Photoevaporation of Planets around Massive Stars

Details Photoevaporation of Planets around Massive Stars Photoevaporation of Planets around Massive Stars

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..241i&link_type=abstract

The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004

Physics

Scientific paper

In the formation of stars, one expects accretion disks to develop. Recent models indicate that gas giants may form rapidly, on the order of centuries, owing to strong gravitational instabilities in disks. Supposing this to be the case even for hot massive stars, we address to what extent high levels of EUV radiation from early-type stars can lead to heating and significant atmospheric losses from a planet. Observationally, we know that such heating can lead to hydrodynamic ``blow-off'' as in the case of HD209485B, a planet in a small orbit around a solar-type star. Assuming a simplified energetics argument, we use a grid of stellar spectral models to calculate the heating and expected mass loss of a Jupiter-like planet.

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