Hydrodynamic Escape of Planetary Atmospheres during a Star’s X-ray/Extreme Ultraviolet Saturation – Size Limit on Rocky Exoplanets
Hydrodynamic Escape of Planetary Atmospheres during a Star’s X-ray and Extreme Ultraviolet Saturation May Impose a Size Limit of ~2 Earth Radii on Rocky Exoplanets
Owen Lehmer, David Catling
(Submitted on 7 Jun 2017)
Recent observations and analysis of small exoplanets have found that rocky planets like the Earth only have radii up to 1.5-2R⊕. Two general hypotheses exist for the cause of the dichotomy between rocky and gas-enveloped planets (or possible water worlds): either small planets do not easily form thick atmospheres, or the thick atmospheres on small planets easily escape driven by x-ray and extreme ultraviolet (XUV) emissions from young parent stars. Here we show that a cutoff between rocky and gas-enveloped planets due to hydrodynamic escape is most likely to occur at a mean radius of 1.76±0.38R⊕ (2σ) Earth radii around Sun-like stars. We examine the limit in rocky planet radii predicted by hydrodynamic escape across a wide range of possible model inputs using 10,000 parameter combinations drawn randomly from plausible parameter ranges. We find a cutoff between rocky and gas-enveloped planets that agrees with the observed cutoff. The large cross-section available for XUV absorption in the extremely distended primitive atmospheres of low mass planets results in complete loss of atmospheres during the ~100 Myr phase of stellar XUV saturation. In contrast, more massive planets have less distended atmospheres and less escape, and so retain thick atmospheres through XUV saturation and then indefinitely as the XUV and escape fluxes drop over time. The agreement between our model and exoplanet data leads us to conclude that hydrodynamic escape plausibly explains the observed upper limit on rocky planet size.
Comments: Submitted to ApJ on May 23, 2017
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1706.02050 [astro-ph.EP] (or arXiv:1706.02050v1 [astro-ph.EP] for this version)
Submission history
From: Owen Lehmer
[v1] Wed, 7 Jun 2017 05:34:12 GMT (731kb)
https://arxiv.org/abs/1706.02050
