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Multi-site continuous spectroscopy .5. Rapid photospheric variability in the Be star 48 Persei from the MUSICOS 1989 campaign
Hubert, AM; Floquet, M; Hao, JX; Caillet, S; Catala, C; Foing, BH; Neff, JE; Huang, L; Hubert, H; Barban, C; Baudrand, J; Cao, H; Char, S; Chatzichristou, H; Cuby, JG; Czarny, J; Dreux, M; Felenbok, P; Guerin, J; Hron, J; Huovelin, J; Jankov, S; Jiang, S; LeContel, JM; Maitzen, HM; Petrov, P; Savanov, I; Shcherbakov, A; Simon, T; Stee, P; Tuominen, I; Zhai, D
1997-08-01
Source PublicationASTRONOMY & ASTROPHYSICS
Volume324Issue:3Pages:929-940
AbstractRapid variability in the photospheric He I 6678 line of the Be star 48 Per (HD 25940, HR 1273) has been detected from 258 high S/N CCD spectra taken with four 1.5-2.0 meter telescopes over three consecutive nights during the multisite spectroscopic MUSICOS 1989 campaign. 48 Per is a rather moderate-V sin i star, known to have presented slight long-term variations in the intensity of Balmer emission lines and in the V/R ratio. It is shown that the MUSICOS 1989 observations preceded a new activity phase. Search for line-profile variations, hereafter Ipv, was performed with time-series analysis using two methods (TF+CLEAN and Least-Squares) and with analysis of residuals. Weak blue-to-red and red-to-blue moving subfeatures with the same acceleration have been detected in the residuals. Their presence confirms that this star is seen under a moderate angle of inclination, i similar to 40 degrees, in agreement with estimates based on fundamental stellar parameters. A 6.04 c/d frequency, associated with the moving subfeatures mentioned above, has been firmly established from time-series analysis and corresponds more closely, in the frame of non-radial pulsations (NRP), to a tesseral mode (\m\ = l - 1 = 9 +/- 2). Two other possible frequencies (0.85 and 2.77 c/d) have been detected but need to be confirmed with new observations obtained over a longer time span. Despite additional spectra obtained at Haute Provence Observatory, we could not confirm the previous value of the orbital period or the amplitude of the radial velocity,curve of 48 Per, and therefore it was premature to search for tidally-forced oscillations.
KeywordLines: Profiles Stars: Emission-line Stars: Oscillations Be Stars: Individual 48 Per
Indexed BySCI
Language英语
WOS IDWOS:A1997XT42200021
Citation statistics
Cited Times:14[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/8107
Collection射电天文研究部
Affiliation1.OBSERV PARIS, URA 335 CNRS, F-92195 MEUDON, FRANCE
2.CHINESE ACAD SCI, BEIJING ASTRON OBSERV, BEIJING 100080, PEOPLES R CHINA
3.OBSERV MIDI PYRENEES, TOULOUSE, FRANCE
4.CNRS, INST ASTROPHYS SPATIALE, F-75700 PARIS, FRANCE
5.PENN STATE UNIV, UNIVERSITY PK, PA 16802 USA
6.OBSERV PARIS, DAEC, MEUDON, FRANCE
7.VIENNA OBSERV, VIENNA, AUSTRIA
8.UNIV HELSINKI, HELSINKI, FINLAND
9.UNIV HAWAII, HONOLULU, HI 96822 USA
Recommended Citation
GB/T 7714
Hubert, AM,Floquet, M,Hao, JX,et al. Multi-site continuous spectroscopy .5. Rapid photospheric variability in the Be star 48 Persei from the MUSICOS 1989 campaign[J]. ASTRONOMY & ASTROPHYSICS,1997,324(3):929-940.
APA Hubert, AM.,Floquet, M.,Hao, JX.,Caillet, S.,Catala, C.,...&Zhai, D.(1997).Multi-site continuous spectroscopy .5. Rapid photospheric variability in the Be star 48 Persei from the MUSICOS 1989 campaign.ASTRONOMY & ASTROPHYSICS,324(3),929-940.
MLA Hubert, AM,et al."Multi-site continuous spectroscopy .5. Rapid photospheric variability in the Be star 48 Persei from the MUSICOS 1989 campaign".ASTRONOMY & ASTROPHYSICS 324.3(1997):929-940.
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