Structure and Evolution of ``Brown'' Dwarfs, Extrasolar Giant Planets, and Jupiter

Details Structure and Evolution of ``Brown'' Dwarfs, Extrasolar Giant Planets, and Jupiter Structure and Evolution of ``Brown'' Dwarfs, Extrasolar Giant Planets, and Jupiter

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..4cf.aa001h&link_type=abstract

American Physical Society, Four Corners Annual Meeting November 2 - 3, 2001 New Mexico State University; Las Cruces, New Mexico

Physics

Scientific paper

Detections of many extrasolar objects in the mass range from ~ Saturn's mass to many tens of Jupiter's mass have provided a new perspective on jovian planets. We now realize that nature somehow can accumulate small gravitationally-bound masses (less than one-thousandth of a solar mass) of nebular gas, and in some cases, transport these masses to orbital distances of only six million km from the primary star. The provisional IAU distinction between planets and brown dwarfs does not assign planethood to Jupiter on the basis of its mode of origin, but on the basis of its being below the threshhold of thermonuclear deuterium burning. The latter phenomenon is a fairly insignificant event in the evolution of brown dwarfs, so differences in mode of origin could in principle provide a better distinction between a planet such as Jupiter and a brown dwarf. The problem is, there is not a clear understanding of these differences at present. This talk will emphasize the points of similarity between brown dwarfs and Jupiter.

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