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Protoplanetary Material Around Nearby Stars

Published online by Cambridge University Press:  04 August 2017

Hartmut H. Aumann
Hartmut H. Aumann*
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 USA

Abstract

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A statistical analysis of IRAS observations indicates that about 20% of the nearby main sequence stars, and probably a similar fraction of main sequence stars not detectable by IRAS, shows evidence of significant infrared excess beyond 12 microns. Spectral type A dwarfs are predominant, but not exclusive in showing large 60 micron excesses. Our solar system, when viewed from sufficient distance, appears to have, in contrast to this, less than 1% of cool infrared excess. These observational facts are consistent with the working hypothesis that cold infrared excess in stable main sequence stars is due to proto-planetary material, observable during the accretion phase in the evolution of a solar system.

Type
Section II. The Search for Other Planetary Systems
Information
Symposium - International Astronomical Union , Volume 112: The Search for Extraterrestrial Life: Recent Developments , 1985 , pp. 43 - 50
Copyright
Copyright © Reidel 1985 

References

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