Haze evolution in temperate exoplanet atmospheres through surface energy measurements
Photochemical hazes are important opacity sources in temperate exoplanet atmospheres, hindering current observations from characterizing exoplanet atmospheric compositions. The haziness of an atmosphere is determined by the balance between haze production and removal. However, the material-dependent...
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Published in | Nature astronomy Vol. 5; no. 8; pp. 822 - 831 |
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Main Authors | , , , , , , , , , , , , , , , |
Format | Journal Article |
Language | English |
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Nature Publishing Group
01.08.2021
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Abstract | Photochemical hazes are important opacity sources in temperate exoplanet atmospheres, hindering current observations from characterizing exoplanet atmospheric compositions. The haziness of an atmosphere is determined by the balance between haze production and removal. However, the material-dependent removal physics of the haze particles are currently unknown under exoplanetary conditions. Here we provide experimentally measured surface energies for a grid of temperate exoplanet hazes to characterize haze removal in exoplanetary atmospheres. We found large variations of surface energies for hazes produced under different energy sources, atmospheric compositions and temperatures. The surface energies of the hazes were found to be the lowest around 400 K for the cold plasma samples, leading to the lowest removal rates. We show a suggestive correlation between haze surface energy and atmospheric haziness with planetary equilibrium temperature. We hypothesize that habitable-zone exoplanets could be less hazy, as they would possess high-surface-energy hazes that can be removed efficiently.Photochemical hazes in exoplanet atmospheres work as opacity barriers, hindering characterization of the atmospheres themselves. Here laboratory experiments quantify the haze surface energies that factor into the removal of hazes from atmospheres, which, when added to existing data on haze production, give a greater understanding of haze properties. |
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AbstractList | Photochemical hazes are important opacity sources in temperate exoplanet atmospheres, hindering current observations from characterizing exoplanet atmospheric compositions. The haziness of an atmosphere is determined by the balance between haze production and removal. However, the material-dependent removal physics of the haze particles are currently unknown under exoplanetary conditions. Here we provide experimentally measured surface energies for a grid of temperate exoplanet hazes to characterize haze removal in exoplanetary atmospheres. We found large variations of surface energies for hazes produced under different energy sources, atmospheric compositions and temperatures. The surface energies of the hazes were found to be the lowest around 400 K for the cold plasma samples, leading to the lowest removal rates. We show a suggestive correlation between haze surface energy and atmospheric haziness with planetary equilibrium temperature. We hypothesize that habitable-zone exoplanets could be less hazy, as they would possess high-surface-energy hazes that can be removed efficiently.Photochemical hazes in exoplanet atmospheres work as opacity barriers, hindering characterization of the atmospheres themselves. Here laboratory experiments quantify the haze surface energies that factor into the removal of hazes from atmospheres, which, when added to existing data on haze production, give a greater understanding of haze properties. Photochemical hazes are important opacity sources in temperate exoplanet atmospheres, hindering current observations from characterizing exoplanet atmospheric compositions. The haziness of an atmosphere is determined by the balance between haze production and removal. However, the material-dependent removal physics of the haze particles is currently unknown under exoplanetary conditions. Here we provide experimentally-measured surface energies for a grid of temperate exoplanet hazes to characterize haze removal in exoplanetary atmospheres. We found large variations of surface energies for hazes produced under different energy sources, atmospheric compositions, and temperatures. The surface energies of the hazes were found to be the lowest around 400 K for the cold plasma samples, leading to the lowest removal rates. We show a suggestive correlation between haze surface energy and atmospheric haziness with planetary equilibrium temperature. We hypothesize that habitable zone exoplanets could be less hazy, as they would possess high-surface-energy hazes which can be removed efficiently. |
Author | He, Chao Morley, Caroline V. Valenti, Jeff A. Dymont, Austin H. Moses, Julianne I. Yu, Xinting Zhang, Xi McGuiggan, Patricia Gao, Peter Powell, Diana Lewis, Nikole K. Hörst, Sarah M. Kempton, Eliza M.-R. Vuitton, Véronique Fortney, Jonathan J. Moran, Sarah E. |
Author_xml | – sequence: 1 givenname: Xinting orcidid: 0000-0002-7479-1437 surname: Yu fullname: Yu, Xinting – sequence: 2 givenname: Chao orcidid: 0000-0002-6694-0965 surname: He fullname: He, Chao – sequence: 3 givenname: Xi surname: Zhang fullname: Zhang, Xi – sequence: 4 givenname: Sarah M. orcidid: 0000-0003-4596-0702 surname: Hörst fullname: Hörst, Sarah M. – sequence: 5 givenname: Austin H. surname: Dymont fullname: Dymont, Austin H. – sequence: 6 givenname: Patricia surname: McGuiggan fullname: McGuiggan, Patricia – sequence: 7 givenname: Julianne I. orcidid: 0000-0002-8837-0035 surname: Moses fullname: Moses, Julianne I. – sequence: 8 givenname: Nikole K. surname: Lewis fullname: Lewis, Nikole K. – sequence: 9 givenname: Jonathan J. surname: Fortney fullname: Fortney, Jonathan J. – sequence: 10 givenname: Peter surname: Gao fullname: Gao, Peter – sequence: 11 givenname: Eliza M.-R. orcidid: 0000-0002-1337-9051 surname: Kempton fullname: Kempton, Eliza M.-R. – sequence: 12 givenname: Sarah E. orcidid: 0000-0002-6721-3284 surname: Moran fullname: Moran, Sarah E. – sequence: 13 givenname: Caroline V. surname: Morley fullname: Morley, Caroline V. – sequence: 14 givenname: Diana orcidid: 0000-0002-4250-0957 surname: Powell fullname: Powell, Diana – sequence: 15 givenname: Jeff A. surname: Valenti fullname: Valenti, Jeff A. – sequence: 16 givenname: Véronique orcidid: 0000-0001-7273-1898 surname: Vuitton fullname: Vuitton, Véronique |
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Snippet | Photochemical hazes are important opacity sources in temperate exoplanet atmospheres, hindering current observations from characterizing exoplanet atmospheric... |
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SubjectTerms | Astronomy Astrophysics Atmosphere Atmospheric aerosols Cold Contact angle Earth Earth and Planetary Astrophysics Energy resources Energy sources Equilibrium Haze Laboratories Opacity Photochemicals Physics Plasma Science Sciences of the Universe |
Title | Haze evolution in temperate exoplanet atmospheres through surface energy measurements |
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