Access the full text.
Sign up today, get DeepDyve free for 14 days.
S. Wolff, G. Preston (1978)
Late B-type stars: rotation and the incidence of HgMn stars.Astrophysical Journal Supplement Series, 37
G. Catanzaro, F. Leone, F. Catalano (1998)
Variability of the Hei5876 Å line in early type chemically peculiar starsAstronomy & Astrophysics Supplement Series, 134
D. Hube, G. Aikman (2015)
Publications of the Astronomical Society of the Pacific 103: 49-62, January 1991 3 VULPECULAE: A NONRADIAL PULSATOR IN A ONE-YEAR BINARY SYSTEM
Robert Jr., W. Kubinec, A. Kubinec, S. Adelman (2003)
A Photometric and Spectroscopic Study of 3 Vulpeculae: An Observer’s NightmareThe Astronomical Journal, 126
D. Hoffleit, C. Jaschek (1982)
The Bright Star Catalogue
E. Fitzpatrick, D. Massa (2004)
Determining the Physical Properties of the B Stars. II. Calibration of Synthetic PhotometryThe Astronomical Journal, 129
S. Hubrig, M. Briquet, M. Schoeller, P. Cat, G. Mathys, C. Aerts (2006)
Discovery of magnetic fields in the βCephei star ξ1 CMa and in several slowly pulsating B starsMonthly Notices of the Royal Astronomical Society, 369
S. Vauclair, J. Hardorp, D. Peterson (1979)
Silicon levitation in chemically peculiar stars and the oblique rotator modelThe Astrophysical Journal, 227
J. Lesh (1968)
The Kinematics of the Gould Belt: an Expanding Group?Astrophysical Journal Supplement Series, 17
P. Mathias, C. Aerts, M. Briquet, P. Cat, J. Cuypers, H. Winckel, J. Contel (2001)
Spectroscopic monitoring of 10 new northern slowly pulsating B star candidates discovered from the HIPPARCOS missionAstronomy and Astrophysics, 379
A. Shavrina, Y. Glagolevskij, J. Silvester, J. Silvester, G. Chuntonov, V. Khalack, Y. Pavlenko (2009)
Spots structure and stratification of helium and silicon in the atmosphere of He-weak star HD 21699Monthly Notices of the Royal Astronomical Society, 401
F. Kupka, N. Piskunov, T. Ryabchikova, H. Stempels, W. Weiss (1999)
VALD{2: Progress of the Vienna Atomic Line Data Base ?Astronomy & Astrophysics Supplement Series, 138
The star HD182255 reveals spectral variability in rotation, irregular short-term variability, as well as long-term variations in the spectra. The He and Si abundances vary in antiphase. According to the theory, silicon accumulates in the regions between the poles, where the field lines are horizontal. Hence the observed behavior of He and Si may indicate the presence of magnetic field, where one of the poles passes through the central meridian in phase Φ = 0 as the star rotates. Given a general weakening of He over the entire surface, in Φ = 0 its abundance is higher, which may be linked with the presence of wind from the magnetic pole. The star definitely belongs to the He-w type. The study of the structure of the upper atmosphere based on the hydrogen line profiles shows that it varies over the years. Our estimates of the magnetic field from the Zeeman spectra are within the measurement errors. According to the spectroscopic characteristics the star can be considered weakly magnetic.
Astrophysical Bulletin – Springer Journals
Published: May 24, 2011
Read and print from thousands of top scholarly journals.
Already have an account? Log in
Bookmark this article. You can see your Bookmarks on your DeepDyve Library.
To save an article, log in first, or sign up for a DeepDyve account if you don’t already have one.
Copy and paste the desired citation format or use the link below to download a file formatted for EndNote
Access the full text.
Sign up today, get DeepDyve free for 14 days.
All DeepDyve websites use cookies to improve your online experience. They were placed on your computer when you launched this website. You can change your cookie settings through your browser.