naa a22 4500 510732364 CHVBK 20180411082957.0 cr unu---uuuuu 180411e20131001xx s 000 0 eng 10.1134/S1063772913100016 doi (NATIONALLICENCE)springer-10.1134/S1063772913100016 Types of gaseous envelopes of "hot Jupiter” exoplanets [Elektronische Daten] [D. Bisikalo, P. Kaigorodov, D. Ionov, V. Shematovich] As a rule, the orbital velocities of "hot Jupiters,” i.e., exoplanets with masses comparable to the mass of Jupiter and orbital semi-major axes less than 0.1 AU, are supersonic relative to the stellar wind, resulting in the formation of a bow shock. Gas-dynamical modeling shows that the gaseous envelopes around hot Jupiters can belong to two classes, depending on the position of the collision point. if the collision point is inside the Roche lobe of the planet, the envelopes have the almost spherical shapes of classical atmospheres, slightly distorted by the influence of the star and interactions with the stellar-wind gas; if the collision point is located outside the Roche lobe, outflows from the vicinity of the Lagrangian points L1 and L2 arise, and the envelope becomes substantially asymmetrical. The latter class of objects can also be divided into two types. If the dynamical pressure of the stellar-wind gas is high enough to stop the most powerful outflow from the vicinity of the inner Lagrangian point L1, a closed quasi-spherical envelope with a complex shape forms in the system. If the wind is unable to stop the outflow from L1, an open aspherical envelope forms. The possible existence of atmospheres of these three types is confirmed by 3D numerical modeling. Using the typical hot Jupiter HD 209458b as an example, it is shown that all three types of atmospheres could exist within the range of estimated parameters of this planet. Since different types of envelopes have different observational manifestations, determining the type of envelope in HD 209458b could apply additional constrains on the parameters of this exoplanet. Pleiades Publishing, Ltd., 2013 Bisikalo D. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut Kaigorodov P. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut Ionov D. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut Shematovich V. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut Astronomy Reports Springer US; http://www.springer-ny.com 57/10(2013-10-01), 715-725 1063-7729 57:10<715 2013 57 11444 https://doi.org/10.1134/S1063772913100016 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1134/S1063772913100016 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Bisikalo D. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut NATIONALLICENCE 700 1- Kaigorodov P. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut NATIONALLICENCE 700 1- Ionov D. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut NATIONALLICENCE 700 1- Shematovich V. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia aut NATIONALLICENCE 773 0- Astronomy Reports Springer US; http://www.springer-ny.com 57/10(2013-10-01), 715-725 1063-7729 57:10<715 2013 57 11444 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer