Differential asteroseismic study of seismic twins observed by CoRoT; Comparison of HD 175272 with HD 181420

TL;DR

This study develops a differential asteroseismic method to analyze noisy oscillation spectra by comparing a target star with a well-characterized reference star, enabling precise determination of stellar properties even with low-quality data.

Contribution

The paper introduces a novel differential approach using seismic twins to extract detailed stellar parameters from low-quality asteroseismic data, enhancing analysis capabilities.

Findings

Successfully characterized HD 175272 using a differential method.

Measured mass, radius, and age differences with HD 181420.

Applicable to stars with low signal-to-noise oscillation spectra.

Abstract

The CoRoT short asteroseismic runs give us the opportunity to observe a large variety of late-type stars through their solar-like oscillations. We report the observation and modeling of the F5V star HD 175272. Our aim is to define a method for extracting as much information as possible from a noisy oscillation spectrum. We followed a differential approach that consists of using a well-known star as a reference to characterize another star. We used classical tools such as the envelope autocorrelation function to derive the global seismic parameters of the star. We compared HD 175272 with HD 181420 through a linear approach, because they appear to be asteroseismic twins. The comparison with the reference star enables us to substantially enhance the scientific output for HD 175272. First, we determined its global characteristics through a detailed seismic analysis of HD 181420. Second, with our differential approach, we measured the difference of mass, radius and age between HD 175272 and HD 181420. We have developed a general method able to derive asteroseismic constraints on a star even in case of low-quality data. %This method is based on the comparison to a star with common seismic and classical properties. Seismic data allow accurate measurements of radii and masses differences between the two stars. This method can be applied to stars with interesting properties but low signal-to-noise ratio oscillation spectrum, such as stars hosting an exoplanet or members of a binary system.