New activity in the large circumstellar disk of the Be-shell star 48 Lib

TL;DR

This study documents the long-term evolution of the circumstellar disk in Be-star 48 Lib through multi-technique observations, revealing disk asymmetry recovery, size, and structure changes over 16 years.

Contribution

It provides a comprehensive, multi-method analysis of disk activity and asymmetry evolution in 48 Lib, highlighting new insights into disk dynamics and structure.

Findings

Disk asymmetries vanished in the late 1990s and recovered between 2004-2007.

Disk diameter is approximately 15 stellar radii with a position angle of 50 degrees.

Interferometric data suggest a large, multi-component disk structure.

Abstract

Spectroscopic, polarimetric, and high spectral resolution interferometric data covering the period 1995-2011 are analyzed to document the transition into a new phase of circumstellar disk activity in the classical Be-shell star 48 Lib. The long-term disk evolution is described using the V/R ratio of the violet and red emission components of H alpha and Br gamma, radial velocities and profiles of He I and optical metal shell lines, multi-band BVRI polarimetry, broad-band and high-resolution interferometric visibilities and phases. Spectroscopic signatures of disk asymmetries in 48 Lib vanished in the late nineties but recovered some time between 2004 and 2007. Variations in the radial velocity and line profile of conventional shell lines correlate with the V/R behavior. They are shared by narrow absorption cores superimposed on otherwise seemingly photospheric He I lines, which may form in high-density gas at the inner disk close to the photosphere. Large radial velocity variations continued also during the V/R-quiet years. The broad H-band interferometry gives a disk diameter of (1.72+-0.2) mas (equivalent to 15 stellar radii), position angle of the disk (50+-9) deg and a relatively low disk flattening of 1.66+-0.3. Within the errors the same disk position angle is derived from polarimetric observations and from photocenter shifts across Br gamma. The high-resolution interferometric visibility and phase profiles show a double or even multiple-component structure. A preliminary estimate based on the size of the Br gamma emitting region indicates a large diameter for the disk (tens of stellar radii).