The formation of Pegasi planets: fluid-dynamics, mass-function and observational tests

Details The formation of Pegasi planets: fluid-dynamics, mass-function and observational tests The formation of Pegasi planets: fluid-dynamics, mass-function and observational tests

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006tafp.conf...59w&link_type=abstract

"Tenth Anniversary of 51 Peg-b: Status of and prospects for hot Jupiter studies. Colloquium held at Observatoire de Haute Proven

Physics

Scientific paper

Fluid-dynamical models based on the planetesimal hypothesis show that Pegasi-planets may form near their stars if sufficiently large reservoirs of gas and solids are available. The conventional minimum mass nebula cannot provide such reservoirs inside ≈1 AU, but more generally, gravitationally stable nebulae do. Alternatively Pegasi planets might form in a special giant planet formation region, further out in the nebula and subsequently migrate to their present-day orbits. Three observational tests distinguish between the two scenarii:
(1) the existence of Hot Neptunes,
(2) birthplace exclusion in binaries, and
(3) Hill-exclusion stability criteria. Scenario (1) uses the fact that migrating planets with about 10 Earth masses usually accrete gas. Scenario (2) uses the absence of an `appropriate' birth-place, and (3) the fact the Hill-spheres shrink as planets migrate inwards with increasing speed. For the in-situ formation-hypothesis the evolution of a Pegasi planet is calculated for the first 200 Myr from planetesimal accretion and the fluid-dynamics of gas-accretion with spherical symmetry.

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