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Title: Core-Envelope Coupling in Intermediate-Mass Core-Helium Burning Stars

Authors: Jamie Tayar et al.

First Author’s Institution: Institute for Astronomy, University of Hawaii

Status: Accepted to ApJ

Disclaimer: The author of this astrobite currently works with the first author of today’s paper, but was not involved in the presented work.

All stars in nature rotate, including our own. However, stellar rotation over a star’s lifetime remains poorly understood. This has a profound impact on the accuracy of stellar models, which are our primary source for understanding the interiors and evolution of stars.

Today’s paper focuses on internal rotation mechanisms; specifically, how a star’s core rotates with respect to its surface. Understanding stellar core rotation can teach us a ton about internal stellar physics and long-term angular momentum transport within a star’s interior.

A Problem of (Astero)Seismic Proportions

Like many outstanding problems in astronomy, this problem can be solved by obtaining more data. How do we get more data on the internal core rotation rates of stars? Through asteroseismology! By studying stellar pulsations, we can infer information about a star’s interior.

The authors of today’s paper focused on evolved intermediate-mass stars, or stars between two and eight times the mass of the Sun. These stars fall in the transition region between low- and high-mass stars, as their name implies. Like their more massive counterparts, these stars have a convective core and rotate rapidly during the main sequence — the phase of evolution where stars burn hydrogen into helium. However, like low-mass stars, intermediate-mass stars become cool red giants as they evolve. It turns out red giant stars also pulsate like the Sun, a low-mass star. By comparing how red giant stars oscillate to how the Sun oscillates, we can measure stellar parameters for red giants, such as their mass and radius.

The Core Tells All

We can additionally infer core rotation periods for red giant stars using asteroseismology, making them the perfect candidates for this study. In red giant stars, waves that propagate near the stellar core interfere with waves that propagate on the surface. By measuring surface pulsations, we can determine how the core and surface waves interact. From there, we can infer details about the stellar core, such as rotation.

After measuring the core rotation periods for the stars in this sample via asteroseismology using data from the Kepler Space Telescope , the authors compared their rotation periods with several other stellar parameters and analyzed how stars with these measured core rotation periods should evolve over time. Figure 1 shows a correlation between measured core rotation periods and surface gravity, which decreases as stars of the same mass evolve. This trend with surface gravity indicates that as these stars evolve, their cores rotate more slowly. The authors also compared their measured core rotation periods with stellar mass and metallicity but found no obvious trends.

Several of the stars in the sample also had surface rotation periods measured by a previous study. This comparison is shown in the left panel of Figure 2. This comparison suggests that as stars decrease in surface gravity (evolve), the ratio between their core rotation period and measured surface rotation period gets closer to 1 (i.e. the surface and core rotation periods become more similar as a star evolves), indicating that the stellar core can become recoupled with the surface as time goes on. The authors, however, exercise caution with such a result. When they predict surface rotation periods with stellar models, that obvious trend disappears (right panel of Figure 2) which shows that there may be a bias when selecting stars with measured surface rotation periods.

Evolving Stellar Astronomy

The results of this study have several implications for our understanding of stellar evolution. The evolution of core rotation periods over time suggests angular momentum transport occurs between the core of the star and the surrounding envelope. The comparison with surface rotation periods also shows some evidence for core-surface recoupling as these stars evolve. This study provides insight into internal stellar rotation that can be used to improve current stellar models and provides a new jumping off point for future work.