Chemical Reactions and Dust Destruction in Protoplanetary Accretion Disks

Details Chemical Reactions and Dust Destruction in Protoplanetary Accretion Disks Chemical Reactions and Dust Destruction in Protoplanetary Accretion Disks

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1101f&link_type=abstract

American Astronomical Society, DPS meeting #28, #11.01; Bulletin of the American Astronomical Society, Vol. 28, p.1106

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We consider the gas phase chemistry in a protoplanetary accretion disk, especially the chemistry initiated in the gas phase by destruction of dust close to the central star. Slow radial particle transport moves gas and dust from the cold outer parts of a protoplanetary accretion into its warm central part where chemical reactions in the gas phase are activated. At the same time gases frozen on the surface of dust grains are vaporized and later the dust grains themselves are vaporized or destroyed by chemical surface reactions. These processes initiate a rich chemistry in the protoplanetary accretion disk. The simulation of chemical reactions, as in the case of an accretion disk, mostly leads to a large and stiff system of differential or differential-algebraic equations. For the integration of such systems implicit methods are required. We use here a efficient BDF-method. Typical applications for chemical processes (chemistry and dust destruction) in an accretion disk are treated with this method. The corresponding code DAESOL turned out to be more robust and much faster than the more conventional code used first. Our conclusion for the chemistry in a protoplanetary accretion disk are presented. The fundamental result of this work is the presence of of huge amounts of methane and ammonia where the terrestrial planets are actually located. These two species are known to have been present in the early atmosphere of the Earth.

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