Infrared Spectroscopy of the Recombination Line Maser Star MWC349 with ISO

Details Infrared Spectroscopy of the Recombination Line Maser Star MWC349 with ISO Infrared Spectroscopy of the Recombination Line Maser Star MWC349 with ISO

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.4719q&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #47.19; Bulletin of the American Astronomical Society, Vol. 29, p.1288

Astronomy and Astrophysics

Astronomy

1

Scientific paper

MWC349 is a peculiar emission line star; among its outstanding features are strong hydrogen recombination line masers associated with the circumstellar disk. We have observed MWC349 with the SWS and LWS grating spectrometers on the ISO satellite. The spectrum covers the full wavelength range from 2.35mu m to 190mu m. Numerous hydrogen and helium recombination lines have been detected, along with about 30 fine structure lines, and the continuum emission from hot circumstellar dust. The fine structure lines cover ionization potentials up to about 50eV. For several elements, lines from different ionization stages are observed. This enables us to determine the effective temperature of the star. The uncertainty of the derived temperature is dominated by uncertainties in the stellar models used. Among the ~ 100 detected hydrogen recombination lines are all 12 alpha -transitions within the wavelength range accessible to ISO, from Bralpha at 4.05mu m to H15alpha at 169.4mu m. The alpha -lines with n <= 6 are optically thick; the lines with higher n are amplified, and thus constitute infrared lasers. By combining the ISO results with millimeter and sub-millimeter data, we can produce the first global view on the recombination line laser / maser phenomenon in this star. We infer that the maximum line-integrated amplification -- by a factor of ~ 30 -- occurs in the region near n = 19 at ~ 300mu m.

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