# 2003A&A...397..747K

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 Query : 2003A&A...397..747K

2003A&A...397..747K - Astronomy and Astrophysics, volume 397, 747-756 (2003/1-2)

The photospheric abundances of active binaries. I. Detailed analysis of HD 113816 (IS Vir) and HD 119285 (V851 Cen).

KATZ D., FAVATA F., AIGRAIN S. and MICELA G.

Abstract (from CDS):

The high-resolution optical spectra of the two X-ray active binaries RS CVn stars HD113816 (IS Vir) and HD119285 (V851 Cen) are analysed and their Na, Mg, Al, Si, Ca, Sc, Ti, Co and NI contents determined, in the framework of a larger program of chemical analysis of RS CVn stellar atmosphere. The analysis of IS Vir and V851 Cen is performed with three different LTE methods. In the first one, abundances are derived for a large set of transitions (among which 28 Fe I lines, spanning a broad interval in excitation potential and equivalent width, and 6 Fe II transitions) using measured equivalent widths and Kurucz LTE model atmospheres as input for the MOOG software package. The input atmospheric parameters and abundances are iteratively modified until (i) the Fe I abundances exhibit no trend with excitation potential or equivalent width, (II) Fe I and Fe II average abundances are the same and (III) Fe and Alpha elements average abundances are consistent with the input values. The second method follows a similar approach, but uses a restricted line list (without the Fe I low excitation potential'' transitions) and relies on the B-V and V-I colour indices to determine the temperature. The third method uses the same restricted line list as the second method and relies on fitting the 6162Å Ca I line wing profiles to derive the surface gravity. The reliability of these methods is investigated in the context of single line RS CVn stars. It is shown that the V-I photometric index gives, on a broader sample of stars, significantly cooler estimates of the effective temperature than the B-V index. All approaches give results in good agreement with each other, except the V-I based method. The analysis of IS Vir and V851 Cen results in both cases in their primaries being giant stars of near-solar metallicity. Their parameters as derived with the first method are respectively Teff=4720K, logg=2.65, [Fe/H]=+0.04 and Teff=4700K, logg=3.0 and [Fe/H]=-0.13. In the case of V851 Cen the derived iron content is significantly higher than a previous determination in the literature. Both stars exhibit relative overabundances of several elements (e.g. Ca) with respect to the solar mix.

Journal keyword(s): stars: fundamental parameters - stars: abundances - stars: individual: HD 113816, HD 119285

Full paper

 Number of rows : 26
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 * 9 Cet BY* 00 22 51.7884553555 -12 12 33.969921319 7.29 7.05 6.39     G2.5V 467 0
2 HD 10307 SB* 01 41 47.1268541099 +42 36 48.221567818 5.69 5.58 4.96 4.43 4.10 G1V 483 0
3 HD 24040 PM* 03 50 22.9675921536 +17 28 34.926384648   8.18   7.1   G1 116 1
4 V* AG Dor RS* 04 07 29.1836707992 -52 34 17.227000956   9.50 8.595   7.526 K2IV-Vk 84 0
5 HD 28099 BY* 04 26 40.1217122952 +16 44 48.885808416 8.98 8.78 8.12 7.56 7.23 G2+V 391 0
6 V* YZ Men RS* 05 10 26.7502372080 -77 13 01.526708712   8.85 7.77   6.566 K1IIIp 46 0
7 V* V344 Pup RS* 07 36 13.8053448264 -44 57 27.454999500   7.95 6.89     K2III 50 0
8 V* VX Pyx RS* 08 32 58.5001559256 -34 38 02.540585832   7.318 6.366     G8III 73 0
9 V* IL Hya RS* 09 24 49.0136973144 -23 49 34.714396272   8.38 7.37     K2IV/Vp 164 0
10 * mu. Leo PM* 09 52 45.8165435 +26 00 25.031882 6.50 5.10 3.88 2.97 2.39 K2IIIbCN1Ca1 427 0
11 * 20 LMi PM* 10 01 00.6568762394 +31 55 25.213014837   6.02   4.9   G3VaHdel1 373 0
12 * 47 UMa PM* 10 59 27.9727514012 +40 25 48.920572724   5.66   4.7   G1-VFe-0.5 748 1
13 V* HU Vir RS* 12 13 20.6914862928 -09 04 46.880926320   9.69 8.71   7.639 K1V 140 0
14 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 537 0
15 V* IS Vir RS* 13 06 26.0092106448 -04 50 45.306856248   9.50 8.432   7.175 K0III 51 1
16 * 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
17 * e Vir PM* 13 16 46.5148594512 +09 25 26.960139646   5.81   4.8   G0V 529 1
18 V* V851 Cen RS* 13 44 00.9212469648 -61 21 59.173175844   8.74 7.798   6.638 K0III 82 0
19 V* GX Lib RS* 15 23 26.0566952568 -06 36 37.745079696   8.39 7.35     G8IVp 109 0
20 * 18 Sco PM* 16 15 37.2702755653 -08 22 09.982125430   6.15 5.50     G2Va 545 0
21 * mu. Aql PM* 19 34 05.3529921054 +07 22 44.184329526 6.87 5.63 4.45 3.55 2.94 K3-IIIbFe0.5 258 1
22 * 16 Cyg A ** 19 41 48.9534996168 +50 31 30.219536784 6.79 6.59 5.95 5.50 5.17 G1.5Vb 717 1
23 * 16 Cyg B PM* 19 41 51.9726777456 +50 31 03.089030916 7.07 6.86 6.20 5.76 5.42 G3V 842 1
24 * omi Aql PM* 19 51 01.6436960928 +10 24 56.592457524   5.66   4.8   F8V 439 0
25 * 51 Peg PM* 22 57 27.9804852576 +20 46 07.797040104 6.39 6.16 5.46 4.97 4.61 G2IV 1120 1
26 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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2022.08.11-00:42:54