Ultraviolet and visible spectropolarimetric variability in P Cygni

TL;DR

This study uses ultraviolet and visible spectropolarimetry to analyze wind clumps in P Cygni, revealing their properties, locations, and potential relation to other wind features, advancing understanding of stellar wind structures.

Contribution

It provides new multi-wavelength spectropolarimetric data and estimates the physical properties and locations of wind clumps in P Cygni, linking polarization features to wind inhomogeneities.

Findings

Clumps are detectable near the wind base at r/R* = 1.3 - 2.5.

Clump density is at least 10^13 cm^-3, about 20 times the mean wind.

Clumps have an electron optical depth of 0.1 - 1 and account for up to 2% of wind mass loss.

Abstract

We report on new data, including four vacuum ultraviolet spectropolarimetric observations by the Wisconsin Ultraviolet Photo-Polarimeter Experiment ("WUPPE") on the Astro-1 (one observation) and Astro-2 (three observations) shuttle missions, and 15 new visible-wavelength observations obtained by the HPOL CCD spectropolarimeter at the Pine Bluff Observatory of the University of Wisconsin. This includes three HPOL observations made within 12 hours of each of the three Astro-2 WUPPE observations, giving essentially simultaneous observations extending from 1500 to 10500 Angstroms. An analysis of these data yields estimates on the properties of wind "clumps" when they are detectable by the polarization of their scattered light. We find that the clumps must be detected near the base of the wind, r/R* = 1.3 - 2.5. At this time the clump density is at least 10^13 cm^-3, 20 times the mean wind, and the temperature is roughly 10,000 K, about 20% cooler than the mean wind. The clumps leading to the largest observed polarization must have electron optical depth of 0.1 - 1 and an angular extent of 0.1 - 1 ster, and account for at most 2% of the wind mass loss. The H and HeI emission lines from the wind are unpolarized, but their P Cygni absorption is enhanced by a factor of 4 in the scattered light. We speculate on the possible relationship of the clumps detected polarimetrically to those seen as Discrete Absorption Features (DACs) and in interferometry.