Planets Formed in Habitable Zones of M Dwarf Stars Probably Lack Volatiles

Details Planets Formed in Habitable Zones of M Dwarf Stars Probably Lack Volatiles Planets Formed in Habitable Zones of M Dwarf Stars Probably Lack Volatiles

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20917906l&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #179.06; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

Dynamical considerations, presented herein via analytic scalings and numerical experiments, imply that Earth-mass planets accreting in regions that become habitable zones of M dwarf stars form within several million years. Collision velocities during and after the prime accretionary epoch are somewhat larger than for Earth. Temperatures in protoplanetary disks and during the star's pre-main sequence evolution are higher than those encountered by Earth. These factors suggest that planets orbiting low mass main sequence stars are likely to be either too distant (and thus too cold) for carbon/water based life on their surfaces or lacking in the required volatiles.

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