Very regular high-frequency pulsation modes in young intermediate-mass stars
Abstract
Asteroseismology is a powerful tool for probing the internal structures of stars by using their natural pulsation frequencies. It relies on identifying sequences of pulsation modes that can be compared with theoretical models, which has been done successfully for many classes of pulsators, including low-mass solar-type stars, red giants, high-mass stars and white dwarfs. However, a large group of pulsating stars of intermediate mass--the so-called delta Scuti stars--have rich pulsation spectra for which systematic mode identification has not hitherto been possible. This arises because only a seemingly random subset of possible modes are excited, and because rapid rotation tends to spoil the regular patterns. Here we report the detection of remarkably regular sequences of high-frequency pulsation modes in 60 intermediate-mass main-sequence stars, allowing definitive mode identification. Some of these stars have space motions that indicate they are members of known associations of young stars, and modelling of their pulsation spectra confirms that these stars are indeed young.
Cite
@article{arxiv.2005.06157,
title = {Very regular high-frequency pulsation modes in young intermediate-mass stars},
author = {Timothy R. Bedding and Simon J. Murphy and Daniel R. Hey and Daniel Huber and Tanda Li and Barry Smalley and Dennis Stello and Timothy R. White and Warrick H. Ball and William J. Chaplin and Isabel L. Colman and Jim Fuller and Eric Gaidos and Daniel R. Harbeck and J. J. Hermes and Daniel L. Holdsworth and Gang Li and Yaguang Li and Andrew W. Mann and Daniel R. Reese and Sanjay Sekaran and Jie Yu and Victoria Antoci and Christoph Bergmann and Timothy M. Brown and Andrew W. Howard and Michael J. Ireland and Howard Isaacson and Jon M. Jenkins and Hans Kjeldsen and Curtis McCully and Markus Rabus and Adam D. Rains and George R. Ricker and Christopher G. Tinney and Roland K. Vanderspek},
journal= {arXiv preprint arXiv:2005.06157},
year = {2020}
}
Comments
published in Nature https://www.nature.com/articles/s41586-020-2226-8