SSP seminar
 

CHON Ices and the Formation of Saturn

Sally Robinson (UCO/Lick Observatory)

Monday 22nd October 2007, 12:00
Pratt conference room, 60 Garden Street

Previous core accretions simulations have found that the formation timescale of Saturn is far longer than a reasonable lifetime of the solar nebula. Saturn's formation is impaired by (1) the long orbital timescale (compared with Jupiter), leading to a slower planetesimal collision rate, and (2) the assumption that H2O is the only volatile that gets incorporated into planetesimals. We use a 1+1-d evolving solar nebula model and a 214-species chemical reaction network to calculate the solid surface density available to form Saturn. New core accretion simulations based on the results of our protostellar disk model show that Saturn can form in less than 4 Myr.

 
 

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