Abstract
Since the advent of CoRoT, and NASA Kepler and K2, the number of low- and intermediate-mass stars classified as pulsators has increased very rapidly with time, now accounting for several $10^4$ targets. With the recent launch of NASA TESS space mission, we have confirmed our entrance to the era of all-sky observations of oscillating stars. TESS is currently releasing good quality datasets that already allow for the characterization and identification of individual oscillation modes even from single 27-days shots on some stars. When ESA PLATO will become operative by the next decade, we will face the observation of several more hundred thousands stars where identifying individual oscillation modes will be possible. However, estimating the individual frequency, amplitude, and lifetime of the oscillation modes is not an easy task. This is because solar-like oscillations and especially their evolved version, the red giant branch (RGB) oscillations, can vary significantly from one star to another depending on its specific stage of the evolution, mass, effective temperature, metallicity, as well as on its level of rotation and magnetism. In this perspective I will present a novel, fast, and powerful way to derive individual oscillation mode frequencies by building on previous results obtained with \diamonds. I will show that the oscillation frequencies obtained with this new approach can reach precisions of about 0.1 % and accuracies of about 0.01 % when compared to published literature values for the RGB star KIC~12008916.
Highlights
Despite both CoRoT (Baglin et al, 2006) and NASA Kepler and K2 missions (Borucki et al, 2010; Koch et al, 2010; Howell et al, 2014) have ended, we keep gathering new datasets of oscillating stars from recently launched NASA TESS (Ricker et al, 2014), which is offering the opportunity to extract individual oscillation mode frequencies even with 27-days long observations
This implies that these frequencies could be used for modeling purposes, precisions do not reach the level of those extracted from a peak bagging analysis using Approach 1, which ranges from 10−2 to 10−3 % for the range of frequencies used in this work, as obtained by C15
This new Approach 2 has two important advantages: (1) it is extremely convenient in terms of computational speed, yielding a factor of about 100 improvement with respect to Approach 1; (2) it does not require any assumption on the location of the frequency peaks, but only a simple average estimate of the oscillation amplitude in a chunk and an estimate of a minimum linewidth for each star, making it an adequate approach for the complex oscillation patterns found in evolved stars
Summary
Despite both CoRoT (Baglin et al, 2006) and NASA Kepler and K2 missions (Borucki et al, 2010; Koch et al, 2010; Howell et al, 2014) have ended, we keep gathering new datasets of oscillating stars from recently launched NASA TESS (Ricker et al, 2014), which is offering the opportunity to extract individual oscillation mode frequencies even with 27-days long observations (see e.g., Huber et al, 2019). My view on the problem is that we require a simple approach that can be at the same time powerful, flexible to be adapted to different conditions, and fast in performing a peak bagging analysis for each star. This approach should be accessible by the global asteroseismic community. For this purpose, I present a novel methodology, based on the public code DIAMONDS (Corsaro and De Ridder, 2014, hereafter C14), to extract individual oscillation mode frequencies that is at the same time fast, easy to use, and accurate. For demonstrating its working principle and performance, I apply it to the RGB star KIC 12008916, for which a detailed peak bagging analysis is available (Corsaro et al, 2015a, hereafter C15)
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
