Observation de la Raie Hα dans les Etoiles Be

Andrillat, Y.; Fehrenbach, Charles

doi:10.1007/978-94-009-8565-0_22

Cited by 29 publications

(56 citation statements)

References 3 publications

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“…To test for other Be star characteristics in δ Sco we checked for correlations between H alpha line parameters like v sin i vs. fullwidth, v sin i vs. halfwidth, peak to continuum intensity ratio vs. equivalent width etc. (Andrillat & Fehrenbach 1982;Banerjee et al 2000;Dachs et al 1986) and found it to exhibit standard Be star behaviour.…”

Section: Resultsmentioning

confidence: 99%

Near infra-red and optical spectroscopy of Delta Scorpii

Banerjee

Janardhan

Ashok

2001

A&A

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Abstract. Spectroscopic observations of δ Sco in the near IR and optical wavelengths, obtained shortly after its recent periastron passage are reported. The IR spectra are dominated by the HI Paschen and Brackett lines. An IR excess is seen which can be attributed to free-free emission from a circumstellar shell. The observed Paschen and Brackett line intensities deviate significantly from Case B predictions and indicate optical depth effects. These effects are modeled. The overall spectral behaviour of δ Sco at present is that of a typical Be star.

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Section: Resultsmentioning

confidence: 99%

Near infra-red and optical spectroscopy of Delta Scorpii

Banerjee

Janardhan

Ashok

2001

A&A

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“…Guo et al (1995) calculated the V/R ratio as (I V − 1)/(I R − 1), so their values are not used and the V/R ratio was calculated from the given peak intensities. -File G (Andrillat & Fehrenbach 1982): Four values of the Hα EW and V/R are given. However, Andrillat & Fehrenbach (1982) measured intensities of the emission from the underlying photospheric line.…”

Section: A2 Spectrophotometric Datamentioning

confidence: 99%

“…-File G (Andrillat & Fehrenbach 1982): Four values of the Hα EW and V/R are given. However, Andrillat & Fehrenbach (1982) measured intensities of the emission from the underlying photospheric line. Consequently, their V/R ratio is not comparable to the values used in this study.…”

Section: A2 Spectrophotometric Datamentioning

confidence: 99%

Properties and nature of Be stars

Ruždjak

Božić

Harmanec

et al. 2009

A&A

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Context. One way to understand the still mysterious Be phenomenon is to study the time variations of particular Be stars with a long observational history. ζ Tau is one obvious candidate. Aims. Using our rich series of spectral and photometric observations and a critical compilation of available radial velocities, spectrophotometry of Hα, and UBV photometry, we characterize the pattern of time variations of ζ Tau over about a century. Our goal is to find the true timescales of its variability and confront them with the existing models related to various aspects of the Be phenomenon. Methods. Spectral reductions were carried out using the IRAF and SPEFO programs. The HEC22 program was used for both photometric reductions and transformations to UBV. Orbital solutions were derived with the latest publicly available version of the program FOTEL, period analyses employed both the PDM and Fourier techniques -programs HEC27 and PERIOD04.

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“…Notes. The Hα peak intensities were measured by HB from the publicly available spectra from the C. Buil Castalet Tolosan Observatory and the BeSS database and from the plots of profiles published by Elias et al (1978), Barker (1983) and Andrillat & Fehrenbach (1982). We adopted the published values from Slettebak & Reynolds (1978), Slettebak et al (1992) and Banerjee et al (2000).…”

Section: Appendix A: Spectroscopymentioning

confidence: 99%

“…Hubert-Delplace & Hubert (1979) stated that o Cas was without emission from 1953to 1959. Between December 1975and November 1976, another emission episode started and continued through the early 1980's (Slettebak & Reynolds 1978;Andrillat & Fehrenbach 1982). In December 1982 the Hα emission reached an intensity of 2.0 relative to the continuum (Barker 1983).…”

Section: Introductionmentioning

confidence: 99%

Properties and nature of Be stars

Koubský

Hummel

Harmanec

et al. 2010

A&A

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The analysis of radial velocities of the Be star o Cas from spectra taken between 1992 and 2008 at the Ondřejov Observatory and the Dominion Astrophysical Observatory allowed us to reconfirm the binary nature of this object, first suggested by Abt and Levy in 1978, but later refuted by several authors. The orbital parameters of this SB1 system imply a very high mass function of about one solar mass. This in turn leads to a very high mass of the secondary, possibly higher than that of the primary. In order to look for such a massive secondary, o Cas was observed with the Navy Prototype Optical Interferometer, which allowed the binary components to be spatially resolved for the first time. The interferometric observations lead to the detection of a secondary, about 3 mag fainter than the primary. The possible properties of this peculiar binary system and the reasons why the massive secondary does not dominate the optical spectrum are discussed.

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Observation de la Raie Hα dans les Etoiles Be

Cited by 29 publications

References 3 publications

Near infra-red and optical spectroscopy of Delta Scorpii

Near infra-red and optical spectroscopy of Delta Scorpii

Properties and nature of Be stars

Properties and nature of Be stars

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