2006A&A...459..215S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST23:41:40

2006A&A...459..215S - Astronomy and Astrophysics, volume 459, 215-227 (2006/11-3)

Variations of the HeII λ1640 line in B0e-B2.5e stars.

SMITH M.A.

Abstract (from CDS):

Using the International Ultraviolet Explorer data archive, we have examined the SWP echellograms of 74 B0-B2.5e stars for statistically significant fluctuations in the HeII (``Hα'') λ1640 line profile. In this sample we found that the HeII line is occasionally variable in 10 stars over short to long timescales. The HeII-variable stars discovered are λ Eri, ω Ori, µ Cen, 6 Cep, HD 67536, ψ1 Ori, η Cen, π Aqr, 2 Vul, and 19 Mon. The most frequent two types of variability are an extended blue wing absorption and a weakening of the line along the profile. Other types of variability are a weak emission in the red wing and occasionally a narrow emission feature. In the overwhelming number of cases, the CIV resonance doublet exhibits a similar response; rarely, it can exhibit a variation in the opposite sense. Similar responses are also often seen in the SiIV doublet, and occasionally even the SiIII λ1206 line. We interpret the weakenings of HeII and of high-velocity absorptions of CIV to localized decreases in the photospheric temperature, although this may not be a unique interpretation. We discuss the variable blue wing absorptions and red wing emissions in terms of changes in the velocity law and mass flux carried by the wind. In the latter case, recent experimental models by Venero, Cidale, & Ringuelet (2000, ASP Conf. Ser., 214, 607) require that during such events the wind must be heated by 35000K at some distance from the star.

Abstract Copyright:

Journal keyword(s): stars: general - stars: emission-line, Be - stars: winds, outflows - ultraviolet: stars

Simbad objects: 15

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Number of rows : 15

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 * lam Eri Be* 05 09 08.7831482 -08 45 14.690823 3.17 4.07 4.27 4.35 4.55 B2III(e)p 283 1
2 * psi01 Ori Be* 05 24 44.8269466961 +01 50 47.202396831 3.83 4.76 4.96 5.04 5.26 B1Vn 322 0
3 HD 36959 Y*O 05 35 01.0063388388 -06 00 33.371107627 4.52 5.33 5.53     B1.2 192 0
4 * sig Ori E Y*O 05 38 47.2050001416 -02 35 40.514907495 5.66 6.38 6.46 6.84 7.08 B2IV-Vp_He 400 0
5 * ome Ori Be* 05 39 11.1463172 +04 07 17.279475 3.73 4.48 4.59 4.57 4.67 B3Ve 388 1
6 * 19 Mon bC* 07 02 54.7766724 -04 14 21.237679 3.87 4.80 5.00 5.06 5.25 B2Vn(e) 181 0
7 * ome CMa Be* 07 14 48.6538664 -26 46 21.609714 2.90 3.64 3.82 3.80 3.90 B2.5Ve 329 0
8 HD 67536 Pu* 08 04 42.9316419264 -62 50 10.842413272   6.136 6.241     B2Vn 53 1
9 * eta UMa PM* 13 47 32.43776 +49 18 47.7602 0.99 1.67 1.86 1.98 2.16 B3V 579 0
10 * mu. Cen Be* 13 49 36.9886294 -42 28 25.429594 2.37 3.27 3.43 3.41 3.50 B2Vnpe 411 0
11 * eta Cen Be* 14 35 30.4241610 -42 09 28.170782 1.30 2.12 2.31 2.41 2.59 B2Ve 322 0
12 * tau Sco * 16 35 52.9528530 -28 12 57.661515 1.55 2.56 2.81 2.93 3.18 B0.2V 854 0
13 * 2 Vul Pu* 19 17 43.6353095659 +23 01 31.939943157 4.64 5.43 5.43     B0.5IV 131 1
14 * 6 Cep Be* 21 19 22.2202464 +64 52 18.682115 4.56 5.14 5.18     B3IVe 152 0
15 * pi. Aqr Be* 22 25 16.6228499 +01 22 38.634579 3.64 4.60 4.64 4.48 4.48 B1III-IVe 384 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-23:41:40

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