From Interstellar Dust to Comets: Distributed Co in Comet Halley View Full Text


Ontology type: schema:Chapter     


Chapter Info

DATE

1998

AUTHORS

J. Mayo Greenberg , Aigen Li

ABSTRACT

Some simple molecules in comet comae like CO, C2, C3, CN, H2CO, 3+ appear to be distributed in such a way that they are neither directly emitted from the nucleus surface nor created as daughter molecules from more complex gas phase species. The only remaining possible source is the organic component in comet dust. The requirements imposed on the comet dust grains by the distributed CO emission are that they be heated sufficiently to evaporate a large fraction of the more volatile fraction of the complex organic refractory molecules and that a large fraction of these contain CO groups. Approximating the size (mass) distribution of the comet dust by that derived for Comet Halley, and assuming that the refractory organics remaining on the silicate cores are the heating agent by solar radiation in fluffy aggregates of interstellar core-mantle particles, imposes a minimum dust porosity of 0.975 ≤ P ≤ 0.99. Such porosities are consistent with those required to account for the silicate and organic spectral emission by Comet Halley dust and imply comet nucleus densities of p < 0.3 gcm−3. More... »

PAGES

337-351

Book

TITLE

Solar System Ices

ISBN

978-94-010-6209-1
978-94-011-5252-5

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-94-011-5252-5_14

DOI

http://dx.doi.org/10.1007/978-94-011-5252-5_14

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1044647120


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