The carbon-rich proto-planetary nebula IRAS 22272 + 5435

Journal Article · Mon Apr 01 04:00:00 EST 1991 · Astrophysical Journal; (United States)

DOI:https://doi.org/10.1086/169928· OSTI ID:5597325

Hrivnak, B J; Kwok, Sun ^[1]

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1. Valparaiso University, IN (USA) Calgary, University (Canada)

Ground-based photometry and spectroscopy is presented for IRAS 22272 + 5435, a 9th mag star with a large infrared excess. The flux distribution is 'double-peaked', with a visible and near-infrared component due to the reddened photosphere and a far-infrared component presumably due to a detached dust shell. About equal amounts of energy are detected from each. The spectrum is that of a peculiar G supergiant, Gp Ia. In addition, strong molecular bands of C3 and C2 are observed. The flux distribution is modeled and, together with published molecular-line radio observations, allows the determination of basic parameters of the central star and the dust shell. The source has the characteristics one would expect of a proto-planetary nebula, an object in transition from the asymptotic giant branch to the planetary nebula phase. 31 refs.

• OSTI ID: 5597325
• Journal Information: Astrophysical Journal; (United States), Journal Name: Astrophysical Journal; (United States) Vol. 371; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CARBON
ELECTROMAGNETIC RADIATION
ELEMENTS
GIANT STARS
INFRARED RADIATION
NEBULAE
NONMETALS
PHOTOMETRY
PLANETARY NEBULAE
RADIATION FLUX
RADIATIONS
SPECTRA
SPECTROSCOPY
STAR EVOLUTION
STARS
STELLAR ATMOSPHERES
SUPERGIANT STARS