# 2006A&A...459..137R

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 Query : 2006A&A...459..137R

2006A&A...459..137R - Astronomy and Astrophysics, volume 459, 137-145 (2006/11-3)

Bright Be-shell stars.

RIVINIUS T., STEFL S. and BAADE D.

Abstract (from CDS):

Echelle observations are presented and discussed for 23 of the 27 known normal'' shell stars brighter than about 6.5mag. In addition to those typical cases, three stars with known transitions between emission&shell and pure emission line appearance, and three rapidly rotating B stars without records of line emission (Bn stars) are added to the sample. Long-term V/R emission-line variability and central quasi emission bumps (CQEs) in photospheric lines were found in 75% of all normal shell stars. This strongly suggests that the velocity law in most, if not all, disks of Be stars is roughly Keplerian. Both phenomena may occur in the same star but not at the same time. This is in agreement with the previous conclusion that CQEs only form in the presence of negligible line-of-sight velocities while long-term V/R variations are due to non-circular gas particle orbits caused by global disk oscillations. V/R variations associated with binary orbits are much less pronounced. Similarly, phase lags between different lines were detected in long-term V/R variable stars only. A binary fraction of only one-third is too low to support binary hypotheses as an explanation of the Be phenomenon. CQEs detected in 3 out of 19 Bn stars reveal the presence of disk-like equatorial concentrations of matter in B stars without emission lines. Accordingly, there seem to be intermediate cases between disk-free B stars and Be stars. Previous claims of the existence of shell stars with low vsini could not be confirmed. Shell stars are Be stars viewed equator-on, and their observed rotational velocities are indistinguishable from the equatorial ones which are the same as in Be stars. The mean fraction of the critical rotation velocity is 81±12%. The standard deviation is comparable to, or even less than, the observational uncertainties. Since this would require star-to-star differences to be negligible, which is unrealistic, the correlation between the widths of strong spectral lines and the stellar rotation velocities may be truncated or severely distorted at its extreme end. A number of not previously known facts about individual stars is also reported.

Journal keyword(s): stars: emission line, Be - stars: circumstellar matter - stars: rotation - stars: statistics

