The density structure of the wind of P Cygni (B1 Ia+)

Details The density structure of the wind of P Cygni (B1 Ia+) The density structure of the wind of P Cygni (B1 Ia+)

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...155..104w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 155, no. 1, Jan. 1986, p. 104-112.

Astronomy and Astrophysics

Astronomy

40

Early Stars, Infrared Astronomy Satellite, Stellar Atmospheres, Stellar Mass Ejection, Stellar Winds, Supergiant Stars, Balmer Series, Cosmic Dust, Cygnus Constellation, Gas Density, Infrared Radiation

Scientific paper

Near-IR and IRAS observations of the hypergiant P Cygni (B1 Ia+) are used to derive the density structure of the wind of P Cygni. The authors find a linear velocity law that is identical to the one derived by Van Blerkom (1978) from an analysis of Balmer line profiles, and differs from the one derived by Barlow and Cohen (1977) based on their analysis of near-IR and radio data. Two models can explain the observed excess at 60 μ: a shell extending from 15 to 50 stellar radii with a density increase of a factor five relative to the quiescent wind, or cold dust with a typical temperature of 30K, situated far away from the star. The dust model can also explain the 100 μ flux if that flux can be attributed to the star and is not a part of the complicated background.

Affiliated with

Also associated with

No associations

Rating

The density structure of the wind of P Cygni (B1 Ia+) does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The density structure of the wind of P Cygni (B1 Ia+), we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The density structure of the wind of P Cygni (B1 Ia+) will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1843809