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- W590400145 abstract "The photolysis Photolysis of hydrogen-rich atmosphere of a close-in exoplanet by the extreme ultraviolet radiation of the parent star leads to the formation of the suprathermal particles (i.e., particles with an excess of kinetic energy), primary photoelectrons in the $$H_{2}/H/mathit{He}$$ ionization and hydrogen atoms in the H 2 dissociation Photo dissociation and dissociative ionization processes. These particles with excess kinetic energies are an important source of thermal energy in the upper atmosphere of the hydrogen-rich exoplanets. In the contemporary aeronomical models the kinetics and transfer of hot hydrogen atoms and fresh photoelectrons were not calculated in detail, because they require solving of the Boltzmann equation for a non-thermal population of these particles. This chapter estimates the effect of the XUV XUV radiation of the parent star on the production of the suprathermals Suprathermal atoms in the $$H_{2} rightarrow H$$ transition region in the upper atmosphere of a hydrogen-rich exoplanet. Partial deposition rates of the stellar XUV radiation due to the photolytic processes in the $$H_{2} rightarrow H$$ transition region in the upper atmosphere of HD 209458b HD 209458b were calculated. The Monte Carlo model developed by authors was used to calculate the collisional kinetics Collisional kinetics and the transport of photoelectrons in the atmosphere of HD209458b. Using this model the partial deposition rates of the stellar XUV radiation due to the electron impact processes in the $$H_{2} rightarrow H$$ transition region in the upper atmosphere of HD209458b were calculated. This allowed us to estimate the heating rate of the atmospheric gas by photoelectrons in the upper atmosphere of exoplanet. For the first time the heating efficiency η with and without taking into account the photoelectron impact Photoelectrons processes in the $$H_{2} rightarrow H$$ transition region in the hydrogen-rich atmosphere of exoplanet was calculated. Using the numerical stochastic model for a hot planetary corona the kinetics and transfer of suprathermal hydrogen Suprathermal atoms atoms in the upper atmosphere and the emergent flux of atoms evaporating from the atmosphere were investigated. The latter is estimated as $$5.8 times 10^{12},text{cm}^{-2}text{s}^{-1}$$ for a moderate stellar activity level of UV radiation, which leads to a planetary atmosphere evaporation rate of 5. 8 × 109 g/s due to the process of the dissociation of H 2. This estimate shows that suprathermal hydrogen atoms provide a significant contribution to the observational estimate of ∼ 1010 g/s for the atmospheric loss rate of HD 209458b." @default.
- W590400145 created "2016-06-24" @default.
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- W590400145 creator A5077772537 @default.
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- W590400145 date "2014-09-18" @default.
- W590400145 modified "2023-09-25" @default.
- W590400145 title "Suprathermal Particles in XUV-Heated and Extended Exoplanetary Upper Atmospheres" @default.
- W590400145 cites W1965833171 @default.
- W590400145 cites W1969601830 @default.
- W590400145 cites W1972890490 @default.
- W590400145 cites W1974579699 @default.
- W590400145 cites W1976802583 @default.
- W590400145 cites W1977126129 @default.
- W590400145 cites W1979291956 @default.
- W590400145 cites W1979959932 @default.
- W590400145 cites W1981454865 @default.
- W590400145 cites W1982549782 @default.
- W590400145 cites W1983475767 @default.
- W590400145 cites W1989395728 @default.
- W590400145 cites W1990553247 @default.
- W590400145 cites W1991368154 @default.
- W590400145 cites W1992439707 @default.
- W590400145 cites W1994302261 @default.
- W590400145 cites W1995541421 @default.
- W590400145 cites W1998589258 @default.
- W590400145 cites W1998866422 @default.
- W590400145 cites W1999039886 @default.
- W590400145 cites W2001375089 @default.
- W590400145 cites W2004543653 @default.
- W590400145 cites W2006058264 @default.
- W590400145 cites W2006406420 @default.
- W590400145 cites W2007665402 @default.
- W590400145 cites W2010671168 @default.
- W590400145 cites W2011930844 @default.
- W590400145 cites W2021669040 @default.
- W590400145 cites W2027776781 @default.
- W590400145 cites W2032509707 @default.
- W590400145 cites W2035444132 @default.
- W590400145 cites W2035523372 @default.
- W590400145 cites W2040244284 @default.
- W590400145 cites W2048222282 @default.
- W590400145 cites W2048370431 @default.
- W590400145 cites W2050155687 @default.
- W590400145 cites W2052648581 @default.
- W590400145 cites W2053300262 @default.
- W590400145 cites W2056553538 @default.
- W590400145 cites W2056876979 @default.
- W590400145 cites W2066154329 @default.
- W590400145 cites W2073414154 @default.
- W590400145 cites W2073688273 @default.
- W590400145 cites W2074984071 @default.
- W590400145 cites W2084563915 @default.
- W590400145 cites W2093492873 @default.
- W590400145 cites W2095965170 @default.
- W590400145 cites W2113695865 @default.
- W590400145 cites W2114376475 @default.
- W590400145 cites W2115309764 @default.
- W590400145 cites W2125819523 @default.
- W590400145 cites W2128340506 @default.
- W590400145 cites W2130622792 @default.
- W590400145 cites W2144186164 @default.
- W590400145 cites W2148848444 @default.
- W590400145 cites W2152602238 @default.
- W590400145 cites W2158770426 @default.
- W590400145 cites W2163940516 @default.
- W590400145 cites W2883132624 @default.
- W590400145 cites W3023210873 @default.
- W590400145 cites W3024211184 @default.
- W590400145 cites W3102430328 @default.
- W590400145 cites W3103590159 @default.
- W590400145 cites W3103831950 @default.
- W590400145 cites W4229628856 @default.
- W590400145 cites W45742637 @default.
- W590400145 doi "https://doi.org/10.1007/978-3-319-09749-7_6" @default.
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