2002A&A...385..951B


Query : 2002A&A...385..951B

2002A&A...385..951B - Astronomy and Astrophysics, volume 385, 951-967 (2002/4-3)

Detailed analysis of Balmer lines in cool dwarf stars.

BARKLEM P.S., STEMPELS H.C., ALLENDE PRIETO C., KOCHUKHOV O.P., PISKUNOV N. and O'MARA B.J.

Abstract (from CDS):

An analysis of Hα and Hβ spectra in a sample of 30 cool dwarf and subgiant stars is presented using MARCS model atmospheres based on the most recent calculations of the line opacities. A detailed quantitative comparison of the solar flux spectra with model spectra shows that Balmer line profile shapes, and therefore the temperature structure in the line formation region, are best represented under the mixing length theory by any combination of a low mixing-length parameter α and a low convective structure parameter y. A slightly lower effective temperature is obtained for the sun than the accepted value, which we attribute to errors in models and line opacities. The programme stars span temperatures from 4800 to 7100K and include a small number of population II stars. Effective temperatures have been derived using a quantitative fitting method with a detailed error analysis. Our temperatures find good agreement with those from the Infrared Flux Method (IRFM) near solar metallicity but show differences at low metallicity where the two available IRFM determinations themselves are in disagreement. Comparison with recent temperature determinations using Balmer lines by Fuhrmann (1998A&A...338..161F, 2000, preprint of Nearby stars of the Galactic disk and halo. II), who employed a different description of the wing absorption due to self-broadening, does not show the large differences predicted by Barklem et al. (2000A&A...363.1091B). In fact, perhaps fortuitously, reasonable agreement is found near solar metallicity, while we find significantly cooler temperatures for low metallicity stars of around solar temperature.

Abstract Copyright:

Journal keyword(s): stars: atmospheres - stars: fundamental parameters - convection

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * mu. Cas SB* 01 08 16.3029454473 +54 55 12.561201263 5.93 5.86 5.17 4.55 4.13 G5Vb 557 1
2 HD 16160 PM* 02 36 04.9013368983 +06 53 12.383654295   6.81   5.2   K3V 515 1
3 HD 19445 PM* 03 08 25.5883873084 +26 19 51.400965175 8.29 8.52 8.06 7.60 7.27 G2VFe-3 753 0
4 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 850 0
5 * 10 Tau PM* 03 36 52.3837044168 +00 24 05.992097829 5.23 5.15 4.30 4.09 3.77 F9IV-V 543 0
6 HD 22879 Pe* 03 40 22.0652879951 -03 13 01.124265616 7.146 7.222 6.667 6.346 6.016 G0VmF2 467 0
7 * omi02 Eri Er* 04 15 16.3196189945 -07 39 10.330779018 5.69 5.25 4.43 3.74 3.29 K0V 776 0
8 * rho Gem PM* 07 29 06.71887 +31 47 04.3773 4.48 4.50 4.18 3.86 3.67 F1V 320 0
9 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1825 0
10 HD 64090 PM* 07 53 33.1208795337 +30 36 18.256204963 8.75 8.86 8.25 7.70 7.30 K0:V_Fe-3 351 0
11 * tet UMa PM* 09 32 51.4338939 +51 40 38.281102 3.67 3.64 3.18 2.74 2.47 F7V 399 0
12 * 35 LMi * 10 36 21.4209550272 +36 19 36.940070136   6.705 6.287     F3V 101 0
13 * bet Vir PM* 11 50 41.7185158616 +01 45 53.001539131 4.26 4.15 3.60 3.13 2.85 F9V 895 0
14 HD 103095 PM* 11 52 58.7673387755 +37 43 07.254113125 7.38 7.20 6.45 5.80 5.35 K1V_Fe-1.5 769 1
15 * alf Crv PM* 12 08 24.8165241 -24 43 43.950354   4.34 4.00     F1V 172 0
16 HD 108177 PM* 12 25 34.9568267745 +01 17 02.259553591 9.87 10.09 9.66 9.21 8.89 F0V 243 0
17 * bet Com PM* 13 11 52.3938268062 +27 52 41.462309460 4.92 4.84 4.25 3.77 3.47 F9.5V 872 0
18 HD 114762 SB* 13 12 19.7410686234 +17 31 01.630334317 7.78         F9VgF8mF4+M6?V 528 1
19 * 70 Vir PM* 13 28 25.8085908881 +13 46 43.638308807 5.930 5.680 4.970 4.37 3.98 G4Va 696 1
20 * iot Vir PM* 14 16 00.8695049 -06 00 01.963348 4.64 4.60 4.08     F7III 348 0
21 * sig Boo PM* 14 34 40.8173867232 +29 44 42.457673940 4.76 4.84 4.47 4.13 3.94 F4VkF2mF1 588 0
22 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 893 0
23 * lam Ser PM* 15 46 26.6142121632 +07 21 11.047378824 5.13 5.03 4.42 3.92 3.60 G0-V 553 0
24 * chi Her PM* 15 52 40.5410491705 +42 27 05.462878877 5.19 5.19 4.62 4.14 3.82 F8VFe-2Hdel-1 490 0
25 * gam Ser PM* 15 56 27.1826948 +15 39 41.820500 4.31 4.34 3.84 3.37 3.13 F6V 546 0
26 * b Her SB* 18 07 01.5906608928 +30 33 43.584892488 5.52 5.67 5.13 4.61 4.28 F6V 441 0
27 * 36 Dra PM* 18 13 53.8328065738 +64 23 50.225760192   5.407 4.987 4.8   F5V 187 0
28 * tet Cyg PM* 19 36 26.5343563 +50 13 15.964573 4.83 4.86 4.48 4.13 3.92 F3+V 339 1
29 * 17 Cyg PM* 19 46 25.6000487071 +33 43 39.353533637   5.46   4.7   F5.5IV-V 260 0
30 HD 219134 Er* 23 13 16.9749603608 +57 10 06.083823619 7.460 6.560 5.570 4.76 4.23 K3V 559 1

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2022.08.08-03:33:12

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