Spectroscopic observations of PU Vulpeculae

Details Spectroscopic observations of PU Vulpeculae Spectroscopic observations of PU Vulpeculae

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986aj.....91..563k&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 91, March 1986, p. 563-569.

Astronomy and Astrophysics

Astronomy

30

A Stars, Binary Stars, M Stars, Stellar Spectrophotometry, Symbiotic Stars, Variable Stars, Giant Stars, Hot Stars, Infrared Spectra, Stellar Spectra, Thermonuclear Reactions

Scientific paper

Optical and infrared spectrophotometric observations demonstrate that the nova-like variable PU Vulpeculae is a symbiotic binary composed of an M4-5 giant and a hot companion whose expanding atmosphere mimics an A supergiant. Fits to the optical/infrared data suggest the system is reddened by E(B-V) = 0.4-0.5. The 1979 outburst appears to be the result of a thermonuclear runaway on the surface of a white dwarf, as in the symbiotic novae AG Peg and RR Tel. Dust condensation in the expanding envelope ejected in the eruption, or an eclipse of the hot component by the M giant companion, can explain many features of the 1980 minimum, but neither mechanism provides a satisfactory explanation for all the available data.

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