Standard

Rapid Spectral Variability of ε Per A. / Dushin, V.V.; Kholtygin, A.F.; Chuntonov, G.A.; Kudryavtsev, D.O.

в: Astrophysical Bulletin, Том 68, № 2, 2013, стр. 184-195.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Dushin, VV, Kholtygin, AF, Chuntonov, GA & Kudryavtsev, DO 2013, 'Rapid Spectral Variability of ε Per A', Astrophysical Bulletin, Том. 68, № 2, стр. 184-195. https://doi.org/10.1134/S1990341313020065

APA

Dushin, V. V., Kholtygin, A. F., Chuntonov, G. A., & Kudryavtsev, D. O. (2013). Rapid Spectral Variability of ε Per A. Astrophysical Bulletin, 68(2), 184-195. https://doi.org/10.1134/S1990341313020065

Vancouver

Dushin VV, Kholtygin AF, Chuntonov GA, Kudryavtsev DO. Rapid Spectral Variability of ε Per A. Astrophysical Bulletin. 2013;68(2):184-195. https://doi.org/10.1134/S1990341313020065

Author

Dushin, V.V. ; Kholtygin, A.F. ; Chuntonov, G.A. ; Kudryavtsev, D.O. / Rapid Spectral Variability of ε Per A. в: Astrophysical Bulletin. 2013 ; Том 68, № 2. стр. 184-195.

BibTeX

@article{97b0ea0d57ee41a3a0ef1f435c64483d,
title = "Rapid Spectral Variability of ε Per A",
abstract = "The results of high-resolution spectropolarimetric observations (R = 60 000) of the B0.5-type subgiant εPerA are reported. Regular components of line profile variations with the frequencies 3.82–12.99 d−1 are found. A possible relation between the non-radial pulsations of the star and the observed regular variations of the line profiles is shown. A wavelet analysis of the difference of line profiles in the spectrum of ε Per A is performed. The amplitude of the wavelet spectrum is found to have two maxima at 10–20 and 50–60 km/s velocity scales. It is suggested that the first maximum corresponds to the amplitude of fluctuations in the velocity field of large-scale motions in the non-radially pulsating photosphere of the star, whereas the second maximum is associated with the variation of the halfwidths of spectral line profiles. An upper limit for the effective magnetic field of the star is inferred.",
author = "V.V. Dushin and A.F. Kholtygin and G.A. Chuntonov and D.O. Kudryavtsev",
year = "2013",
doi = "10.1134/S1990341313020065",
language = "English",
volume = "68",
pages = "184--195",
journal = "Astrophysical Bulletin",
issn = "1990-3413",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "2",

}

RIS

TY - JOUR

T1 - Rapid Spectral Variability of ε Per A

AU - Dushin, V.V.

AU - Kholtygin, A.F.

AU - Chuntonov, G.A.

AU - Kudryavtsev, D.O.

PY - 2013

Y1 - 2013

N2 - The results of high-resolution spectropolarimetric observations (R = 60 000) of the B0.5-type subgiant εPerA are reported. Regular components of line profile variations with the frequencies 3.82–12.99 d−1 are found. A possible relation between the non-radial pulsations of the star and the observed regular variations of the line profiles is shown. A wavelet analysis of the difference of line profiles in the spectrum of ε Per A is performed. The amplitude of the wavelet spectrum is found to have two maxima at 10–20 and 50–60 km/s velocity scales. It is suggested that the first maximum corresponds to the amplitude of fluctuations in the velocity field of large-scale motions in the non-radially pulsating photosphere of the star, whereas the second maximum is associated with the variation of the halfwidths of spectral line profiles. An upper limit for the effective magnetic field of the star is inferred.

AB - The results of high-resolution spectropolarimetric observations (R = 60 000) of the B0.5-type subgiant εPerA are reported. Regular components of line profile variations with the frequencies 3.82–12.99 d−1 are found. A possible relation between the non-radial pulsations of the star and the observed regular variations of the line profiles is shown. A wavelet analysis of the difference of line profiles in the spectrum of ε Per A is performed. The amplitude of the wavelet spectrum is found to have two maxima at 10–20 and 50–60 km/s velocity scales. It is suggested that the first maximum corresponds to the amplitude of fluctuations in the velocity field of large-scale motions in the non-radially pulsating photosphere of the star, whereas the second maximum is associated with the variation of the halfwidths of spectral line profiles. An upper limit for the effective magnetic field of the star is inferred.

U2 - 10.1134/S1990341313020065

DO - 10.1134/S1990341313020065

M3 - Article

VL - 68

SP - 184

EP - 195

JO - Astrophysical Bulletin

JF - Astrophysical Bulletin

SN - 1990-3413

IS - 2

ER -

ID: 7375349