# The envelope of the semiregular variable V CVn

## TL;DR

This study investigates the polarimetric variability of the semiregular star V CVn, revealing an asymmetric nebula and phase-shifted brightness changes, providing insights into its complex circumstellar environment.

## Contribution

First detailed polarimetric imaging of V CVn revealing an asymmetric nebula and its relation to stellar pulsation.

## Key findings

- Detected an asymmetric reflection nebula around V CVn.
- Observed brightness variations of nebula components with the star's pulsation period.
- Identified phase shifts in nebula brightness changes.

## Abstract

V CVn is a semiregular variable star with a V-band amplitude of $\approx2$ mag. This star has an unusually high amplitude of polarimetric variability: up to 6 per cent. It also exhibits a prominent inverse correlation between the flux and the fraction of polarization and a substantial constancy of the angle of polarization. To figure out the nature of these features, we observed the object using the Differential Speckle Polarimetry at three bands centered on 550, 625 and 880 nm using the 2.5-m telescope of Sternberg Astronomical Institute. The observations were conducted on 20 dates distributed over three cycles of pulsation. We detected an asymmetric reflection nebula consisting of three regions and surrounding the star at the typical distance of 35 mas. The components of the nebula change their brightness with the same period as the star, but with significant and different phase shifts. We discuss several hypotheses that could explain this behavior.