Water vapour masers in long-period variable stars II. The semi-regular variables R Crt and RT Vir

TL;DR

This study presents a long-term monitoring of water vapor masers in semi-regular variable stars R Crt and RT Vir, revealing short-term feature variability, long-term brightness changes, and an exceptional constant velocity feature indicating a stable maser cloud in the outer shell.

Contribution

It provides the first detailed analysis of maser feature longevity and dynamics in semi-regular variables over multiple decades, including a rare stable velocity feature.

Findings

Short-term maser feature variations occur on months to 1.5-year timescales.

Long-term brightness levels vary independently of optical lightcurves.

A stable maser feature in RT Vir suggests a cloud in the outer shell moving at terminal velocity.

Abstract

Within the 'Medicina/Effelsberg H2O maser monitoring program' we have observed the maser emission of R Crt and RT Vir for more than two decades. To get insight in the distribution and longevity of maser spots in the circumstellar envelopes, we have collected interferometric data, taken in the same period, from the literature. We confirm short-time variations of individual maser features on timescales of months to up to 1.5 years. Also decade-long variations of the general brightness level independent from individual features were seen in both stars. These are due to brightness variations occurring independently from each other in selected velocity ranges, and are independent of the optical lightcurves. Expected drifts in velocity of individual features are usually masked by blending. However, in RT Vir we found an exceptional case of a feature with a constant velocity over 7.5 years (<0.06 km/s/yr). We attribute the long-term brightness variations to the presence of regions with higher-than-average density in the stellar wind, which host several clouds which emit maser radiation on the short time scales. These regions typically need ~20 years to cross the H2O maser shell, where the right conditions to excite H2O masers are present. The constant velocity feature (11 km/s) is likely to come from a single maser cloud, which moved through about half of RT Vir's H2O maser shell without changing velocity. From this we infer that its path was located in the outer part of the H2O maser shell, where RT Vir's stellar wind apparently has already reached its terminal outflow velocity. This conclusion is corroborated by the observation that the highest H2O maser outflow velocity in RT Vir approaches the terminal outflow velocity as given by OH and CO observations. This is generally not observed in other semi-regular variable stars.