Distant future of the Sun and Earth revisited
Article first published online: 13 MAR 2008
©2008 The Authors. Journal compilation © 2008 RAS
Monthly Notices of the Royal Astronomical Society
Volume 386, Issue 1, pages 155–163, May 2008
How to Cite
Schröder, K.-P. and Connon Smith, R. (2008), Distant future of the Sun and Earth revisited. Monthly Notices of the Royal Astronomical Society, 386: 155–163. doi: 10.1111/j.1365-2966.2008.13022.x
- Issue published online: 13 MAR 2008
- Article first published online: 13 MAR 2008
- Accepted 2008 January 23. Received 2007 December 14; in original form 2007 September 25
- Sun: evolution;
- solar-terrestrial relations;
- stars: evolution;
- stars: mass-loss;
- white dwarfs
We revisit the distant future of the Sun and the Solar system, based on stellar models computed with a thoroughly tested evolution code. For the solar giant stages, mass loss by the cool (but not dust-driven) wind is considered in detail. Using the new and well-calibrated mass-loss formula of Schröder & Cuntz, we find that the mass lost by the Sun as a red giant branch (RGB) giant (0.332 M⊙, 7.59 Gyr from now) potentially gives planet Earth a significant orbital expansion, inversely proportional to the remaining solar mass.
According to these solar evolution models, the closest encounter of planet Earth with the solar cool giant photosphere will occur during the tip-RGB phase. During this critical episode, for each time-step of the evolution model, we consider the loss of orbital angular momentum suffered by planet Earth from tidal interaction with the giant Sun, as well as dynamical drag in the lower chromosphere. As a result of this, we find that planet Earth will not be able to escape engulfment, despite the positive effect of solar mass loss. In order to survive the solar tip-RGB phase, any hypothetical planet would require a present-day minimum orbital radius of about 1.15 au. The latter result may help to estimate the chances of finding planets around white dwarfs.
Furthermore, our solar evolution models with detailed mass-loss description predict that the resulting tip-AGB (asymptotic giant branch) giant will not reach its tip-RGB size. Compared to other solar evolution models, the main reason is the more significant amount of mass lost already in the RGB phase of the Sun. Hence, the tip-AGB luminosity will come short of driving a final, dust-driven superwind, and there will be no regular solar planetary nebula (PN). The tip-AGB is marked by a last thermal pulse, and the final mass loss of the giant may produce a circumstellar (CS) shell similar to, but rather smaller than, that of the peculiar PN IC 2149 with an estimated total CS shell mass of just a few hundredths of a solar mass.