Abstract
The paper presents the results of calculations using an approximate approach to estimating the thermal loss of the atmosphere of a hot exoplanet. The objective of simulation was to study a system of a yellow dwarf of the spectral type G with an exoplanet like a hot sub-Neptune or super-Earth. Estimates of the atmospheric loss rate for a hot sub-Neptune in weakly and strongly elliptical orbits are obtained. Calculations have shown that the atmospheric loss \(\dot{M}_{T}\) averaged over the orbital period of the model hot sub-Neptune varies from \(5.8\times 10^{17}\) g for an orbit with \(e=0.0\) to \(2.6\times 10^{18}\) g for an orbit with \(e=0.8\), that is, it increases by almost 4.5 times. Moreover, for \(e=0.2,0.4,\) and \(0.6\) the values of \(\dot{M}_{T}\) are equal to \(6.3\times 10^{17}\) g, \(7.6\times 10^{17}\) g, and \(1.2\times 10^{18}\) g respectively. Using the average atmospheric mass loss per orbit, we can approximately estimate the time of total atmospheric escape of the considered sub-Neptune—at \(e=0.0\), this time is approximately equal to 0.32 billion years, and at \(e=0.8\)—approximately 0.07 billion years. Accordingly, we can conclude that the initial ellipticity of the hot exoplanet’s orbit is an important factor in estimating the loss rate of the primary hydrogen-helium atmosphere for sub-Neptunes and super-Earths.
REFERENCES
A. A. Avtaeva and V. I. Shematovich, Solar System Research 55 (2), 150 (2021).
A. A. Avtaeva and V. I. Shematovich, Solar System Research 55 (2), 150 (2021).
A. A. Avtaeva and V. I. Shematovich, Solar System Research 56 (2), 67 (2022).
D. V. Bisikalo, V. I. Shematovich, P. V. Kaygorodov, and A. G. Zhilkin, Physics Uspekhi 64 (8), 747 (2021).
R. P. Butler, J. T. Wright, G. W. Marcy, et al., Astrophys. J. 646 (1), 505 (2006).
N. V. Erkaev, Y. N. Kulikov, H. Lammer, et al., Astron. and Astrophys. 472 (1), 329 (2007).
N. Fujita, Y. Hori, and T. Sasaki, Astrophys. J. 928 (2), id. 105 (2022).
B. Jackson, E. Jensen, S. Peacock, et al., Celestial Mechanics and Dynamical Astronomy 126 (1–3), 227 (2016).
P. V. Kaygorodov and D. V. Bisikalo, Astronomy Reports 66 (11), 1017 (2022).
D. Kubyshkina, L. Fossati, N. V. Erkaev, et al., Astrophys. J. 866 (2), article id. L18 (2018).
D. Kubyshkina, A. A. Vidotto, L. Fossati, and E. Farrell, Monthly Notices Royal Astron. Soc. 499 (1), 77 (2020).
H. Lammer, F. Selsis, I. Ribas, et al., Astrophys. J. 598 (2), L121 (2003).
R. Luger, R. Barnes, E. Lopez, et al., Astrobiology 15 (1), 57 (2015).
J. E. Owen, Annual Rev. Earth and Planetary Sci. 47, 67 (2019).
V. I. Shematovich, Solar System Research 44 (2), 96 (2010).
V. I. Shematovich, D. E. Ionov, and H. Lammer, Astron. and Astrophys. 571, id. A94 (2014).
V. I. Shematovich and M. Y. Marov, Physics Uspekhi 61 (3), 217 (2018).
L. Sproß, M. Scherf, V. I. Shematovich, et al., Astronomy Reports 65 (4), 275 (2021).
V. Van Eylen, S. Albrecht, X. Huang, et al., Astron. J. 157 (2), article id. 61 (2019).
J.-W. Xie, S. Dong, Z. Zhu, et al., Proc. National Academy Sci. 113 (41), 11431 (2016).
Funding
This work was supported by the Russian Science Foundation (project No. 22-22-00909).
Author information
Authors and Affiliations
Corresponding author
Ethics declarations
The authors declare no conflict of interest.
Additional information
Translated by T. Sokolova
Rights and permissions
About this article
Cite this article
Simonova, A.A., Shematovich, V.I. Approximate Calculation of the Thermal Loss of the Atmosphere of a Hot Exoplanet in a Low Orbit with Taking into Account the Ellipticity. Astrophys. Bull. 78, 217–224 (2023). https://doi.org/10.1134/S1990341323020098
Received:
Revised:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1134/S1990341323020098