# Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE - Constellation

## TL;DR

This study uses photometric data from BRITE to measure granulation and oscillation time scales in 23 bright red giants, enabling improved estimates of their surface gravities and masses through calibrated seismic scaling relations.

## Contribution

It introduces a method to calibrate seismic scaling relations for bright red giants using Kepler data, and applies probabilistic analysis to extract stellar parameters from BRITE observations.

## Key findings

- Detected granulation and oscillation signals in all 23 stars.
- Calibrated seismic scaling relations for granulation components.
- Derived stellar surface gravities and masses consistent with literature.

## Abstract

Context: The study of stellar structure and evolution depends crucially on accurate stellar parameters. The photometry from space telescopes has provided superb data that allowed asteroseismic characterisation of thousands of stars. However, typical targets of space telescopes are rather faint and complementary measurements are difficult to obtain. On the other hand, the brightest, otherwise well-studied stars, are lacking seismic characterization. Aims: Our goal is to use the granulation and/or oscillation time scales measured from photometric time series of bright red giants (1.6$\leq$Vmag$\leq$5.3) observed with BRITE to determine stellar surface gravities and masses. Methods: We use probabilistic methods to characterize the granulation and/or oscillation signal in the power density spectra and the autocorrelation function of the BRITE time series. Results: We detect a clear granulation and/or oscillation signal in 23 red giant stars and extract the corresponding time scales from the power density spectra as well as the autocorrelation function of the BRITE time series. To account for the recently discovered non-linearity of the classical seismic scaling relations, we use parameters from a large sample of Kepler stars to re-calibrate the scalings of the high- and low-frequency components of the granulation signal. We develop a method to identify which component is measured if only one granulation component is statistically significant in the data. We then use the new scalings to determine the surface gravity of our sample stars, finding them to be consistent with those determined from the autocorrelation signal of the time series. We further use radius estimates from the literature to determine the stellar masses of our sample stars from the measured surface gravities. We also define a statistical measure for the evolutionary stage of the stars.