The structure of dust disks around G35.2N, NGC 2071 and LkH-alpha234

Details The structure of dust disks around G35.2N, NGC 2071 and LkH-alpha234 The structure of dust disks around G35.2N, NGC 2071 and LkH-alpha234

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.238.1497d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 238, June 15, 1989, p. 1497-1512.

Astronomy and Astrophysics

Astronomy

29

Accretion Disks, Cosmic Dust, Early Stars, Pre-Main Sequence Stars, Thermal Emission, Ammonia, Astronomical Maps, Heating, Stellar Winds, Submillimeter Waves

Scientific paper

Observations of the thermal continuum emission from the dust around three young luminous stars have been used to determine the density structure of the dust. For G35.2N and NGC 2071, if the hot dust in the outflow region is heated by the mechanical energy of the stellar wind, then the wind mechanical luminosity is 5-40 percent of the bolometric luminosity. LkH-alpha234 is found to have a dust ring of radius of about 0.15 pc with a mass 10 times greater than that of the material inside it.

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