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Line profile variability of OB stars : Pulsation, rotation, clumps and magnetic fields. / Kholtygin, A. F.; Fabrika, S. N.; Chountonov, G. A.; Burlakova, T. E.; Valyavin, G. G.; Kang, Dong Il.

In: Astronomische Nachrichten, Vol. 328, No. 10, 01.10.2007, p. 1170-1172.

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

Harvard

Kholtygin, AF, Fabrika, SN, Chountonov, GA, Burlakova, TE, Valyavin, GG & Kang, DI 2007, 'Line profile variability of OB stars: Pulsation, rotation, clumps and magnetic fields', Astronomische Nachrichten, vol. 328, no. 10, pp. 1170-1172. https://doi.org/10.1002/asna.200710878

APA

Kholtygin, A. F., Fabrika, S. N., Chountonov, G. A., Burlakova, T. E., Valyavin, G. G., & Kang, D. I. (2007). Line profile variability of OB stars: Pulsation, rotation, clumps and magnetic fields. Astronomische Nachrichten, 328(10), 1170-1172. https://doi.org/10.1002/asna.200710878

Vancouver

Kholtygin AF, Fabrika SN, Chountonov GA, Burlakova TE, Valyavin GG, Kang DI. Line profile variability of OB stars: Pulsation, rotation, clumps and magnetic fields. Astronomische Nachrichten. 2007 Oct 1;328(10):1170-1172. https://doi.org/10.1002/asna.200710878

Author

Kholtygin, A. F. ; Fabrika, S. N. ; Chountonov, G. A. ; Burlakova, T. E. ; Valyavin, G. G. ; Kang, Dong Il. / Line profile variability of OB stars : Pulsation, rotation, clumps and magnetic fields. In: Astronomische Nachrichten. 2007 ; Vol. 328, No. 10. pp. 1170-1172.

BibTeX

@article{2db74831d734421886ca09048c724b0f,
title = "Line profile variability of OB stars: Pulsation, rotation, clumps and magnetic fields",
abstract = "The variability of line profiles in spectra of bright OB stars has been studied. We obtain more than 1000 high quality spectra of δ Ori A, λ Ori A, α Cam, 19 Cep, l Her, ρ Leo and other target stars. We revealed the line profile microvariability of small amplitude (0.5-3% in the adjacent continuum units) for all observed stars. For most stars only cyclic components of the line profile variability (LPV) at the time scales from hours to days were detected. These components seem to be connected with both the non-radial pulsations (NRP) and rotation line profile modulation. In the spectra of δ Ori A and λ Ori A we found the evidences of the stochastic LPV in spectra, probably connected with the small clumps in the stellar wind. On the basis of recent observations we discuss the origin of the magnetic field of early-type stars.",
keywords = "Stars: atmospheres, Stars: magnetic fields, Stars: winds, outflows",
author = "Kholtygin, {A. F.} and Fabrika, {S. N.} and Chountonov, {G. A.} and Burlakova, {T. E.} and Valyavin, {G. G.} and Kang, {Dong Il}",
year = "2007",
month = oct,
day = "1",
doi = "10.1002/asna.200710878",
language = "English",
volume = "328",
pages = "1170--1172",
journal = "Astronomische Nachrichten",
issn = "0004-6337",
publisher = "Wiley-Blackwell",
number = "10",

}

RIS

TY - JOUR

T1 - Line profile variability of OB stars

T2 - Pulsation, rotation, clumps and magnetic fields

AU - Kholtygin, A. F.

AU - Fabrika, S. N.

AU - Chountonov, G. A.

AU - Burlakova, T. E.

AU - Valyavin, G. G.

AU - Kang, Dong Il

PY - 2007/10/1

Y1 - 2007/10/1

N2 - The variability of line profiles in spectra of bright OB stars has been studied. We obtain more than 1000 high quality spectra of δ Ori A, λ Ori A, α Cam, 19 Cep, l Her, ρ Leo and other target stars. We revealed the line profile microvariability of small amplitude (0.5-3% in the adjacent continuum units) for all observed stars. For most stars only cyclic components of the line profile variability (LPV) at the time scales from hours to days were detected. These components seem to be connected with both the non-radial pulsations (NRP) and rotation line profile modulation. In the spectra of δ Ori A and λ Ori A we found the evidences of the stochastic LPV in spectra, probably connected with the small clumps in the stellar wind. On the basis of recent observations we discuss the origin of the magnetic field of early-type stars.

AB - The variability of line profiles in spectra of bright OB stars has been studied. We obtain more than 1000 high quality spectra of δ Ori A, λ Ori A, α Cam, 19 Cep, l Her, ρ Leo and other target stars. We revealed the line profile microvariability of small amplitude (0.5-3% in the adjacent continuum units) for all observed stars. For most stars only cyclic components of the line profile variability (LPV) at the time scales from hours to days were detected. These components seem to be connected with both the non-radial pulsations (NRP) and rotation line profile modulation. In the spectra of δ Ori A and λ Ori A we found the evidences of the stochastic LPV in spectra, probably connected with the small clumps in the stellar wind. On the basis of recent observations we discuss the origin of the magnetic field of early-type stars.

KW - Stars: atmospheres

KW - Stars: magnetic fields

KW - Stars: winds, outflows

UR - http://www.scopus.com/inward/record.url?scp=38049187644&partnerID=8YFLogxK

U2 - 10.1002/asna.200710878

DO - 10.1002/asna.200710878

M3 - Article

AN - SCOPUS:38049187644

VL - 328

SP - 1170

EP - 1172

JO - Astronomische Nachrichten

JF - Astronomische Nachrichten

SN - 0004-6337

IS - 10

ER -

ID: 36161222