Magnetic stars with wide depressions in the continuum. 2. The silicon star with a complex field structure HD 27404

Semenko, E. A.; Romanyuk, I. I.; Semenova, Ekaterina; Moiseeva, A. V.; Kudryavtsev, D. O.; Yakunin, I. A.

doi:10.1134/s1990341317040034

Cited by 8 publications

(3 citation statements)

References 20 publications

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“…To normalize the spectra to the continuum, the latter was interpolated by a cubic spline using the spectool package of the IRAF 1 environment. The process of the reduction of observations obtained at the MSS is described in more detail in the papers by Kudryavtsev (2000); Semenko et al (2017). The spectral resolution was approximately 15000 (the slit size 0 5), the obtained wavelength range was 4425-4982 Å, average .…”

Section: Basic Information On the Star Observations And Spectra Reductionmentioning

confidence: 99%

Super-Fast Line-Profile Variability in the Spectra of OBA Stars. IV: ζ Ori A

et al. 2021

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The present study continues the investigation of the super-fast variability of line profiles in the spectra of stars of early spectral types. We studied the line-profile variability in the spectrum of the binary (O9.7Ib+B0III) star Ori A using the MSS spectrograph of the 6-m BTA telescope based on observations carried out on February 19, 2019. Short-period regular variations of the hydrogen Balmer lines and He I lines with periods from 89 to 295 minutes were found. The presence of short-period variations in the period interval of 10-20 minutes is also possible. An analysis of the stellar brightness variations from observations by the TESS satellite showed the presence of seven regular components, one of which is probably the second harmonic of the rotation period of the main component of the Aa star Ori A. The magnetic field of the star was determined for the whole series of observations. The longitudinal component of the root-mean-square magnetic field measured by the regression method over the whole observation period is G.

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Section: Basic Information On the Star Observations And Spectra Reductionmentioning

confidence: 99%

Super-Fast Line-Profile Variability in the Spectra of OBA Stars. IV: ζ Ori A

et al. 2021

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“…When performing wavelength calibration for the series of spectra, we used the nearest in time ThAr lamp spectrum. To normalize the spectra to the continuum, the latter was interpolated by a cubic spline using the "spectool"package in the IRAF 2 described in more detail by Kudryavtsev et al [21] and Semenko et al [22]. The spectral resolution amounts to about 15000 (slit size 0 .…”

Section: Observations and Reduction Of Spectramentioning

confidence: 99%

Superfast Line Profile Variations in the Spectra of OBA Stars. III. A0 Star α2 Cvn, New Results

et al. 2020

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This work is a continuation of the studies of the ultrafast variability of line profiles in the spectra of early-type stars. Line profile variations (LPVs) in the spectrum a chemically peculiar A0Vp star α 2 CVn are investigated using the January 6, 2020 observations carried out with the 6-meter BTA telescope at Special Astrophysical observatory (SAO) of the Russian Academy of Sciences (RAS) equipped with the MSS spectrograph. Regular shortterm periodic variations of the H β , Fe II, and Cr II lines were detected with periods ranging from ∼4 to ∼140 minutes. The magnetic field of the star was determined for all observations. The average measured longitudinal magnetic field component over the entire duration of observations is about ≈600 G, which is close to the value expected from the well-known magnetic field phase curve.

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“…The observational technique and data reduction had been demonstrated in multiple papers (e.g. Kudryavtsev et al 2006;Romanyuk et al 2017;Semenko et al 2017).…”

Section: Observational Materialsmentioning

confidence: 99%

Binary Stars in the Orion OB1 Association, Subgroup $\textit{a}$

Semenko,

Romanyuk,

Yakunin

et al. 2019

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A detailed spectroscopic survey of chemically peculiar (CP) stars in the Orion OB1 association is the most comprehensive observational program in the field of stellar magnetism that has been carried out at SAO so far. As at the end of 2018, we have completed surveying CP stars in the oldest subgroup a of the association. In this paper we give a short overview of CP members of the subgroup showing both direct and indirect signatures of multiplicity. Among the overall 11 stars which had been classified as peculiar, we found several good candidates for further detailed study.

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Magnetic stars with wide depressions in the continuum. 2. The silicon star with a complex field structure HD 27404

Cited by 8 publications

References 20 publications

Super-Fast Line-Profile Variability in the Spectra of OBA Stars. IV: ζ Ori A

Super-Fast Line-Profile Variability in the Spectra of OBA Stars. IV: ζ Ori A

Superfast Line Profile Variations in the Spectra of OBA Stars. III. A0 Star α2 Cvn, New Results

Binary Stars in the Orion OB1 Association, Subgroup $\textit{a}$

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