4, N2O, and CH3Cl. To observe signatures of life - O2/O3 in combination with reducing species like CH4 - we find that early and active M dwarfs are the best targets of the M star grid for future telescopes. The O2 spectral feature at 0.76 μm is increasingly difficult to detect in reflected light of later M dwarfs owing to low stellar flux in that wavelength region. N2O, another biosignature detectable in the IR, builds up to observable concentrations in our planetary models around M dwarfs with low UV flux. CH3Cl could become detectable, depending on the depth of the overlapping N2O feature. We present a spectral database of Earth-like planets around cool stars for directly imaged planets as a framework for interpreting future light curves, direct imaging, and secondary eclipse measurements of the atmospheres of terrestrial planets in the habitable zone to design and assess future telescope capabilities.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/0004-637X/809/1/57en
dc.subjectAstrobiologyen
dc.subjectPlanets and satellites: atmospheresen
dc.subjectPlanets and satellites: terrestrial planetsen
dc.subjectStars: low-massen
dc.subjectQB Astronomyen
dc.subjectNuclear and High Energy Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.titleEffect of UV radiation on the spectral fingerprints of Earth-like planets orbiting M starsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Earth and Environmental Sciencesen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/809/1/57
dc.description.statusPeer revieweden


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