Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-27T07:59:18.308Z Has data issue: false hasContentIssue false
  • English
  • Français

Mass-loss varying luminosity and its implication to the solar evolution

Published online by Cambridge University Press:  29 January 2021

Negessa Tilahun Shukure ,
Solomon Belay Tessema  and
Endalkachew Mengistu
Negessa Tilahun Shukure
Affiliation:
Astronomy and Astrophysics Research and Development Division, Entoto Observatory and Research Center, Ethiopian Space Science and Technology Institute, P.O.Box 33679, Addis Ababa, Ethiopia Addis Ababa University, P.O.Box 1176, Addis Ababa, Ethiopia Dilla University, P.O.Box 419, Dilla, Ethiopia emails: nagessa2006@gmail.com; tessemabelay@gmail.com; 2fendalk@gmail.com
Solomon Belay Tessema
Affiliation:
Astronomy and Astrophysics Research and Development Division, Entoto Observatory and Research Center, Ethiopian Space Science and Technology Institute, P.O.Box 33679, Addis Ababa, Ethiopia
Endalkachew Mengistu
Affiliation:
Astronomy and Astrophysics Research and Development Division, Entoto Observatory and Research Center, Ethiopian Space Science and Technology Institute, P.O.Box 33679, Addis Ababa, Ethiopia
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Several models of the solar luminosity, , in the evolutionary timescale, have been computed as a function of time. However, the solar mass-loss, , is one of the drivers of variation in this timescale. The purpose of this study is to model mass-loss varying solar luminosity, , and to predict the luminosity variation before it leaves the main sequence. We numerically computed the up to 4.9 Gyrs from now. We used the solution to compute the modeled . We then validated our model with the current solar standard model (SSM). The shows consistency up to 8 Gyrs. At about 8.85 Gyrs, the Sun loses 28% of its mass and its luminosity increased to 2.2. The model suggests that the total main sequence lifetime is nearly 9 Gyrs. The model explains well the stage at which the Sun exhausts its central supply of hydrogen and when it will be ready to leave the main sequence. It may also explain the fate of the Sun by making some improvements in comparison to previous models.

Keywords

Sunmass-losssolar luminosity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S356: Nuclear Activity in Galaxies Across Cosmic Time , October 2019 , pp. 403 - 404
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Bahcall, J. N., Pinsonneault, M. H., & Basu, S. 2001, APJ, 555(2), p. 990 10.1086/321493CrossRefGoogle Scholar
Feulner, G. 2012, Reviews of Geophysics, 50 (2)10.1029/2011RG000375CrossRefGoogle Scholar
Gough, D. O. 1981, Sol. Phys., 74, 21–34 10.1007/BF00151270CrossRefGoogle Scholar
Kaplan, G. H. 1981, editor US Naval Observatory, No. 163Google Scholar
Kopp, G. 2016, Journal of space weather and space climate, 6, p. A30 10.1051/swsc/2016025CrossRefGoogle Scholar