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Wamsteker, W.; Skillen, I.; Ponz, J. D.; Fuente, Anton de la; Barylak, M.; Yurrita, I.

doi:10.1023/a:1002780814330

Cited by 34 publications

(20 citation statements)

References 4 publications

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“…However, to construct a consistent picture and to understand the underlying physical processes in T CrB better, simultaneous UV and optical spectral observations during future active phases are needed. Space observatories offering simultaneous optical/UV spectroscopic capabilities like Kronos (Peterson et al 2001) and WSO/UV (Wamsteker & Ponz 2001) would be a good solution.…”

Section: Discussionmentioning

confidence: 99%

Hα variability of the recurrent nova T Coronae Borealis

Stanishev

Zamanov

Tomov

et al. 2004

A&A

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Abstract.We analyze Hα observations of the recurrent nova T CrB obtained during the last decade. For the first time the Hα emission profile is analyzed after subtraction of the red giant contribution. Based on our new radial velocity measurements of the Hα emission line we estimate the component masses of T CrB. It is found that the hot component is most likely a massive white dwarf. We estimate the inclination and the component masses to be i 67 • , M WD 1.37 ± 0.13 M and M RG 1.12 ± 0.23 M , respectively. The radial velocity of the central dip in the Hα profile changes nearly in phase with that of the red giant's absorption lines. This suggests that the dip is most likely produced by absorption in the giant's wind. Our observations cover an interval when the Hα and the U-band flux vary by a factor of ∼6, while the variability in B and V is much smaller. Based on our observations, and archival ultraviolet and optical data we show that the optical, ultraviolet and Hα fluxes strongly correlate. We argue that the presence of an accretion disc can account for most of the observed properties of T CrB.

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Section: Discussionmentioning

confidence: 99%

Hα variability of the recurrent nova T Coronae Borealis

Stanishev

Zamanov

Tomov

et al. 2004

A&A

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“…Adelman et al (1989), Breger (1976), Alekseeva et al (1996), Burnashev (1985) and Glushneva et al (1992) covering the near-UV, visual, and near-IR wavelengths. The code can additionally use data from the Space Telescope Imaging Spectrograph (STIS, Hubble Space Telescope; Woodgate et al 1998), the International Ultraviolet Explorer (IUE; Wamsteker et al 2000), and the Ultraviolet Sky Survey Telescope (TD1; Boksenberg et al 1973;Thompson et al 1978). These archives cover the ultraviolet part of SED.…”

Section: Effective Temperature From Sedmentioning

confidence: 99%

Spectroscopic survey of γ Doradus stars – I. Comprehensive atmospheric parameters and abundance analysis of γ Doradus stars

Aliçavuş

Niemczura

Cat

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a spectroscopic survey of known and candidate γ Doradus stars. The high-resolution, high signal-to-noise spectra of 52 objects were collected by five different spectrographs. The spectral classification, atmospheric parameters (T eff , log g, ξ), v sin i and chemical composition of the stars were derived. The stellar spectral and luminosity classes were found between G0-A7 and IV-V, respectively. The initial values for T eff and log g were determined from the photometric indices and spectral energy distribution. Those parameters were improved by the analysis of hydrogen lines. The final values of T eff , log g and ξ were derived from the iron lines analysis. The T eff values were found between 6000 K and 7900 K, while log g values range from 3.8 to 4.5 dex. Chemical abundances and v sin i values were derived by the spectrum synthesis method. The v sin i values were found between 5 and 240 km s −1 . The chemical abundance pattern of γ Doradus stars were compared with the pattern of non-pulsating stars. It turned out that there is no significant difference in abundance patterns between these two groups. Additionally, the relations between the atmospheric parameters and the pulsation quantities were checked. A strong correlation between the v sin i and the pulsation periods of γ Doradus variables was obtained. The accurate positions of the analysed stars in the H-R diagram have been shown. Most of our objects are located inside or close to the blue edge of the theoretical instability strip of γ Doradus.

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“…The BeSS database has been initially filled with Be star spectra available in various other spectral databases, such as the Elodie archive (http://atlas.obs-hp.fr/elodie; Moultaka et al 2004) of the OHP (Observatoire de Haute-Provence), the GAUDI database (http://sdc.laeff.inta.es/gaudi/; Solano et al 2005) of the ground-based preparatory work of the CoRoT satellite which includes data from Elodie, SARG, and Feros, and the INES database (http://sdc.laeff.inta.es/ines; Wamsteker et al 2000) of the IUE satellite. Some additional spectra have already been added by individual PIs and the database currently contains over 54,000 spectra concerning 626 different Be stars among the 2027 known Be stars in the catalog.…”

Section: Spectra In the Bess Databasementioning

confidence: 99%

THE Be STAR SPECTRA (BeSS) DATABASE

Neiner

Batz

Cochard³

et al. 2011

The Astronomical Journal

119

102

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Be stars vary on many timescales, from hours to decades. A long time base of observations to analyze certain phenomena in these stars is therefore necessary. Collecting all existing and future Be star spectra into one database has thus emerged as an important tool for the Be star community. Moreover, for statistical studies, it is useful to have centralized information on all known Be stars via an up-to-date catalog. These two goals are what the Be Star Spectra (BeSS, http://basebe.obspm.fr) database proposes to achieve. The database contains an as-completeas-possible catalog of known Be stars with stellar parameters, as well as spectra of Be stars from all origins (any wavelength, any epoch, any resolution, etc.). It currently contains over 54,000 spectra of more than 600 different Be stars among the ∼2000 Be stars in the catalog. A user can access and query this database to retrieve information on Be stars or spectra.

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Cited by 34 publications

References 4 publications

Hα variability of the recurrent nova T Coronae Borealis

Hα variability of the recurrent nova T Coronae Borealis

Spectroscopic survey of γ Doradus stars – I. Comprehensive atmospheric parameters and abundance analysis of γ Doradus stars

THE Be STAR SPECTRA (BeSS) DATABASE

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