Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5805e&link_type=abstract
American Astronomical Society, DPS meeting #40, #58.05; Bulletin of the American Astronomical Society, Vol. 40, p.503
Astronomy and Astrophysics
Astronomy
Scientific paper
Early in terrestrial planet evolution energetic impact, radiodecay, and core formation may have created one or more whole or partial silicate mantle magma oceans. In young extrasolar systems, such hot objects could be visible despite their small size. Here I describe the expected solidification process of rocky planets, and model the time to cool surface conditions for whole and partial magma oceans. Included in my calculations are partitioning of water and carbon dioxide between solidifying mantle cumulate mineral assemblages, evolving liquid compositions, and a growing atmosphere. I find that for Earth-sized planets small initial volatile contents (0.05 wt% H2O, 0.01 wt% CO2) can produce atmospheres in excess of 100 bars, and that mantle solidification is 98% complete in less than 5 Myr years for all magma oceans investigated on both Earth and Mars, and less than 100,000 years for low-volatile magma oceans. Subsequent cooling to surface temperatures below 600C occurs in five to tens of Ma, underscoring the likelihood of observing young planets.
No associations
LandOfFree
Temperatures of Hot Young Accreting Planets and Timescales for Cooling does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Temperatures of Hot Young Accreting Planets and Timescales for Cooling, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Temperatures of Hot Young Accreting Planets and Timescales for Cooling will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1792126