When a star reaches the red giant stage in the course of its evolution, its closest planets are in its atmosphere. Numerical gas dynamic models are constructed for hypersonic flow around planets by matter in the atmosphere of a red giant. The results are compared with analytic models for the motion of planets in the atmospheres of stars.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
G. M. Rudnitskij, The Impact of Large-Scale Surveys on Pulsating Star Research, ASP Conference Series 203, 384 (2000).
G. M. Rudnitskij, Publ. Astron. Soc. Aust. 19, 499 (2002).
M. A. Tsikulin, Shock Waves Produced by the Motion of Large Meteoric Objects in the Atmosphere [in Russian], Nauka, Moscow (1969).
V. P. Stulov, V. N. Mirskii, and A. I. Vislyi, Aerodynamics of Bolides [in Russian], Fizmatlit, Moscow (1995).
O. M. Belotserkovskii and V. N. Fomin, Calculation of radiative gas flows in shock layers, Zhurnal vychislitel’noi matematiki i matematicheskoi fiziki 9, 397 (1969).
Bai Shi-i, Radiative Gas Dynamics [Russian translation], Mir, Moscow (1968).
K. P. Stanyukovich, Nonstationary Motion of Continuous Media [in Russian], Nauka, Moscow (1971).
Ya. B. Zeldovich and Yu. P. Raizer, Physics of Shock Waves and High-temperature Hydrodynamic Phenomena [in Russian], Nauka, Moscow (1966).
R. W. MacCormack, AIAA Paper 69-354 (1969).
M. I. Verigin, et al., Kosmicheskie issledovaniya 37, 38 (1999).
Author information
Authors and Affiliations
Corresponding author
Additional information
Translated from Astrofizika, Vol. 58, No. 3, pp. 465-475 (August 2015).
Rights and permissions
About this article
Cite this article
Volobueva, M.I., Tarakanov, P.A. Planetary Motion in the Atmospheres of Red Giants. Astrophysics 58, 430–440 (2015). https://doi.org/10.1007/s10511-015-9396-3
Received:
Revised:
Published:
Issue Date:
DOI: https://doi.org/10.1007/s10511-015-9396-3