2003A&A...411..229R


Query : 2003A&A...411..229R

2003A&A...411..229R - Astronomy and Astrophysics, volume 411, 229-247 (2003/11-4)

Non-radially pulsating Be stars.

RIVINIUS T., BAADE D. and STEFL S.

Abstract (from CDS):

Based on more than 3000 high-resolution echelle spectra of 27 early-type Be stars, taken over six years, it is shown that the short-term periodic line profile variability of these objects is due to non-radial pulsation. The appearance of the line profile variability depends mostly on the projected rotational velocity v sin i and thus, since all Be stars rotate rapidly, on the inclination i. The observed variability of the investigated stars is described, and for some of them line profile variability periods are given for the first time. For two of the investigated stars the line profile variability was successfully modeled as non-radial pulsation with l=m=+2 already in previous works. Since Be stars with similarly low vsini share the same variability properties, these are in general explainable under the same model assumptions. The line profile variability of stars with higher vsini is different from the one observed in low vsini stars, but can be reproduced by the same model, if only the model inclination is modified to more equatorial values. Only for a few stars with periodic line profile variability the l=m=2 non-radial pulsation mode is not able to provide a satisfying explanation. These objects might pulsate in different modes (e.g. tesseral ones, l≠|m|). Almost all stars in the sample show traces of outburst-like variability, pointing to an ephemeral nature of the mass-loss phenomenon responsible for the formation of the circumstellar disk of early-type Be stars, rather than a steady star-to-disk mass transfer. In addition to the variability due to non-radial pulsation present in most stars, several objects were found to show other periods residing in the immediate circumstellar environment. The presence of these secondary periods is enhanced in the outburst phases. Short-lived aperiodic phenomena were clearly seen in two stars. But, given the unfavourable sampling of our database to follow rapid variability of transient nature, they might be more common. Only in two out of 27 stars short-term spectroscopic variability was not detected at all.

Abstract Copyright:

Journal keyword(s): stars: emission-line, Be - stars: oscillations

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 - 2023
#notes
1 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 460 0
2 * eps Per bC* 03 57 51.2320472 +40 00 36.775143 1.71 2.71 2.89 2.96 3.14 B1.5III 509 0
3 * 228 Eri Be* 04 29 06.9254098152 -13 02 54.127769208 4.45 5.23 5.41 5.46 5.63 B2(V)ne 271 0
4 * 56 Eri Be* 04 44 05.3207274312 -08 30 12.852684720 4.97 5.75 5.81 5.72 5.74 B2(V)nne 176 0
5 * lam Eri Be* 05 09 08.7831482 -08 45 14.690823 3.17 4.07 4.27 4.35 4.55 B2III(e)p 294 1
6 * zet Tau Be* 05 37 38.6854231 +21 08 33.158804 2.22 2.84 3.03 3.06 3.15 B1IVe_shell 711 0
7 * ome Ori Be* 05 39 11.1463172 +04 07 17.279475 3.73 4.48 4.59 4.57 4.67 B3Ve 398 1
8 * 10 CMa Be* 06 44 28.4671043496 -31 04 13.892357820 4.18 5.08 5.17 5.15 5.17 B2V 139 0
9 * kap CMa Be* 06 49 50.4593263 -32 30 30.522482 2.73 3.68 3.89 3.91 4.05 B1.5Ve 278 0
10 * ome CMa Be* 07 14 48.6538664 -26 46 21.609714 2.90 3.64 3.82 3.80 3.90 B2.5Ve 343 0
11 HD 58343 Be* 07 24 40.1873324160 -16 12 05.302248804 4.52 5.15 5.19 5.05 5.06 B2Vne 206 0
12 * E Car Be* 09 05 38.3753516880 -70 32 18.594082500 3.75 4.500 4.652     B3III 93 0
13 HD 88661 Be* 10 11 46.4595963216 -58 03 37.958712444 4.77 5.66 5.75 5.66 5.70 B5Vne 143 0
14 * J Vel Be* 10 20 54.7957129824 -56 02 35.655748188 3.80 4.38 4.51 6.02   B5II 101 0
15 * p Car Be* 10 32 01.4629679 -61 41 07.196308 2.46 3.18 3.27 3.22 3.28 B4Vne 227 0
16 * del Cen Be* 12 08 21.4976373 -50 43 20.738614 1.51 2.39 2.52 2.48 2.62 B2Vne 302 0
17 HD 105521 Be* 12 08 54.5892904200 -41 13 53.771811240 4.87 5.402 5.498     B3IVe 77 0
18 * mu. Cen Be* 13 49 36.9886294 -42 28 25.429594 2.37 3.27 3.43 3.41 3.50 B2Vnpe 425 0
19 HD 120991 Be* 13 53 57.2397645360 -47 07 41.390612184 5.11 6.03 6.10 6.24 6.34 B2Ve 133 0
20 * eta Cen Be* 14 35 30.4241610 -42 09 28.170782 1.30 2.12 2.31 2.41 2.59 B2Ve 332 0
21 * chi Oph Be* 16 27 01.4355697915 -18 27 22.499961252 3.95 4.71 4.43 3.97 3.73 B2Vne 582 0
22 * iot Ara Be* 17 23 16.0762402440 -47 28 05.505681720 4.32 5.14 5.25 5.12 5.20 B1V 141 0
23 * alf Ara Be* 17 31 50.4915282 -49 52 34.122041 2.09 2.78 2.95 3.05 3.29 B2Vne 250 0
24 * 66 Oph Be* 18 00 15.7982457 +04 22 07.016285 3.77 4.58 4.60 4.47 4.49 B2Ve 336 0
25 * lam Pav Be* 18 52 13.0342656 -62 11 15.332363 3.19 4.048 4.207     B2Ve 145 0
26 * b02 Cyg Be* 20 09 25.6190611128 +36 50 22.633958400 4.03 4.80 4.93     B2.5Ve 256 0
27 * eps Cap Be* 21 37 04.8306787 -19 27 57.646354 3.69 4.35 4.55 4.60 4.74 B3V 248 0
28 * 31 Peg Be* 22 21 31.0751048 +12 12 18.662815 4.08 4.89 4.99 5.06 5.20 B3III 217 0
29 * pi. Aqr Be* 22 25 16.6228499 +01 22 38.634579 3.64 4.60 4.64 4.48 4.48 B1III-IVe 400 0
30 * omi And Be* 23 01 55.2645930 +42 19 33.533383 3.00 3.53 3.62 3.61 3.69 B6IV/V_sh 419 0

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2022.12.09-19:29:39

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