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/ D. Kubyshkina [et al.] // Astron. Astrophys. - 2018. - Vol. 619. - Ст. A151, DOI 10.1051/0004-6361/201833737. - Cited References:101. - We acknowledge the Austrian Forschungsforderungsgesellschaft FFG project "TAPAS4CHEOPS" P853993, the Austrian Science Fund (FWF) NFN project S11607-N16, the FWF project P27256-N27 and the FWF project P30949-N36. N.V.E. acknowledges support by the RFBR grant No. 18-05-00195-a and 16-52-14006 ANF_a. We thank the anonymous referee for the positive approach and the useful comments that led to a significant improvement of the manuscript. . - ISSN 1432-0746РУБ Astronomy & Astrophysics

Аннотация: There is growing observational and theoretical evidence suggesting that atmospheric escape is a key driver of planetary evolution. Commonly, planetary evolution models employ simple analytic formulae (e.g. energy limited escape) that are often inaccurate, and more detailed physical models of atmospheric loss usually only give snapshots of an atmosphere's structure and are difficult to use for evolutionary studies. To overcome this problem, we have upgraded and employed an existing upper atmosphere hydrodynamic code to produce a large grid of about 7000 models covering planets with masses 1-39 M-circle plus with hydrogen-dominated atmospheres and orbiting late-type stars. The modelled planets have equilibrium temperatures ranging between 300 and 2000 K. For each considered stellar mass, we account for three different values of the high-energy stellar flux (i.e. low, moderate, and high activity). For each computed model, we derived the atmospheric temperature, number density, bulk velocity, X-ray and EUV (XUV) volume heating rates, and abundance of the considered species as a function of distance from the planetary centre. From these quantities, we estimate the positions of the maximum dissociation and ionisation, the mass-loss rate, and the effective radius of the XUV absorption. We show that our results are in good agreement with previously published studies employing similar codes. We further present an interpolation routine capable to extract the modelling output parameters for any planet lying within the grid boundaries. We used the grid to identify the connection between the system parameters and the resulting atmospheric properties. We finally applied the grid and the interpolation routine to estimate atmospheric evolutionary tracks for the close-in, high-density planets CoRoT-7 b and HD219134 b,c. Assuming that the planets ever accreted primary, hydrogen-dominated atmospheres, we find that the three planets must have lost them within a few Myr.

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Держатели документа:
Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
Russian Acad Sci, Siberian Branch, Inst Computat Modelling, Krasnoyarsk 660036, Russia.
Siberian Fed Univ, Krasnoyarsk 660041, Russia.
Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
Univ Graz Univ, IGAM, Inst Phys, Univ Pl 5, A-8010 Graz, Austria.

Доп.точки доступа:
Kubyshkina, D.; Fossati, L.; Erkaev, N. V.; Johnstone, C. P.; Cubillos, P. E.; Kislyakova, K. G.; Lammer, H.; Lendl, M.; Odert, P.; Austrian Forschungsforderungsgesellschaft FFG project "TAPAS4CHEOPS" [P853993]; Austrian Science Fund (FWF) NFN project [S11607-N16]; FWF [P30949-N36, P27256-N27]; RFBR [18-05-00195-a, 16-52-14006 ANF_a]