2002A&A...388..978K

Query : 2002A&A...388..978K

2002A&A...388..978K - Astronomy and Astrophysics, volume 388978-984 (2002/6-4)

Do dusty A stars exhibit accretion signatures in their photospheres?

KAMP I., HEMPEL M. and HOLWEGER H.

Abstract (from CDS):

We determined abundances of O, Ca, Fe, Ba and Y for a sample of dusty and dust-free A stars, taken from the list of Cheng et al. (1992ApJ...396L..83C). Five of the stars have an infrared-excess due to circumstellar dust. Ongoing accretion from their circumstellar surroundings might have modified the abundances in the photospheres of these stars, but our results clearly show, that there is no difference in the photospheric composition of the dusty and dust-free stars. Instead all of them show the typical diffusion pattern which diminishes towards larger rotational velocities.

Abstract Copyright: ∼

Journal keyword(s): stars: atmospheres - stars: abundances - stars: early type - stars: circumstellar matter

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * bet Ari SB* 01 54 38.41099 +20 48 28.9133 2.88 2.78 2.65 2.51 2.43 kA4hA5mA5Va 426 1
2 * gam Cet ** 02 43 18.03910 +03 14 08.9390 3.63 3.56 3.47 3.36 3.32 A2Vn+F4V 185 0
3 HD 29573 ** 04 38 53.5501496352 -12 07 23.068127568   5.065 5.002     A0V 99 0
4 * bet Eri PM* 05 07 50.9748851089 -05 05 11.389142292 3.02 2.92 2.79 2.65 2.57 A3IV 231 0
5 * 131 Tau ** 05 47 13.1536316 +14 29 17.967416   5.785 5.721     A3Vn 108 0
6 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 2087 1
7 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1610 0
8 * lam Gem PM* 07 18 05.5789195368 +16 32 25.389581244   3.674 3.559     A4IV 269 0
9 V* DD Lyn dS* 07 55 40.8273346368 +35 24 45.653471280   6.478 6.221     A3p 78 0
10 * iot UMa A SB* 08 59 12.4531549177 +48 02 30.562298470   3.36 3.13     A7V(n) 257 0
11 * iot UMa ** 08 59 12.45362 +48 02 30.5741 3.40 3.33 3.14 2.92 2.85 A6 307 0
12 * bet UMa PM* 11 01 50.4797515135 +56 22 56.761138187 2.35 2.35 2.37 2.31 2.35 A1IVps 462 0
13 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 605 1
14 * rho Vir dS* 12 41 53.0569475088 +10 14 08.252569320 5.00 4.97 4.88 4.80 4.78 A0Va_lB 232 0
15 * lam Boo dS* 14 16 23.0184083839 +46 05 17.895459693 4.31 4.26 4.18 4.16 4.13 A0Va_lB 362 0
16 * alf02 Lib SB* 14 50 52.71309 -16 02 30.3955 2.99 2.90 2.75 2.61 2.57 kA2hA5mA4IV-V 231 0
17 * alf CrB SB* 15 34 41.2684881676 +26 42 52.866000089 2.19 2.22 2.24 2.21 2.25 A1IV 499 0
18 * b Ser ** 15 51 15.5919760102 -03 05 25.822526196   5.23 5.10     A2IV-Vn 121 0
19 * eta Oph ** 17 10 22.68689 -15 43 29.6639 2.56 2.47 2.42 2.39 2.38 A2IV-V 271 0
20 * alf Oph ** 17 34 56.06945 +12 33 36.1346 2.32 2.22 2.07 1.93 1.85 A5IVnn 495 0
21 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0V 2787 1
22 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1303 3
23 * 15 And dS* 23 34 37.5368337288 +40 14 11.182658856   5.652 5.563 6.91   A1Va 141 0

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