Optical, infrared and millimetre-wave properties of Vega-like systems - II. Radiative transfer modelling

Details Optical, infrared and millimetre-wave properties of Vega-like systems - II. Radiative transfer modelling Optical, infrared and millimetre-wave properties of Vega-like systems - II. Radiative transfer modelling

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.283..457s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 283, Issue 2, pp. 457-470.

Astronomy and Astrophysics

Astronomy

33

Circumstellar Matter, Stars: Evolution, Planetary Systems, Infrared: Stars

Scientific paper

Vega-like stars are main-sequence stars that exhibit excess infrared emission due to dust grains which are believed to be distributed in circumstellar discs. We have recently published a new observational database for a large sample of candidate Vega-like systems, comprising optical, near-infrared and mm/submm-wave photometry, and mid-infrared spectra. This paper presents radiative transfer models of eight of our sources, calculated using an optically thin code. For some of the sources the observations are unable to constrain the models successfully, while for those with larger fractional excess luminosities, we are able to determine the parameters of the dust discs. Dust masses for the well-constrained models lie in the range (1-70)x10^-7 M_solar - considerably less than the derived masses for pre-main-sequence discs. The grain size distributions favour smaller grains, as is generally found for interstellar and Solar system dust. Large (~1 mm) grains are found to be abundant around SAO 179815 (HD 98800), but not around SAO 112630 and SAO 140789. The disc densities are found to fall off steeply with distance from the central stars. The derived inner radii of the discs vary from approximately one to several hundred au.

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