Mathematics – Probability
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p21a1589t&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P21A-1589
Mathematics
Probability
[5430] Planetary Sciences: Solid Surface Planets / Interiors
Scientific paper
With the rapid development of observational instruments and techniques, more than a dozen of "super Earths" (which is defined as a planet of which mass is less than 10M_E) have been detected already. Ongoing and oncoming space transit surveys (CoRoT, Kepler, TESS and JWST) will detect more and more planets of these sizes. The detection probability of transit method is proportional to inverse of semi-major axis of planet, and thus closer planets are more easily detected. In fact, most of detected super Earths is orbiting with relatively small semi-major axis around its host star. In this situation, the tidal interaction with host star is a very important heating mechanism for the planetary interior, while the situation is not the case of planets in our Solar system (except for the satellites of Jupiter and Saturn). Thus, the close-in super Earths are good targets to understand the mechanism of tidal dissipation inside rocky planets. In this context, we have simulated coupled thermal- and orbital-evolution of extra solar super Earths due to tidal dissipation inside them taking into account temperature- dependence of mantle rheology of rocky planets. The tidal dissipation affects the thermal state of planetary interior, whereas the tidal dissipation rate is highly affected by thermal state of planetary interior due to temperature dependence of mantle rheology. Especially, the viscosity of rocky mantle depends strongly on the temperature, which controls the dissipation rate. Therefore, the thermal evolution and orbital evolution is coupled through this tidal dissipation. Thus, we took into account such temperature dependencies of rock rheology and examined how it affects the evolution. We will show there are 2 regimes in the a-e plane where the thermal- and orbital-evolution is clearly changed. If the initial eccentricity is too high and/or semi-major axis is too low, the tidal dissipation occurs sufficiently to balance the mantle cooling rate due to convection. Thus the thermal evolution is regulated by temperature dependency of mantle rheology. On the other hand, if initial a and e are suitable, the tidal dissipation rate does not overcome the cooling rate and the mantle temperature is also monotonically decreased. This is because the higher the temperature is, the lower the dissipation rate is. According to the result, we would like to discuss about the observational constraints for tidal dissipation inside these super Earths.
Tachinami Chihiro
Yuen Dave A.
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