J/A+A/704/A332 BAF-type main-sequence stars rotation velocities (Aerts, 2025)
Distributions and evolution of the equatorial rotation velocities of
2937 BAF-type main-sequence stars from asteroseismology.
A break in the specific angular momentum at M∼2.5M☉.
Aerts C.
<Astron. Astrophys. 704, A332 (2025)>
=2025A&A...704A.332A 2025A&A...704A.332A (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Stars, fundamental ; Rotational velocities ;
Stars, dwarfs ; Stars, F-type ; Stars, A-type ; Stars, B-type
Keywords: asteroseismology - stars: evolution - stars: interiors -
stars: magnetic field - stars: oscillations - stars: rotation
Abstract:
Studies of the rotational velocities of intermediate-mass
main-sequence stars are crucial to test stellar evolution theory. They
often rely on spectroscopic measurements of the projected rotation
velocities, Veq*sini. These not only suffer from the unknown
projection factor sini but tend to ignore additional line-profile
broadening mechanisms aside from rotation, such as pulsations and
turbulent motions near the stellar surface. This limits the accuracy
of Veq distributions derived from Veq*sini measurements. We use
asteroseismic measurements to investigate the distribution of the
equatorial rotation velocity Veq, its ratio with respect to the
critical rotation velocity, Veq/Vcrit, and the specific angular
momentum, J/M, for several thousands of BAF-type stars, covering a
mass range from 1.3M☉ to 8.8M☉ and almost the entire
core-hydrogen burning phase.
We rely on high-precision model-independent internal rotation
frequencies, as well as on masses and radii from asteroseismology to
deduce Veq, Veq/Vcrit, and J/M for 2937 gravity-mode pulsators in the
Milky Way. The sample stars have rotation frequencies between almost
zero and 33uHz, corresponding to rotation periods above 0.35d.
We find that intermediate-mass stars experience a break in their J/M
occurring {in the mass interval [2.3,2.7]M☉.} We establish
unimodal Veq and Veq/Vcrit distributions for the mass range
[1.3,2.5[M☉ while stars with M in [2.5,8.8]M☉ reveal some
structure in their distributions. We find {that the near-core rotation
slows down as stars evolve,} pointing to very efficient angular
momentum transport.
The kernel density estimators of the asteroseismic internal rotation
frequency, equatorial rotation velocity, and specific angular momentum
of this large sample of intermediate-mass field stars can conveniently
be used for population synthesis studies and to fine-tune the theory
of stellar rotation across the main sequence evolution.
Description:
The tables contain the near-core rotation frequency, mass, radius, and
evolutionary stage, as well as their errors, for 2937
intermediate-mass pulsators.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 115 490 Asteroseismic and stellar properties for F stars
table2.dat 115 2447 Asteroseismic and stellar properties for BAF stars
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See also:
J/A+A/684/A112 : Effect on rotation for red giant ages (Fritzewski+, 2024)
J/A+A/695/A214 : Near-core rotation of intermediate-mass stars (Aerts+, 2025)
Byte-by-byte Description of file: table1.dat table2.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 Mass mass estimate
52- 59 F8.5 Msun e_Mass lower error of mass estimate
60- 67 F8.5 Msun E_Mass upper error of mass estimate
68- 75 F8.5 Rsun Rad radius estimate
76- 83 F8.5 Rsun e_Rad lower error of radius estimate
84- 91 F8.5 Rsun E_Rad upper error of radius estimate
92- 99 F8.5 --- Xc/Xini central versus initial H mass fraction
as a proxy for evolutionary stage
100-107 F8.5 --- e_Xc/Xini lower error of Xc/Xini
108-115 F8.5 --- E_Xc/Xini upper error of Xc/Xini
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Acknowledgements:
Conny Aerts, conny.aerts(at)kuleuven.be
(End) Patricia Vannier [CDS] 03-Nov-2025