J/A+A/695/A214 Near-core rotation of intermediate-mass stars (Aerts+, 2025)
Evolution of the near-core rotation frequency of 2497 intermediate-mass stars
from their dominant gravito-inertial mode.
Aerts C., Van Reeth T., Mombarg J.S.G., Hey D.
<Astron. Astrophys. 695, A214 (2025)>
=2025A&A...695A.214A 2025A&A...695A.214A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, fundamental; Rotational velocities; Stars, dwarfs;
Stars, F-type; Stars, A-type; Stars, B-type
Keywords: asteroseismology - waves - stars: evolution - stars: interiors -
stars: oscillations - stars: rotation
Abstract:
The sparsely sampled time-series photometry from Gaia Data Release 3
(DR3) led to the discovery of more than 100000 main-sequence
non-radial pulsators. The majority of these were further scrutinised
by uninterrupted high-cadence space photometry assembled by the
Transiting Exoplanet Survey Satellite (TESS).
We combine Gaia DR3 and TESS photometric light curves to estimate the
internal physical properties of 2497 gravity-mode pulsators. We
perform asteroseismic analyses with two major aims: 1) to measure the
near-core rotation frequency and its evolution during the main
sequence and 2) to estimate the mass, radius, evolutionary stage, and
convective core mass from stellar modelling.
We rely on asteroseismic properties of Kepler γ Doradus and
Slowly Pulsating B stars to derive the cyclic near-core rotation
frequency, frot, of the Gaia-discovered pulsators from their
dominant prograde dipole gravito-inertial pulsation mode. Further, we
investigate the impact of adding frot as extra asteroseismic
observable aside from the luminosity and effective temperature on the
outcome of grid-based modelling from rotating stellar models.
We offer a recipe based on linear regression to deduce frot from the
dominant gravito-inertial mode frequency, which we show to be
applicable to prograde dipole modes in the sub-inertial regime, having
an amplitude above 4mmag. By applying it to 2497 pulsators with such
a mode, we increase the sample of intermediate-mass dwarfs with such
an asteroseismic observable by a factor of 4. We use the estimate of
frot to deduce spin parameters between 2 and 6, while the sample's
near-core rotation rates range from 0.7% to 25% of the critical
Keplerian rate. We use frot, along with the Gaia effective
temperature and luminosity to deduce the (convective core) mass,
radius, and evolutionary stage from grid modelling based on rotating
stellar models. We derive a decline of frot with a factor of two
during the main-sequence evolution for this population of field stars,
which covers a mass range from 1.3M☉ to 7M_{sun. We find
observational evidence for an increase in the radial order of excited
gravity modes as the stars evolve. For 307 pulsators, we derive an
upper limit of the radial differential rotation between the convective
core boundary and the surface from Gaia's vbroad measurement and find
values up to 5.4.
Our recipe to deduce the near-core rotation frequency from the
dominant prograde dipole gravito-inertial mode detected in the
independent Gaia and TESS light curves is easy to use and facilitates
applications to large samples of pulsators, mapping their angular
momentum and evolutionary stage in the Milky Way.
Description:
The tables contain the near-core rotation and dominant oscillation
frequencies, as well as asteroseismically inferred stellar properties
from grid modelling for 2497 Gaia-discovered TESS-confirmed
intermediate-mass stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 171 2464 Asteroseismic and stellar properties for Z=0.0140
tableb2.dat 171 2439 Asteroseismic and stellar properties for Z=0.0080
tableb3.dat 171 2375 Asteroseismic and stellar properties for Z=0.0045
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
Byte-by-byte Description of file: tableb1.dat tableb2.dat tableb3.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaDR3 Gaia DR3 identification number
20- 27 F8.5 d-1 frot Cyclic near-core rotation frequency
28- 35 F8.5 d-1 e_frot Lower error of frot
36- 43 F8.5 d-1 E_frot Upper error of frot
44- 51 F8.5 Msun Mstar Mass estimate
52- 59 F8.5 Msun e_Mstar Lower error of mass estimate
60- 67 F8.5 Msun E_Mstar Upper error of mass estimate
68- 75 F8.5 --- Xc/Xini Central versus initial H mass fraction
as a proxy for evolutionary stage
76- 83 F8.5 --- e_Xc/Xini Lower error of Xc/Xini
84- 91 F8.5 --- E_Xc/Xini Upper error of Xc/Xini
92- 99 F8.5 Msun Mcc Convective core mass estimate
100-107 F8.5 Msun e_Mcc Lower error of Mcc
108-115 F8.5 Msun E_Mcc Upper error of Mcc
116-123 F8.5 [Rsun] log(Rstar) Logarithm of stellar radius
124-131 F8.5 [Rsun] e_log(Rstar) Lower error for radius (expressed in
log space wrt solar radius)
132-139 F8.5 [Rsun] E_log(Rstar) Upper error for radius (expressed in
log space wrt solar radius)
140-147 F8.5 d-1 fco-rot Mode frequency in co-rotating frame
148-155 F8.5 --- Spin Spin, 2frot/fco-rot
156-163 F8.5 d-1 fsurfsini Projected surface rotation frequency
164-171 F8.5 --- frot/fsurfsini ?=- Upper limit for the near-core to
surface rotation limit
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Acknowledgements:
Conny Aerts, conny.aerts(at)kuleuven.be
(End) Patricia Vannier [CDS] 25-Feb-2025