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The Beta Pictoris Phenomenon in Young Stars With Accreting GasProgram Hae2BPIC resulted in usable ISO spectra of three young, Herbig Ae stars: HR 5999 (A7e, t=0.6 Myr), SV Cep (al-2e, t=1-3 Myr), and MW Vul (Al-2e, t=1-3 Myr). While too small a sample to pursue our original goal of surveying the silicate emission in these young, protoplanetary disk systems, comparison of these data with ground-based IR spectra, and published ISO observations of other HAe stars (especially the posters at PPIV) reveals the following: The known binary stars in the sample show signatures of partially crystal line silicate features by t=0.6 Myr, at an epoch when ostensibly single Herbig Ae stars have substantially stronger silicate emission dominated by amorphous grains. The known binary stars also show deficits in the optically thick continuum flux relative to coeval single stars. Comparison of ISO spectra indicates that the flux deficit seen in WD 163296 over 10-100 microns relative to AB Aur reflects a real deficit of material interior to 300.
Document ID
19990078758
Acquisition Source
Goddard Space Flight Center
Document Type
Contractor or Grantee Report
Authors
Grady, Carol A. (Eureka Scientific, Inc. Oakland, CA United States)
Date Acquired
September 6, 2013
Publication Date
September 1, 1999
Subject Category
Astronomy
Funding Number(s)
CONTRACT_GRANT: NASA Order S-78611-Z
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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