Geometry and physical conditions in the stellar wind of AG Carinae

Details Geometry and physical conditions in the stellar wind of AG Carinae Geometry and physical conditions in the stellar wind of AG Carinae

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...428..292l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 428, no. 1, p. 292-318

Astronomy and Astrophysics

Astronomy

74

Asphericity, Giant Stars, Mass Flow Rate, Stellar Envelopes, Stellar Evolution, Stellar Winds, Ultraviolet Astronomy, Wind Variations, Abundance, Helium, Photometry, Polarimeters, Spectroscopy, Stellar Models

Scientific paper

AG Carinae is one of the prototypes of the class of Luminous Blue Variables (LBVs). Since 1990 the star has continuously brightened in its visual continuum. We report on a multi-instrument and -wavelength observing campaign to monitor the current activity phase of AG Car. Ground-based photometry, polarimetry, spectroscopy, and space-ultraviolet spectroscopy and spectropolarimetry have been obtained. From the variability of the polarization at ultraviolet and optical wavelengths we detect significant intrinsic polarization. Pint greater than or equal to 0.5% is a large value for a hot, luminous star, suggesting departure from spherical symmetry in the wind of AG Car. The intrinsic polarization is variable on a timescale of 2 months or less. The measured ultraviolet polarization (intrinsic + interstellar) dropped to 0.5% in 1992 May and returned to 1% in 1992 July. The results are interpreted in terms of a variable outflow with a density enhancement in the equatorial plane. A similar model was suggested for the related object R127 in the Large Magellanic Cloud (LMC). This geometry is reminiscent of the large-scale morphology of the gas nebula and dust 'jet' surrounding AG Car. It is therefore likely that physical conditions close to the stellar surface are responsible for the geometry of the spatially resolved circumstellar material around AG Car. Despite the drastic change of the photospheric conditions, the mass-loss rate did not increase. We find no evidence for a positive correlation between wind density and stellar radius. This makes models that explain the radius increase by opacity effects in the outflow unlikely. The mechanism responsible for the temperature and radius variations is still unknown but most likely has its origin in subphotospheric regions.

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