J/A+A/684/A112 Effect on rotation for red giant ages (Fritzewski+, 2024)
Age uncertainties of red giants due to cumulative rotational mixing of
progenitors calibrated by asteroseismology.
Fritzewski D.J., Aerts C., Mombarg J.S.G., Gossage S., Van Reeth T.
<Astron. Astrophys. 684, A112 (2024)>
=2024A&A...684A.112F 2024A&A...684A.112F (SIMBAD/NED BibCode)
ADC_Keywords: Stars, ages; Stars, fundamental; Rotational velocities;
Models, evolutionary
Keywords: asteroseismology - stars: evolution - stars: fundamental parameters -
stars: interiors - stars: oscillations - stars: rotation
Abstract:
Galactic archaeology largely relies on precise ages of distant evolved
stars in the Milky Way. Nowadays, asteroseismology can deliver ages
for many red giants observed with high-cadence, high-precision
photometric space missions such as CoRoT, Kepler, K2, TESS, and soon
PLATO.
Our aim is to quantify the age uncertainties of currently slowly
rotating red giants due to the cumulative effect of their fast
rotation during core-hydrogen burning: their rotation in earlier
evolutionary phases caused mixing of elements, resulting in heavier
helium cores and the prolongation of their main-sequence lifetime.
These rotational effects are usually ignored when age-dating red
giants, despite our knowledge of fast rotation for stars with
M≥1.3M☉.
We used a sample of 490 F-type gravito-inertial pulsators (gamma
Doradus stars) with precise asteroseismic estimates of their internal
rotation rate from Kepler asteroseismology and with luminosity
estimates from Gaia. For this sample, which includes stars rotating
from nearly zero to about 60% of the critical rate, we computed the
cumulative effect on the age in their post-main-sequence evolution
caused by rotational mixing on the main sequence. We used stellar
model grids with different physical prescriptions that mimic
rotational mixing to assess systematic uncertainties on the age.
With respect to non-rotating models, the sample of 490 gamma Doradus
stars, as red giant progenitors, reveals age differences up to 5% by
the time they start hydrogen-shell burning when relying on the theory
of rotationally induced diffusive mixing as included in the MIST
isochrones. Using rotational mixing based on an advective-diffusive
approach that includes meridional circulation leads to an age shift of
20% by the time of the tip of the red giant branch.
The age-dating of red giants is affected by the cumulative effect of
rotational mixing during the main sequence. Such rotationally induced
age shifts should be taken into account in addition to other effects
if the aim is to perform Galactic archaeological studies at the
highest precision.
Description:
The table holds the input parameters for the asteroseismic
grid-modelling and the asteroseismicly inferred stellar properties
for all 490 considered stars in the sample of Li et al.
(2020MNRAS.491.3586L 2020MNRAS.491.3586L, Cat. J/MNRAS/491/3586). Further, it contains the
age inferred from both the non-rotating and rotating MIST tracks at
four post- main sequence evolution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 231 490 Asteroseismic and stellar properties
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/MNRAS/491/3586 : 611 γ Doradus stars Kepler data (Li+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC Kepler Input Catalog ID (KIC)
10- 18 F9.5 deg RAdeg Right ascension from Gaia DR3 (ICRS)
at Ep=2016.0 (Cat. I/355) (RA)
20- 27 F8.5 deg DEdeg Declination from Gaia DR3 (ICRS)
at Ep=2016.0 (Cat. I/355) (DEC)
29- 33 F5.2 Lsun Lum Photometric luminosity (Lum)
35- 38 F4.2 Lsun e_Lum Uncertainty of photometric luminosity
(err_Lum)
40- 43 I4 K Teff Effective temperature from Gaia DR3
(Cat. I/355) (Teff)
45- 48 I4 K e_Teff Uncertainty of Teff (err_Teff)
50- 53 I4 s Pi0 Buoyancy travel time (Pi0) (1)
55- 58 I4 s e_Pi0 Lower uncertainty of Pi0 (errl_Pi0) (1)
60- 63 I4 s E_Pi0 Upper uncertainty of Pi0 (erru_Pi0) (1)
65- 72 F8.6 d-1 frot Near-core rotation rate (frot) (1)
74- 81 F8.6 d-1 e_frot Lower uncertainty of frot (errl_frot) (1)
83- 90 F8.6 d-1 E_frot Upper uncertainty of frot (erru_frot) (1)
92- 95 F4.2 --- Xc' Normalised core hydrogen mass fraction
(Xc')
97-100 F4.2 --- e_Xc' Lower uncertainty of Xc' (errl_Xc')
102-105 F4.2 --- E_Xc' Upper uncertainty of Xc' (erru_Xc')
107-111 F5.3 Gyr Age Asteroseismic age (age)
113-117 F5.3 Gyr e_Age Lower uncertainty of age (errl_age)
119-124 F6.3 Gyr E_Age Upper uncertainty of age (erru_age)
126-129 F4.2 Msun Mass Asteroseismic mass (mass)
131-134 F4.2 Msun e_Mass Lower uncertainty of mass (errl_mass)
136-139 F4.2 Msun E_Mass Upper uncertainty of mass (erru_mass)
141-144 F4.2 Rsun Rad Asteroseismic radius (radius)
146-149 F4.2 Rsun e_Rad Lower uncertainty of radius (errl_radius)
151-154 F4.2 Rsun E_Rad Upper uncertainty of radius (erru_radius)
156-159 F4.2 --- vvcrit Ratio of current rotation rate to
critical rotation rate (vvcrit)
161-165 F5.3 Gyr M-age-TAMS Age of rotating MIST track at TAMS
(MISTageTAMS)
167-171 F5.3 Gyr NR-M-age-TAMS Age non-rot. MIST track at TAMS
(NRMISTage_TAMS)
173-177 F5.3 --- TAMS-frac Fraction of rotating to non-rotating age
at TAMS (TAMS_frac)
179-183 F5.3 Gyr M-age-TRGB Age of rotating MIST track at TRGB
(MISTageTRGB)
185-189 F5.3 Gyr NR-M-age-TRGB Age non-rot. MIST track at TRGB
(NRMISTage_TRGB)
191-195 F5.3 --- TRGB-frac Fraction of rotating to non-rotating age
at TRGB (TRGB_frac)
197-201 F5.3 Gyr M-age-ZAHeB Age of rotating MIST track at ZAHeB
(MISTageZAHeB)
203-207 F5.3 Gyr NR-M-age-ZAHeB Age non-rot. MIST track at ZAHeB
(NRMISTage_ZAHeB)
209-213 F5.3 --- ZAHeB-frac Fraction of rotating to non-rotating age
at ZAHeB (ZAHeB_frac)
215-219 F5.3 Gyr M-age-TAHeB ? Age of rotating MIST track at TAHeB
(MISTageTAHeB)
221-225 F5.3 Gyr NR-M-age-TAHeB Age non-rot. MIST track at TAHeB
(NRMISTage_TAHeB)
227-231 F5.3 --- TAHeB-frac ? Fraction of rotating to non-rotating
age at TAHeB (TAHeB_frac)
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Note (1): from Li et al., 2020, Cat. J/MNRAS/491/3586.
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Acknowledgements:
Dario Fritzewski, dario.fritzewski(at)kuleuven.be
(End) Patricia Vannier [CDS] 12-Feb-2024