Fast winds in central stars of some planetary nebulae

Journal Article · Sun Oct 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167908· OSTI ID:5096438

Cerruti-Sola, M; Perinotto, M ^[1]

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1. Arcetri, Osservatorio Astrofisico, Florence (Italy) Firenze Universita, Florence (Italy)

Winds from the central stars of the planetary nebulae NGC 1535, NGC 6210, NGC 7009, IC 418, and IC 4593 have been investigated with high-resolution IUE spectra. All these stars present P Cygni profiles in some of the following lines: N V 1240, O IV 1342, O V 1371, Si IV 1397, C IV 1549, and N IV 1719 A. These profiles have been analyzed with the SEI method developed by Lamers et al. (1987). The mass-loss rates of the winds are found to be 1.4 x 10 to the -9th, 2.2 x 10 to the -9th, 2.8 x 10 to the -9th, 6.3 x 10 to the -9th, and 4.2 x 10 to the -8th solar mass/yr for the above stars, respectively. Despite all efforts made in order to reach the maximum accuracy, the uncertainty of these determinations remains in some cases quite large. Nevertheless, it is possible to show that the mechanism producing the winds is likely to be the radiation pressure. 35 refs.

• OSTI ID: 5096438
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 345; 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
ABUNDANCE
DWARF STARS
MASS
MASS TRANSFER
NEBULAE
PLANETARY NEBULAE
RADIATION PRESSURE
SPECTRA
STARS
STELLAR ACTIVITY
STELLAR WINDS
ULTRAVIOLET SPECTRA
WHITE DWARF STARS