OH/IR stars and their superwinds as observed by the Herschel Space Observatory

TL;DR

This study uses Herschel and ground-based CO observations to analyze the mass loss history of extreme OH/IR stars, revealing recent superwind phases and evidence of hot-bottom burning in massive AGB stars.

Contribution

It provides detailed modeling of circumstellar envelopes and mass loss rates, highlighting the recent superwind phase and nuclear processing evidence in these stars.

Findings

Stars entered superwind phase 200-500 years ago

Low isotopic ratios indicate hot-bottom burning

Massive AGB stars with M >= 5 solar masses

Abstract

Aim : In order to study the history of mass loss in extreme OH/IR stars, we observed a number of these objects using CO as a tracer of the density and temperature structure of their circumstellar envelopes. Method : Combining CO observations from the Herschel Space Observatory with those from the ground, we trace mass loss rates as a function of radius in five extreme OH/IR stars. Using radiative transfer modelling, we modelled the dusty envelope as well as the CO emission. The high-rotational transitions of CO indicate that they originate in a dense superwind region close to the star while the lower transitions tend to come from a more tenuous outer wind which is a result of the mass loss since the early AGB phase. Result : The models of the circumstellar envelopes around these stars suggest that they have entered a superwind phase in the past 200 - 500 years. The low 18O/17O (~ 0.1 compared to the solar abundance ratio of ~ 5) and 12C/13C (3-30 cf. the solar value of 89) ratios derived from our study support the idea that these objects have undergone hot-bottom burning and hence that they are massive M >= 5 solar-mass AGB stars.