Access to Astronomical Catalogues

← Click to display the menu
J/A+A/526/A116      W Virginis high-resolution spectra       (Kovtyukh+, 2011)

Neutral and ionized emission lines in the Type II Cepheid W Virginis Kovtyukh V.V., Wallerstein G., Andrievsky S.M., Gillet D., Fokin A.B., Templeton M., Henden A.A. <Astron. Astrophys. 526, A116 (2011)> =2011A&A...526A.116K
ADC_Keywords: Stars, variable ; Spectroscopy Keywords: stars: atmospheres - stars: variables: Cepheids Abstract: The aim of this work was to perform a multiphase spectroscopic study of W Vir which represents stars of the class of Population II cepheids, in order to trace the behaviour of emission features in different lines, and to use the data to describe the dynamical processes in the atmosphere of this star associated with the shock wave propagation. Description: Our spectroscopic study of W Vir involved 18 high-resolution spectra obtained with the help of 3.5-m telescope of Apache Point Observatory. These spectra cover W Vir's pulsational cycle with good phase resolution that enabled us to precisely fix the intervals of appearance, existence and disappearance of many anomalous spectral features, as well as to construct their radial velocity curves. We detected and investigated the behaviour of emission and line doubling in many metallic lines (NaI, FeI, FeII, BaII etc), as well as in hydrogen and helium lines. Analysis of the temporal characteristics of those emission features allowed us to make, in particular, the following conclusion. W Vir consists of two parts: the inner part, which is, in fact, a pulsating star itself with periodic shocks penetrating into the upper atmosphere, an outer one - a circumstellar envelope. The interaction of the main shock wave with the infalling envelope layers can explain the observed peculiarities of the spectral line variability. Objects: ------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------- 13 26 02.0 -03 22 43 W Vir = HD 116802 ------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 52 196 Emission lines at phase φ=0.666 tablea1.tex 73 259 LaTeX version of tablea1 sp/02_02_22.dat 16 54810 2002/02/22 spectrum sp/02_03_02.dat 16 52120 2002/03/02 spectrum sp/06_01_20.dat 16 54574 2006/01/20 spectrum sp/06_01_23.dat 16 56351 2006/01/23 spectrum sp/06_01_27.dat 16 52922 2006/01/27 spectrum sp/06_06_12.dat 16 56522 2006/06/12 spectrum
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm lambda Wavelength 10- 14 A5 --- Ion Element 17- 20 I4 --- Mult ? Multiplet number 23- 25 I3 0.1pm EW Equivalent width 29- 32 F4.2 eV Elow Excitation potential for the lower level 35- 36 I2 --- glow Statistical weight for the lower level 39- 40 I2 --- gup Statistical weight for the upper level 43- 46 F4.2 eV Eup Excitation potential for the upper level 49- 52 F4.2 [-] logA Logarithm of the emission transition probability
Byte-by-byte Description of file: sp/*
Bytes Format Units Label Explanations
3- 10 F8.3 0.1nm lambda Wavelength 12- 16 F5.3 --- RFlux Relative flux
Acknowledgements: V. Kovtyukh, val(at)deneb1.odessa.ua
(End) Patricia Vannier [CDS] 10-Jan-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact