Abundances and radial velocity analysis of BW Vulpeculae

Stankov, A.; Ilyin, I.; Fridlund, C. V. M.

doi:10.1051/0004-6361:20031005

Cited by 6 publications

(2 citation statements)

References 12 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The sequences of calculated (solid curves) and observed (dots) profiles of the Si  4553 Å line for phases 0.239-0.664. (Stankov et al 2003). The line profiles have been convolved with the relevant instrumental profile.…”

Section: Line Profiles: Theory Vs Observationsmentioning

confidence: 99%

Hydrodynamic models for βCephei variables

Фокин

Mathias²,

Chapellier³

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract.A hydrodynamical model is generated for the high-amplitude β Cephei star BW Vulpeculae, and the spectral line profiles are calculated for different pulsational phases. The pulsational characteristics and line profiles are compared with recent observational data obtained during seven consecutive nights in August 2000. We found a generally good agreement in the basic photometric and spectral parameters. Two strong shock waves appear during one period, and the "stillstand" is due to the gas dynamics between the passages of these shocks. Note that this good agreement suppose a metallicity Z = 0.03, while a metallicity Z = 0.02 does not lead to the correct amplitudes and shapes of the curves.

show abstract

Section: Line Profiles: Theory Vs Observationsmentioning

confidence: 99%

Hydrodynamic models for βCephei variables

Фокин

Mathias²,

Chapellier³

et al. 2004

A&A

View full text Add to dashboard Cite

show abstract

“…Stankov et al () have obtained T eff = 23 850 ± 940 K, log g = 3.76 ± 0.04, and the projected rotational velocity, v sin i , of 24 km s −1 for this star. The log( L / L ⊙ ) = 4.1457 was obtained by Moskalik & Buchler ().…”

Section: Introductionmentioning

confidence: 73%

BW Vul: First results from magnetic field measurements in helium and hydrogen lines

2017

View full text Add to dashboard Cite

show abstract

Magnetic field measurements and wind-line variability of OB-type stars

Schnerr

Henrichs

Neiner

et al. 2008

A&A

View full text Add to dashboard Cite

Context. The first magnetic fields in O-and B-type stars that do not belong to the Bp-star class, have been discovered. The cyclic UV wind-line variability, which has been observed in a significant fraction of early-type stars, is likely to be related to such magnetic fields. Aims. We attempt to improve our understanding of massive-star magnetic fields, and observe twenty-five carefully-selected, OB-type stars. Methods. Of these stars we obtain 136 magnetic field strength measurements. We present the UV wind-line variability of all selected targets and summarise spectropolarimetric observations acquired using the MUSICOS spectropolarimeter, mounted at the TBL, Pic du Midi, between December 1998 and November 2004. From the average Stokes I and V line profiles, derived using the LSD method, we measure the magnetic field strengths, radial velocities, and first moment of the line profiles. Results. No significant magnetic field is detected in any OB-type star that we observed. Typical 1σ errors are between 15 and 200 G. A possible magnetic-field detection for the O9V star 10 Lac remains uncertain, because the field measurements depend critically on the fringe-effect correction in the Stokes V spectra. We find excess emission in UV-wind lines, centred about the rest wavelength, to be a new indirect indicator of the presence of a magnetic field in early B-type stars. The most promising candidates to host magnetic fields are the B-type stars δ Cet and 6 Cep, and a number of O stars. Conclusions. Although some O and B stars have strong dipolar field, which cause periodic variability in the UV wind-lines, such strong fields are not widespread. If the variability observed in the UV wind-lines of OB stars is generally caused by surface magnetic fields, these fields are either weak ( < ∼ few hundred G) or localised.

show abstract

Abundances and radial velocity analysis of BW Vulpeculae

Cited by 6 publications

References 12 publications

Hydrodynamic models for βCephei variables

Hydrodynamic models for βCephei variables

BW Vul: First results from magnetic field measurements in helium and hydrogen lines

Magnetic field measurements and wind-line variability of OB-type stars

Contact Info

Product

Resources

About