The Young Sun's XUV-activity As A Constraint For Lower CO2-limits In The Earth's Archean Atmosphere


The evolution of the Sun’s X-ray flux at the orbit of the Earth during the Archean for three cases of the Sun rotational evolution. These cases are for the Sun being a slow (10th percentile), medium (50th percentile), and fast (90th percentile) rotator. The initial rotation periods (at 1 Myr after solar system formation) for the Sun in these three scenarios are 9, 4, and 0.7 days respectively. Two of the X-ray and ultraviolet spectra from Claire et al. (2012) that we use at two different values for the X-ray flux are shown in the insert.

Despite their importance for determining the evolution of the Earth's atmosphere and surface conditions, the evolutionary histories of the Earth's atmospheric CO2 abundance during the Archean eon and the Sun's activity are poorly constrained.

In this study, we apply a state-of-the-art physical model for the upper atmosphere of the Archean Earth to study the effects of different atmospheric CO2/N2 mixing ratios and solar activity levels on the escape of the atmosphere to space.

We find that unless CO2 was a major constituent of the atmosphere during the Archean eon, enhanced heating of the thermosphere by the Sun's strong X-ray and ultraviolet radiation would have caused rapid escape to space. We derive lower limits on the atmospheric CO2 abundance of approximately 40\% at 3.8~billion years ago, which is likely enough to counteract the faint young Sun and keep the Earth from being completely frozen.

Furthermore, our results indicate that the Sun was most likely born as a slow to moderate {rotating young G-star} to prevent rapid escape, putting essential constraints on the Sun's activity evolution throughout the solar system's history. In case that there were yet unknown cooling mechanisms present in the Archean atmosphere, this could reduce our CO2 stability limits, and it would allow a more active Sun.

C.P. Johnstone, H. Lammer, K.G. Kislyakova, M. Scherf, M. Güdel

Comments: 40 pages, 6 figures. This is a preprint accepted to be published in Earth and Planetary Science Letters
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR); Atmospheric and Oceanic Physics (physics.ao-ph); Geophysics (physics.geo-ph)
Cite as: arXiv:2109.01604 [astro-ph.EP] (or arXiv:2109.01604v1 [astro-ph.EP] for this version)
Submission history
From: Manuel Scherf
[v1] Fri, 3 Sep 2021 16:28:10 UTC (1,371 KB)
https://arxiv.org/abs/2109.01604
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