The infrared spectrum of the eruptive star PU Vulpeculae

Details The infrared spectrum of the eruptive star PU Vulpeculae The infrared spectrum of the eruptive star PU Vulpeculae

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...245..575b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 245, no. 2, May 1991, p. 575-579.

Astronomy and Astrophysics

Astrophysics

9

Binary Stars, Flare Stars, Infrared Stars, Symbiotic Stars, Accretion Disks, Cool Stars, Stellar Mass Ejection

Scientific paper

Infrared spectra were taken of PU Vul in 1988 to facilitate an understanding of the rapid changes that have been occurring on it. The infrared spectrum of what is probably a symbiotic nova showed both the CO absorption lines characteristic of a cool star and a rich emission line spectrum. The emission line flux ratios, calibrated by infrared photometry, do not agree with case B. If the conditions are not too far from case B and the lines are formed in a wind from the hot component of the binary, a mass loss rate of about 4 x 10 to the -6th solar mass/yr in 1988 is calculated. Analysis of line profiles indicates the presence of two peaks in addition to the main one. It is suggested that this structure is due to bipolar flow. The optimal thickness for Thomson scattering corresponding to the mass loss rate is calculated at 0.3.

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