Photoionized and Photodissociated Regions Around Main-Sequence Stars

Details Photoionized and Photodissociated Regions Around Main-Sequence Stars Photoionized and Photodissociated Regions Around Main-Sequence Stars

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.4010d&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #40.10; Bulletin of the American Astronomical Society, Vol. 28, p.885

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We obtain, using a radiative transfer model, the basic structures and sizes of the photoionized and photodissociated (PDR) regions produced by stars of different effective temperatures and metallicities for dusty and dust-free environments. The rate of ionizing and dissociating photons that give rise to those regions are calculated using the LTE atmosphere models of Kurucz (1993). In addition, the stars are assumed to be embedded in molecular clouds with uniform densities ranging from 10 cm(-3) to 10(5) {cm}(-3) . The results for the different environments indicate that metallicity effects are evident only for low temperature stars, while dust effects are considerable only for hot stars in a high density medium.

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