XUV-driven mass loss from extrasolar giant planets orbiting active stars
•XUV spectra for eps Eri, AD Leo and AU Mic are constructed using a coronal model.•Density and temperature profiles are derived for EGPs around active stars.•We derive an improved scaling method for the solar XUV spectrum to match the stellar.•EGPs around more active stars have stability limit at la...
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| Vydáno v: | Icarus (New York, N.Y. 1962) Ročník 250; s. 357 - 367 |
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01.04.2015
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| ISSN: | 0019-1035, 1090-2643 |
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| Abstract | •XUV spectra for eps Eri, AD Leo and AU Mic are constructed using a coronal model.•Density and temperature profiles are derived for EGPs around active stars.•We derive an improved scaling method for the solar XUV spectrum to match the stellar.•EGPs around more active stars have stability limit at larger orbital distances.
Upper atmospheres of Hot Jupiters are subject to extreme radiation conditions that can result in rapid atmospheric escape. The composition and structure of the upper atmospheres of these planets are affected by the high-energy spectrum of the host star. This emission depends on stellar type and age, which are thus important factors in understanding the behaviour of exoplanetary atmospheres. In this study, we focus on Extrasolar Giant Planets (EPGs) orbiting K and M dwarf stars. XUV spectra for three different stars – ∊ Eridani, AD Leonis and AU Microscopii – are constructed using a coronal model. Neutral density and temperature profiles in the upper atmosphere of hypothetical EGPs orbiting these stars are then obtained from a fluid model, incorporating atmospheric chemistry and taking atmospheric escape into account. We find that a simple scaling based solely on the host star’s X-ray emission gives large errors in mass loss rates from planetary atmospheres and so we have derived a new method to scale the EUV regions of the solar spectrum based upon stellar X-ray emission. This new method produces an outcome in terms of the planet’s neutral upper atmosphere very similar to that obtained using a detailed coronal model of the host star. Our results indicate that in planets subjected to radiation from active stars, the transition from Jeans escape to a regime of hydrodynamic escape at the top of the atmosphere occurs at larger orbital distances than for planets around low activity stars (such as the Sun). |
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| AbstractList | Upper atmospheres of Hot Jupiters are subject to extreme radiation conditions that can result in rapid atmospheric escape. The composition and structure of the upper atmospheres of these planets are affected by the high-energy spectrum of the host star. This emission depends on stellar type and age, which are thus important factors in understanding the behaviour of exoplanetary atmospheres. In this study, we focus on Extrasolar Giant Planets (EPGs) orbiting K and M dwarf stars. XUV spectra for three different stars - Eridani, AD Leonis and AU Microscopii - are constructed using a coronal model. Neutral density and temperature profiles in the upper atmosphere of hypothetical EGPs orbiting these stars are then obtained from a fluid model, incorporating atmospheric chemistry and taking atmospheric escape into account. We find that a simple scaling based solely on the host star's X-ray emission gives large errors in mass loss rates from planetary atmospheres and so we have derived a new method to scale the EUV regions of the solar spectrum based upon stellar X-ray emission. This new method produces an outcome in terms of the planet's neutral upper atmosphere very similar to that obtained using a detailed coronal model of the host star. Our results indicate that in planets subjected to radiation from active stars, the transition from Jeans escape to a regime of hydrodynamic escape at the top of the atmosphere occurs at larger orbital distances than for planets around low activity stars (such as the Sun). •XUV spectra for eps Eri, AD Leo and AU Mic are constructed using a coronal model.•Density and temperature profiles are derived for EGPs around active stars.•We derive an improved scaling method for the solar XUV spectrum to match the stellar.•EGPs around more active stars have stability limit at larger orbital distances. Upper atmospheres of Hot Jupiters are subject to extreme radiation conditions that can result in rapid atmospheric escape. The composition and structure of the upper atmospheres of these planets are affected by the high-energy spectrum of the host star. This emission depends on stellar type and age, which are thus important factors in understanding the behaviour of exoplanetary atmospheres. In this study, we focus on Extrasolar Giant Planets (EPGs) orbiting K and M dwarf stars. XUV spectra for three different stars – ∊ Eridani, AD Leonis and AU Microscopii – are constructed using a coronal model. Neutral density and temperature profiles in the upper atmosphere of hypothetical EGPs orbiting these stars are then obtained from a fluid model, incorporating atmospheric chemistry and taking atmospheric escape into account. We find that a simple scaling based solely on the host star’s X-ray emission gives large errors in mass loss rates from planetary atmospheres and so we have derived a new method to scale the EUV regions of the solar spectrum based upon stellar X-ray emission. This new method produces an outcome in terms of the planet’s neutral upper atmosphere very similar to that obtained using a detailed coronal model of the host star. Our results indicate that in planets subjected to radiation from active stars, the transition from Jeans escape to a regime of hydrodynamic escape at the top of the atmosphere occurs at larger orbital distances than for planets around low activity stars (such as the Sun). |
| Author | Galand, M. Sanz-Forcada, J. Unruh, Y.C. Koskinen, T.T. Chadney, J.M. |
| Author_xml | – sequence: 1 givenname: J.M. surname: Chadney fullname: Chadney, J.M. email: joshua.chadney10@imperial.ac.uk organization: Department of Physics, Imperial College London, Prince Consort Road, London SW7 2BW, UK – sequence: 2 givenname: M. surname: Galand fullname: Galand, M. organization: Department of Physics, Imperial College London, Prince Consort Road, London SW7 2BW, UK – sequence: 3 givenname: Y.C. surname: Unruh fullname: Unruh, Y.C. organization: Department of Physics, Imperial College London, Prince Consort Road, London SW7 2BW, UK – sequence: 4 givenname: T.T. surname: Koskinen fullname: Koskinen, T.T. organization: Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA – sequence: 5 givenname: J. surname: Sanz-Forcada fullname: Sanz-Forcada, J. organization: Centro de Astrobiología (CSIC-INTA), ESAC Campus, P.O. Box 78, E-28691 Villanueva de la Cañada, Madrid, Spain |
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| Snippet | •XUV spectra for eps Eri, AD Leo and AU Mic are constructed using a coronal model.•Density and temperature profiles are derived for EGPs around active... Upper atmospheres of Hot Jupiters are subject to extreme radiation conditions that can result in rapid atmospheric escape. The composition and structure of the... |
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| SubjectTerms | Aeronomy Atmospherics Emission Extra-solar planets Extrasolar Extrasolar planets Fluid flow Photochemistry Solar radiation Stars Stellar atmospheres Upper atmosphere |
| Title | XUV-driven mass loss from extrasolar giant planets orbiting active stars |
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