The K giant star Arcturus: the hybrid nature of its infrared spectrum

TL;DR

This study investigates the complex infrared spectrum of Arcturus, revealing hybrid atmospheric components and suggesting the presence of molecular clouds in cool giant stars, challenging classical stellar atmosphere models.

Contribution

It uncovers the hybrid nature of CO line formation in Arcturus and proposes molecular clouds as a common feature in cool luminous stars, supported by spectral analysis.

Findings

CO lines exhibit an abrupt change at logW/nu = -4.75.

Strong CO lines are enhanced, weaker lines are weakened, indicating extended atmospheric effects.

Evidence suggests molecular clouds exist in the atmospheres of cool giant stars.

Abstract

We study infrared spectrum of Arcturus to clarify the nature of the cool component of its atmosphere, referred to as the CO-mosphere, with the use of the IR spectral atlas by Hinkle et al.(1995). The nature of CO lines shows an abrupt change at logW/nu = -4.75, and the lines stronger than this limit can no longer be analyzed by the classical line-formation theory. A more simple manifestation of this fact is that the curves-of-growth (CG) of CO lines show an unpredictable upturn at logW/nu = -4.75. Similar unusual behaviors of empirical CG are confirmed in other red (super)giant stars, and it looks as if the CG is a hybrid of at least two components of different origins. Although strong lines of the CO fundamentals observed in Arcturus show strengthening compared with the predicted photospheric spectrum, the weaker lines show slight weakening, and we interpret these results as due to absorption/emission by the molecular clouds formed in the extended atmosphere. Now do clouds exist in stellar atmospheres? It is by no means easy to answer this question by spectroscopic observations alone, but we find several arguments in favor of such a possibility in Arcturus by analyzing the CO lines. In cooler (super)giant stars in which CO lines show similar unusual behaviors as in Arcturus, the presence of molecular clouds in the outer atmospheres was demonstrated by direct observations with spatial interferometry. We suggest that the formation of molecular clouds is a general feature in cool luminous stars from early K to late M (super)giant stars.