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Evolution of magnetic field of massive stars. / Medvedev, A. S.; Kholtygin, A. F.; Hubrig, S.; Fabrika, S. N.; Valyavin, G. G.; Schöller, M.; Tsiopa, O. A.

In: Contributions of the Astronomical Observatory Skalnate Pleso, Vol. 48, No. 1, 01.01.2018, p. 223-227.

Research output: Contribution to journal › Article › peer-review

Harvard

Medvedev, AS, Kholtygin, AF, Hubrig, S, Fabrika, SN, Valyavin, GG, Schöller, M & Tsiopa, OA 2018, 'Evolution of magnetic field of massive stars', Contributions of the Astronomical Observatory Skalnate Pleso, vol. 48, no. 1, pp. 223-227.

APA

Medvedev, A. S., Kholtygin, A. F., Hubrig, S., Fabrika, S. N., Valyavin, G. G., Schöller, M., & Tsiopa, O. A. (2018). Evolution of magnetic field of massive stars. Contributions of the Astronomical Observatory Skalnate Pleso, 48(1), 223-227.

Vancouver

Medvedev AS, Kholtygin AF, Hubrig S, Fabrika SN, Valyavin GG, Schöller M et al. Evolution of magnetic field of massive stars. Contributions of the Astronomical Observatory Skalnate Pleso. 2018 Jan 1;48(1):223-227.

Author

Medvedev, A. S. ; Kholtygin, A. F. ; Hubrig, S. ; Fabrika, S. N. ; Valyavin, G. G. ; Schöller, M. ; Tsiopa, O. A. / Evolution of magnetic field of massive stars. In: Contributions of the Astronomical Observatory Skalnate Pleso. 2018 ; Vol. 48, No. 1. pp. 223-227.

BibTeX

@article{318723d698174016b16b2a9ce87083b9,
title = "Evolution of magnetic field of massive stars",
abstract = "We model the evolution of massive magnetic stars in the Galaxy using our own population synthesis code. A comparison of our model magnetic field distribution with that obtained from an analysis of measurements of magnetic fields shows that both model and real distributions can be approximated by a log-normal law with a mean log(B) =2.5. Based on this comparison we conclude that the magnetic flux variations of OBA stars on the main sequence (MS) are very slow. The shape of the magnetic field distribution for O, B and A stars appeared to be similar. This means that the mechanisms of the generation of their magnetic field are probably identical.",
keywords = "Stars: early type, Stars: evolution, Stars: magnetic field",
author = "Medvedev, {A. S.} and Kholtygin, {A. F.} and S. Hubrig and Fabrika, {S. N.} and Valyavin, {G. G.} and M. Sch{\"o}ller and Tsiopa, {O. A.}",
year = "2018",
month = jan,
day = "1",
language = "English",
volume = "48",
pages = "223--227",
journal = "Contributions of the Astronomical Observatory Skalnate Pleso",
issn = "1335-1842",
publisher = "Astronomical Institute, Slovak Academy of Sciences",
number = "1",

}

RIS

TY - JOUR

T1 - Evolution of magnetic field of massive stars

AU - Medvedev, A. S.

AU - Kholtygin, A. F.

AU - Hubrig, S.

AU - Fabrika, S. N.

AU - Valyavin, G. G.

AU - Schöller, M.

AU - Tsiopa, O. A.

PY - 2018/1/1

Y1 - 2018/1/1

N2 - We model the evolution of massive magnetic stars in the Galaxy using our own population synthesis code. A comparison of our model magnetic field distribution with that obtained from an analysis of measurements of magnetic fields shows that both model and real distributions can be approximated by a log-normal law with a mean log(B) =2.5. Based on this comparison we conclude that the magnetic flux variations of OBA stars on the main sequence (MS) are very slow. The shape of the magnetic field distribution for O, B and A stars appeared to be similar. This means that the mechanisms of the generation of their magnetic field are probably identical.

AB - We model the evolution of massive magnetic stars in the Galaxy using our own population synthesis code. A comparison of our model magnetic field distribution with that obtained from an analysis of measurements of magnetic fields shows that both model and real distributions can be approximated by a log-normal law with a mean log(B) =2.5. Based on this comparison we conclude that the magnetic flux variations of OBA stars on the main sequence (MS) are very slow. The shape of the magnetic field distribution for O, B and A stars appeared to be similar. This means that the mechanisms of the generation of their magnetic field are probably identical.

KW - Stars: early type

KW - Stars: evolution

KW - Stars: magnetic field

UR - http://www.scopus.com/inward/record.url?scp=85042682736&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:85042682736

VL - 48

SP - 223

EP - 227

JO - Contributions of the Astronomical Observatory Skalnate Pleso

JF - Contributions of the Astronomical Observatory Skalnate Pleso

SN - 1335-1842

IS - 1

ER -

ID: 27739349