The problematically short superwind of OH/IR stars - Probing the outflow with the 69 {\mu}m spectral band of forsterite

TL;DR

This study uses the 69 μm spectral band of crystalline olivine to analyze the outflow properties of OH/IR stars, revealing that their superwinds are short-lived and compact, challenging current stellar evolution models.

Contribution

First application of Herschel/PACS to observe the 69 μm olivine band in OH/IR stars, linking spectral features to outflow timescales and superwind characteristics.

Findings

Superwinds are geometrically compact, starting less than 1200 years ago.

The 69 μm band indicates high crystalline olivine abundance.

Outflow models suggest a short-lived, recent superwind phase.

Abstract

Spectra of OH/IR stars show prominent spectral bands of crystalline olivine (Mg$_{(2-2x)}$Fe$_{(2x)}$SiO$_{4}$). To learn more about the timescale of the outflows of OH/IR stars, we study the spectral band of crystalline olivine at 69 {\mu}m. The 69 {\mu}m band is of interest because its width and peak wavelength position are sensitive to the grain temperature and to the exact composition of the crystalline olivine. With Herschel/PACS, we observed the 69 {\mu}m band in the outflow of 14 OH/IR stars. By comparing the crystalline olivine features of our sample with those of model spectra, we determined the size of the outflow and its crystalline olivine abundance. The temperature indicated by the observed 69 {\mu}m bands can only be reproduced by models with a geometrically compact superwind ($R_{\rm{SW}}\lesssim$ 2500 AU = 1400 R$_{*}$).This means that the superwind started less than 1200 years ago (assuming an outflow velocity of 10 km/s). The small amount of mass lost in one superwind and the high progenitor mass of the OH/IR stars introduce a mass loss and thus evolutionary problem for these objects, which has not yet been understood.