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dc.contributor.authorDomagal-Goldman, S.D.
dc.contributor.authorSegura, A.
dc.contributor.authorClaire, M.W.
dc.contributor.authorRobinson, T.D.
dc.contributor.authorMeadows, V.S.
dc.date.accessioned2014-09-12T10:31:01Z
dc.date.available2014-09-12T10:31:01Z
dc.date.issued2014-09-10
dc.identifier.citationDomagal-Goldman , S D , Segura , A , Claire , M W , Robinson , T D & Meadows , V S 2014 , ' Abiotic ozone and oxygen in atmospheres similar to prebiotic earth ' , Astrophysical Journal , vol. 792 , no. 2 , 90 . https://doi.org/10.1088/0004-637X/792/2/90en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 147758008
dc.identifier.otherPURE UUID: 9aaa257f-efb7-4953-a855-a62bfbbb03f6
dc.identifier.otherScopus: 84906751369
dc.identifier.otherORCID: /0000-0001-9518-089X/work/34103243
dc.identifier.otherWOS: 000341172200008
dc.identifier.urihttp://hdl.handle.net/10023/5410
dc.description.abstractThe search for life on planets outside our solar system will use spectroscopic identification of atmospheric biosignatures. The most robust remotely detectable potential biosignature is considered to be the detection of oxygen (O2) or ozone (O3) simultaneous to methane (CH4) at levels indicating fluxes from the planetary surface in excess of those that could be produced abiotically. Here we use an altitude-dependent photochemical model with the enhanced lower boundary conditions necessary to carefully explore abiotic O2 and O3 production on lifeless planets with a wide variety of volcanic gas fluxes and stellar energy distributions. On some of these worlds, we predict limited O2 and O3 buildup, caused by fast chemical production of these gases. This results in detectable abiotic O3 and CH4 features in the UV-visible, but no detectable abiotic O2 features. Thus, simultaneous detection of O3 and CH4 by a UV-visible mission is not a strong biosignature without proper contextual information. Discrimination between biological and abiotic sources of O2 and O3 is possible through analysis of the stellar and atmospheric context—particularly redox state and O atom inventory—of the planet in question. Specifically, understanding the spectral characteristics of the star and obtaining a broad wavelength range for planetary spectra should allow more robust identification of false positives for life. This highlights the importance of wide spectral coverage for future exoplanet characterization missions. Specifically, discrimination between true and false positives may require spectral observations that extend into infrared wavelengths and provide contextual information on the planet's atmospheric chemistry.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectEarthen
dc.subjectPlanets and satellites: atmospheresen
dc.subjectPlanets and satellites: terrestrial planetsen
dc.subjectPlanet-star interactionsen
dc.subjectUltraviolet: planetary systemsen
dc.subjectInfrared: planetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleAbiotic ozone and oxygen in atmospheres similar to prebiotic earthen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Earth and Environmental Sciencesen
dc.contributor.institutionUniversity of St Andrews.St Andrews Isotope Geochemistryen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/792/2/90
dc.description.statusPeer revieweden


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