2011A&A...526A.100P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST19:27:34

2011A&A...526A.100P - Astronomy and Astrophysics, volume 526A, 100-100 (2011/2-1)

Surface convection and red-giant radius measurements.

PIAU L., KERVELLA P., DIB S. and HAUSCHILDT P.

Abstract (from CDS):

Phenomenological models of convection adopt characteristic length scales that are chosen to fit solar or stellar observations. We investigate whether changes in these length scales are required between the Sun and low mass stars on the red giant branch (RGB). The question is addressed jointly in the frameworks of the mixing length theory and the full spectrum of turbulence model. For both models, the convective length scale is assumed to be a fixed fraction of the local pressure scale height. We use constraints provided by the observed effective temperatures and linear radii independently. We consider a sample of 38 nearby giants and subgiants for which surface temperatures and luminosities are known accurately and the radii are determined by interferometry to better than 10%. We computed dedicated models for the few cases where the stellar masses were determined by asteroseismological measurements. First we calibrated the solar models. With the same physics, we then computed RGB models for masses between 0.9M and 2.5M and metallicities ranging from [Fe/H]=-0.34 to solar. The evolution is followed up to 103L. Special attention is given to the opacities and the non-grey atmosphere models used as boundary conditions for which the model of convection is the same as in the interior. For both the mixing length theory and the full spectrum of turbulence models, the characteristic solar length scale for convection has to be slightly reduced to fit the lower edge of the observed RGB. The corresponding models also agree more closely with the expected mass distribution on the RGB and the seismic constraints. These results are robust regardless of effective temperatures determined spectroscopically or radii determined interferometrically are used.

Abstract Copyright:

Journal keyword(s): stars: low-mass - convection - stars: evolution - asteroseismology

Simbad objects: 37

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Number of rows : 37

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * del And SB* 00 39 19.6751809 +30 51 39.678320 6.04 4.56 3.28 2.36 1.70 K3III-IIIbCN0.5 313 0
2 * l Psc PM* 01 21 07.3725839920 +28 44 17.553616356   6.630 5.223     K5III 37 0
3 * ups Per PM* 01 37 59.5569926 +48 37 41.569533 6.29 4.85 3.57 2.61 1.96 K3-IIICN0.5 217 0
4 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 604 1
5 * 39 Ari PM* 02 47 54.5414187 +29 14 49.613199 6.710 5.630 4.510 3.72 3.14 K0.5IIIb 154 0
6 * 24 Per * 02 59 03.6763920773 +35 10 59.286480336 7.460 6.170 4.930     K2III 115 0
7 * del Ari PM* 03 11 37.7646526 +19 43 36.039699 6.26 5.40 4.37 3.60 3.09 G9.5IIIb 172 0
8 * del Eri RS* 03 43 14.9008787 -09 45 48.208444 5.13 4.46 3.54 2.82 2.32 K0+IV 542 0
9 * 37 Tau PM* 04 04 41.7148415 +22 04 54.924282 6.41 5.44 4.37 3.58 3.05 K0III-IIIb 171 0
10 * del Tau SB* 04 22 56.1010361735 +17 32 33.055967140 5.56 4.74 3.76 5.56   G9.5IIICN0.5 497 0
11 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1178 1
12 * sig Gem RS* 07 43 18.7269793 +28 53 00.642191 6.38 5.41 4.29 3.37 2.79 K1IIIe 444 0
13 * bet Cnc PM* 08 16 30.9210081 +09 11 07.957924 6.750 5.000 3.520 2.42 1.62 K4IIIBa0.5: 342 0
14 * alf Lyn PM* 09 21 03.3007431 +34 23 33.224546 6.63 4.69 3.14 1.91 1.01 K6III 196 0
15 * alf Hya * 09 27 35.24270 -08 39 30.9583 5.14 3.42 1.97 0.93 0.16 K3IIIa 406 0
16 * 31 Leo PM* 10 07 54.2705662 +09 59 51.023021 7.57 5.82 4.38 3.26 2.49 K3.5IIIbFe-1: 127 0
17 * 46 LMi PM* 10 53 18.7048735 +34 12 53.537492 5.79 4.87 3.83 3.00 2.46 K0+III-IV 222 0
18 * psi UMa PM* 11 09 39.8086764 +44 29 54.552050 5.27 4.15 3.01 2.18 1.61 K1III 261 0
19 * nu. UMa * 11 18 28.7366424 +33 05 39.510697 6.44 4.89 3.49 2.43 1.73 K3-III: 188 0
20 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 231 0
21 * ups Boo PM* 13 49 28.6407858 +15 47 52.460283 7.46 5.59 4.07 2.87 2.00 K5.5III 135 0
22 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2133 0
23 * rho Boo PM* 14 31 49.7896173 +30 22 17.178087 6.33 4.89 3.59 2.67 2.02 K3-III 245 0
24 * bet UMi V* 14 50 42.32580 +74 09 19.8142 5.32 3.55 2.08 0.97 0.21 K4-III 302 0
25 * omi CrB PM* 15 20 08.5587408139 +29 36 58.343581022 7.30 6.53 5.51     K0III 131 1
26 * eps Oph PM* 16 18 19.2897431 -04 41 33.034466 4.95 4.21 3.23 2.54 2.05 G9.5IIIbFe-0.5 225 0
27 * mu.01 Her ** 17 46 27.5266778 +27 43 14.437984 4.56 4.17 3.42 2.89 2.51 G5IV 648 0
28 * gam Dra * 17 56 36.36988 +51 29 20.0242 5.630 3.760 2.230 1.08 0.23 K5III 516 0
29 * eta Ser PM* 18 21 18.6005560 -02 53 55.776595 4.84 4.19 3.25 2.55 2.05 K0III-IV 351 0
30 * eps Aql SB* 18 59 37.3616087625 +15 04 05.880705609 6.14 5.10 4.02 3.26 2.74 K1-IIICN0.5 178 0
31 * i Aql V* 19 01 40.8270735 -05 44 20.813427 6.15 5.11 4.02 3.23 2.69 K1III 88 0
32 * bet Aql PM* 19 55 18.7925630 +06 24 24.342501 5.040 4.560 3.710 3.05 2.56 G8IV 514 0
33 * gam Sge PM* 19 58 45.4286265 +19 29 31.728079 6.97 5.04 3.47 2.27 1.35 M0-III 241 0
34 * 39 Cyg SB* 20 23 51.6206989 +32 11 24.619097 7.27 5.77 4.44 3.43 2.76 K2.5IIIFe-0.5 129 0
35 * eta Cep PM* 20 45 17.3755540 +61 50 19.616737 4.960 4.320 3.410 2.76 2.27 K0IV 419 0
36 * eps Cyg ** 20 46 12.6823609 +33 58 12.924926 4.370 3.520 2.480 1.73 1.19 K0III 480 0
37 * 11 Lac PM* 22 40 30.8588068 +44 16 34.704241 7.15 5.79 4.46 3.54 2.86 K2.5III 123 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-19:27:34

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