Volatiles in Terrestrial Planets Orbiting Within Habitable Zones of Low-Mass Stars

Details Volatiles in Terrestrial Planets Orbiting Within Habitable Zones of Low-Mass Stars Volatiles in Terrestrial Planets Orbiting Within Habitable Zones of Low-Mass Stars

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.b11e..07l&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #B11E-07

Biology

[0406] Biogeosciences / Astrobiology And Extraterrestrial Materials, [6296] Planetary Sciences: Solar System Objects / Extra-Solar Planets

Scientific paper

Dynamical considerations derived from analytic calculations and numerical experiments imply that Earth-mass planets that accrete in regions that become habitable zones of M dwarf stars form within several million years. Temperatures in these regions during planetary accretion are higher than those encountered by the material that formed the Earth. Collision velocities during and after the prime planetary accretionary epoch are larger than for 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 have abundances of the volatiles required life that are substantially less than those of Earth.

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