VizieR on-line data: <Available at CDS (J/A+A/459/137): tables 2-11 tables.tex>

Full paper

 Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 * gam Cas Be* 00 56 42.5310945 +60 43 00.264089 1.18 2.29 2.39 2.32 2.40 B0.5IVpe 1182 2
2 * phi Per Be* 01 43 39.6379209 +50 41 19.432832 3.10 4.02 4.06 3.90 3.88 B1.5V:e-shell 563 0
3 * mu. For * 02 12 54.4699976208 -30 43 25.773757068   5.243 5.260   5.26 A0V 80 0
4 * psi Per Be* 03 36 29.3798227 +48 11 33.478941 3.60 4.17 4.23     B5Ve 409 0
5 * 28 Tau Be* 03 49 11.2165977912 +24 08 12.156712008 4.73 5.01 5.09   5.08 B8Vne 461 0
6 HD 35165 Be* 05 21 16.8603281544 -34 20 42.173559132 5.24 5.90 6.09 6.12 6.26 B3IVe 74 1
7 * zet Tau Be* 05 37 38.6854231 +21 08 33.158804 2.22 2.84 3.03 3.06 3.15 B1IVe_shell 719 0
8 HD 41335 Be* 06 04 13.5003372120 -06 42 32.225392980 4.31 5.14 5.21 5.13 5.09 B1V 293 0
9 * bet Mon ** 06 28 49.06971 -07 01 59.0101 2.85 3.59 3.74 3.75 3.91 B4Ve+B2Vn(e)+B3V:nne 224 0
10 * bet Mon A Be* 06 28 49.0704018024 -07 01 59.013827328 3.87 4.50 4.60     B4Veshell 245 0
11 * nu. Gem Be* 06 28 57.7861342 +20 12 43.685624 3.51 4.00 4.14 4.17 4.28 B6IVe 254 0
12 * nu. Pup Ce* 06 37 45.6713527 -43 11 45.360171 2.65 3.06 3.17 3.17 3.24 B8III 138 0
13 * 27 CMa Be* 07 14 15.2119175 -26 21 09.031206 3.76 4.45 4.65 4.64 4.73 B4Ve_sh 228 0
14 * ome CMa Be* 07 14 48.6538664 -26 46 21.609714 2.90 3.64 3.82 3.80 3.90 B2.5Ve 347 0
15 HD 65875 Be* 08 00 44.1338106480 -02 52 54.913100736 5.68 6.49 6.59 6.48 6.50 B2.5Ve 136 0
16 * ome Car Be* 10 13 44.2173938 -70 02 16.456305 2.92 3.25 3.33 3.29 3.32 B7III 120 0
17 * J Vel Be* 10 20 54.7957129824 -56 02 35.655748188 3.80 4.38 4.51 6.02   B5II 105 0
18 HD 91120 Be* 10 30 59.8371178656 -13 35 18.495281472 5.38 5.54 5.58     B9IIIe 105 0
19 HD 93563 Be* 10 46 57.4726412 -56 45 25.890016 4.82 5.15 5.23     B5III 69 0
20 * 39 Cru Be* 12 41 56.5691823528 -59 41 08.954444508 4.55 4.91 4.94     B5III 102 0
21 * eta Cen Be* 14 35 30.4241610 -42 09 28.170782 1.30 2.12 2.31 2.41 2.59 B2Ve 337 0
22 * tet Cir Be* 14 56 43.9873836 -62 46 51.657921 4.34 5.11 5.11 4.87 4.79 B2III 108 0
23 * kap01 Aps Be* 15 31 30.8221293192 -73 23 22.529543604 4.60 5.37 5.49     B2Vnpe 114 0
24 * tet CrB Be* 15 32 55.78214 +31 21 32.8762 3.45 4.00 4.13 4.18 4.29 B6Vnne 286 0
25 * b Sco * 15 50 58.7444628720 -25 45 04.658676984 3.84 4.552 4.635     B1.5Vn 287 0
26 * 2 Sco ** 15 53 36.71880 -25 19 37.7087 3.86 4.52 4.59     B2.5Vn 157 0
27 * 4 Her Be* 15 55 30.5919435384 +42 33 58.291421364 5.23 5.64 5.75   5.82 B9pe 177 0
28 * 48 Lib Be* 15 58 11.3682502453 -14 16 45.681109093 4.61 4.77 4.87 4.91 4.96 B5IIIp_sh 436 0
29 * c Oph Be* 17 31 24.9538710166 -23 57 45.514802684 4.75 4.81 4.81 4.74 4.72 A0V 270 0
30 * z Her Be* 17 50 03.3345672768 +48 23 38.948985636 6.380 6.790 6.890     B6IIInp_sh 159 0
31 HD 178175 Be* 19 08 16.7018664360 -19 17 25.037957508 4.79 5.43 5.49 5.50 5.51 B2Ve 142 0
32 HD 183656 Be* 19 30 33.1219108488 +03 26 39.860267784 5.69 6.064 6.082     B7III 128 0
33 HD 193182 Be* 20 17 25.1772454344 +39 35 36.746489184 6.23 6.42 6.51     B7IV/V:(e) 80 0
34 * 1 Del ** 20 30 17.96064 +10 53 45.3233 5.94 6.05 6.08     A1:III 106 0
35 * f01 Cyg Be* 20 59 49.5541247496 +47 31 15.363746436 3.77 4.71 4.75 4.62 4.63 B1.5Vnne 488 0
36 * eps Cap Be* 21 37 04.8306787 -19 27 57.646354 3.69 4.35 4.55 4.60 4.74 B3V 252 0
37 * omi Aqr Be* 22 03 18.8440292 -02 09 19.306758 4.22 4.64 4.69 4.70 4.74 B5V 265 0
38 * eta Aqr PM* 22 35 21.38126 -00 07 02.9888 3.690 3.950 4.030 4.06 4.13 B8/9V 159 0
39 HD 217050 Be* 22 57 04.5020619144 +48 41 02.645623680 4.81 5.34 5.43     B4IIIpe 327 1
40 * omi And Be* 23 01 55.2645930 +42 19 33.533383 3.00 3.53 3.62 3.61 3.69 B6IV/V_sh 425 0

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2023.03.27-06:19:42