2001A&A...375..899K


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.14CEST14:20:35

2001A&A...375..899K - Astronomy and Astrophysics, volume 375, 899-908 (2001/9-1)

Light element non-LTE abundances of λ Bootis stars. II. Nitrogen and sulphur.

KAMP I., ILIEV I.K., PAUNZEN E., PINTADO O.I., SOLANO E. and BARZOVA I.S.

Abstract (from CDS):

One of the main characteristics proclaimed for the group of the λ Bootis stars is the apparent solar abundance of the light elements C, N, O and S. The typical abundance pattern is completed by the strong underabundances of the Fe-peak elements. In the first paper of this series, we have shown that carbon is less abundant than oxygen but both elements are still significantly more abundant than Fe-peak elements. The mean abundances, based on a detailed non-LTE investigation, were found -0.37dex and -0.07dex, respectively. As a further step, we now present non-LTE abundances of nitrogen and sulphur for thirteen members of the λ Bootis group based on several spectral lines between 8590Å and 8750Å. Furthermore, LTE abundances for calcium in the same spectral range were derived and compared with values from the literature. Similar to the mean abundances of carbon and oxygen, nearly solar values were found (-0.30dex for nitrogen and -0.11dex for sulphur) for our sample of program stars. Among our sample, one previously undetected binary system (HD 64491) was identified. From a statistical point of view, the abundances of the light elements range from slightly overabundant to moderately underabundant compared to the Sun. However, the individual objects always exhibit a similiar pattern, with the Fe-peak elements being significantly more underabundant than the light elements. No correlation of the derived abundances with astrophysical parameters such as the effective temperature, surface gravity or projected rotational velocity was found. Furthermore, the abundances of the light elements do not allow us to discriminate between any proposed theory.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: atmospheres - stars: chemically peculiar - stars: early-type

Simbad objects: 33

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Number of rows : 33

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 HD 319 PM* 00 07 46.9004138978 -22 30 30.805804687   6.055 5.923     A1VbmA2_lB 96 0
2 HD 4158 * 00 43 54.0507216077 -20 23 59.224550251   9.76 9.54     F2VkA1.5mA1.5_lB 36 0
3 V* BS Tuc dS* 01 08 03.9684578139 -61 52 17.819432212   7.71 7.45     hF0mA1_lB 89 0
4 V* BD Phe dS* 01 50 54.4351104603 -50 12 22.093636860   6.080 5.929     F0VkA2mA2_lB 96 0
5 HD 15165 dS* 02 26 45.6479225723 +10 33 55.067355855   6.94 6.69     F0IV 85 0
6 V* EX Eri dS* 04 46 25.7495931083 -28 05 14.805481115   6.347 6.173     A7VkA3mA3 107 0
7 * pi.01 Ori PM* 04 54 53.7287660 +10 09 02.995200   4.723 4.648     A0Va_lB 239 0
8 NAME Ori I As* 05 38 -02.8           ~ 559 0
9 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1593 1
10 V* DD Lyn dS* 07 55 40.8263456114 +35 24 45.669980557   6.478 6.221     A3p 64 0
11 V* HZ Vel dS* 08 49 52.3521085534 -39 08 29.770890153   6.602 6.368     A2/3II/III 64 0
12 HD 84123 PM* 09 44 06.8765461366 +42 03 03.131298842   7.135 6.838     A4III 49 0
13 * 33 LMi * 10 31 51.3746360193 +32 22 46.412107377   6.001 5.905     A0Va- 63 0
14 HD 101108 * 11 38 19.3665601704 +38 45 16.899688742   9.05 8.87     A5_lB 38 0
15 HD 107233 PM* 12 19 55.6449203485 -48 18 59.468148848   7.60 7.36     hF0VakA1mA1_lB 36 0
16 HD 111005 * 12 46 14.8232750824 +02 27 51.466749998   8.30 7.97     A9V 36 0
17 V* FQ Boo dS* 13 49 44.1555631872 +08 24 31.089806068   6.717 6.604     hA5VkA2mA2_lB 42 0
18 * lam Boo dS* 14 16 23.0187965 +46 05 17.900526 4.31 4.26 4.18 4.16 4.13 A0Va_lB 325 0
19 * b Ser ** 15 51 15.5941805 -03 05 25.793806   5.23 5.10     A2IV-Vn 104 0
20 V* HR Lib dS* 15 56 33.3735361896 -14 49 45.972376397   6.345 6.117     A2Ib/II 105 0
21 HD 149303 * 16 31 47.2283629879 +45 35 53.746886684 5.850 5.78 5.68 7.16   A2Vn_lB 56 0
22 V* NP TrA dS* 16 33 05.1549259176 -60 54 12.846211369   8.09 7.90     A2IVn 21 0
23 V* V346 Pav dS* 18 25 31.6299481485 -63 01 17.532599707   6.313 6.122     A8VkA2mA2_lB 64 0
24 HD 170680 * 18 31 26.2981687662 -18 24 09.706451275   5.126 5.117     B9/9.5V 77 0
25 * c Aql dS* 19 29 00.9870438377 +01 57 01.618441082   5.865 5.783     A0IVp 163 0
26 * b03 Cyg dS* 20 14 32.0319919055 +36 48 22.684605093 5.10 5.11 4.99 4.79 4.72 A2V 241 0
27 HD 193256 * 20 20 26.5741252340 -29 11 28.761537820   7.703 7.525 8.49   A8VnkA3mA3(_lB) 61 0
28 HD 193281 * 20 20 27.8805474206 -29 11 49.975108388   6.76 6.64 7.50   A2IV-V 90 0
29 HD 198160 PM* 20 51 38.5079641449 -62 25 45.594366275   6.347 6.207 6.55   A3IV(n) 68 0
30 HD 198161 PM* 20 51 38.8562507171 -62 25 45.255721251   6.733 6.555     A3III 32 0
31 HD 204041 PM* 21 25 51.5846178730 +00 32 03.619939380   6.593 6.450     A1Vb 94 0
32 HD 210111 dS* 22 08 42.6438955365 -33 07 32.498239929   6.564 6.386     A9VkA2mA2_lB 72 0
33 * 15 And dS* 23 34 37.5365247800 +40 14 11.179472901   5.652 5.563 6.91   A1Va 125 0

    Equat.    Gal    SGal    Ecl

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2020.08.14-14:20:35

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