J/MNRAS/372/1804 Magnetic fields of chem. peculiar stars (Kudryavtsev+, 2006)
New magnetic chemically peculiar stars.
Kudryavtsev D.O., Romanyuk I.I., Elkin V.G., Paunzen E.
<Mon. Not. R. Astron. Soc., 372, 1804-1828 (2006)>
=2006MNRAS.372.1804K 2006MNRAS.372.1804K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, Ap; Stars, Bp ; Stars, peculiar ; Stars, standard ;
Magnetic fields
Keywords: stars: chemically peculiar - stars: magnetic fields - stars: rotation
Abstract:
Spectropolarimetric observations of 96 chemically peculiar (CP)
main-sequence stars have been carried out at the 6-m telescope at the
Special Astrophysical Observatory of the Russian Academy of Sciences
(SAO RAS) with the aim of searching for the presence of stellar
magnetic fields. The stars selected for investigation were CP stars
known to have strong anomalies in the wavelength region of the
continuum flux depression around λ 5200Å. This selection was
conducted with the aid of low-resolution spectral observations, made
with the SAO RAS 1-m telescope, and of published differential
photometric data. Magnetic fields have been successfully detected in
72 stars of which only three stars were previously known to have
magnetic fields. For two stars, the longitudinal component of the
magnetic field Beexceeds 5kG: HD178892 - 7.4kG, and HD258686
- 6.7kG. We failed to reliably detect the magnetic field in the other
24 CP stars. These stars are mostly fast rotators, a feature which
hampers accurate measurements of Be. It is demonstrated in
this paper that selecting candidate magnetic stars by considering
their photometric indices Z or Δalpha, or alternatively,
by inspecting low-resolution spectra around the λ5200Å flux
depression, considerably increases the detection rate.
Description:
Data was obtained at the Main Stellar Spectrograph of the Russian 6-m
telescope. We got 438 zeeman spectra for 93 CP stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sources.dat 38 93 Studied sources
table3.dat 42 438 Individual measurements of the longitudinal
magnetic field, Be, for new magnetic stars
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Byte-by-byte Description of file: sources.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Name
13- 14 I2 h RAh Simbad right ascension (J2000)
16- 17 I2 min RAm Simbad right ascension (J2000)
19- 23 F5.2 s RAs Simbad right ascension (J2000)
25 A1 --- DE- Simbad declination sign (J2000)
26- 27 I2 deg DEd Simbad declination (J2000)
29- 30 I2 arcmin DEm Simbad declination (J2000)
32- 35 F4.1 arcsec DEs Simbad declination (J2000)
37- 38 I2 --- N Number of measurements in table3.dat
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name BD or ND name
14- 24 F11.3 d JD Julian Date
27- 29 I3 --- S/N Signal-to-noise ratio
32- 36 I5 gauss Be Longitudinal magnetic field, measured by the
standard Babcock method
39- 42 I4 gauss e_Be rms uncertainty on magnetic field
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Acknowledgements:
Anastasiya Moiseeva, agreana(at)mail.ru
(End) Anastasiya Moiseeva [RAS], Patricia Vannier [CDS] 13-Oct-2020