The General Catalog of Variable Stars (GCVS)

Samus, N. N.; Durlevich, O. V.; Kazarovets, E. V.

doi:10.1515/astro-1997-0229

Cited by 239 publications

(328 citation statements)

References 1 publication

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“…According to the GCVS (Samus et al 2009), there are 153 RV Tauri variables in our Galaxy and several have been found in the LMC and SMC (Alcock et al 1998;Soszyński et al 2008;Buchler et al 2009;Soszyñski et al 2010). In this paper, we focus on the Galactic sample.…”

Section: Introductionmentioning

confidence: 89%

“…These subclasses are indicated with letter a and b. The RVa stars have a constant mean magnitude, while the RVb stars have a varying mean magnitude on a time scale between 600 and 1500 days (Samus et al 2009). In addition to the photometric subclasses, RV Tauri stars are divided into three spectroscopic subclasses (Preston et al 1963).…”

Section: Introductionmentioning

confidence: 99%

“…Here, we present a systematic study of the IR properties of RV Tauri stars and we use all Galactic RV Tauri stars listed in the GCVS (Samus et al 2009) as our sample. The IR photometry is a good tracer of the temperature gradient of the circumstellar dust (if present), which we want to correlate with the properties of the central object.…”

Section: Introductionmentioning

confidence: 99%

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TheWISEview of RV Tauri stars

Gezer

Winckel

Bozkurt

et al. 2015

Mon. Not. R. Astron. Soc.

128

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We present a detailed study based on infrared photometry of all Galactic RV Tauri stars from the General Catalogue of Variable Stars (GCVS). RV Tauri stars are the brightest among the population II Cepheids. They are thought to evolve away from the asymptotic giant branch (AGB) towards the white dwarf domain. IRAS detected several RV Tauri stars because of their large IR excesses and it was found that they occupy a specific region in theWe used the all sky survey of WISE to extend these studies and compare the infrared properties of all RV Tauri stars in the GCVS with a selected sample of post-AGB objects with the goal to place the RV Tauri pulsators in the context of post-AGB evolution. Moreover, we correlated the IR properties of both the RV Tauri stars and the comparison sample with other observables like binarity and the presence of a photospheric chemical anomaly called depletion. We find that Galactic RV Tauri stars display a range of infrared properties and we differentiate between disc sources, objects with no IR excess and objects for which the spectral energy distribution (SED) is uncertain. We obtain a clear correlation between disc sources and binarity. RV Tauri stars with a variable mean magnitude are exclusively found among the disc sources. We also find evidence for disc evolution among the binaries. Furthermore our studies show that the presence of a disc seems to be a necessary but not sufficient condition for the depletion process to become efficient.

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Section: Introductionmentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

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TheWISEview of RV Tauri stars

Gezer

Winckel

Bozkurt

et al. 2015

Mon. Not. R. Astron. Soc.

128

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“…The most complete information on variable stars, including their coordinates, extensive cross-identification, photometry, spectral type, variability period, light-curve parameters, classification and detailed notes can be found in the General Catalogue of Variable Stars, GCVS (Samus et al 2013). It represents one of the largest databases on variables and lists about 50,000 variable stars in the Milky Way, as well as over 10,000 in other galaxies, and more than 25,000 suspected variables.…”

Section: Data On Variable Starsmentioning

confidence: 99%

Russian Virtual Observatory: Data Sources

et al. 2016

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Abstract. The purpose of this review is to analyze main directions of creation and functioning of major data sources developed by Russian astronomers or with their participation and to compare them with the worldwide trends in these fields. We discuss astronomical space missions of the past, present, and future (Astron, INTEGRAL, WSO-UV, Spectrum Roentgen Gamma, Lyra-B), high-quality photometric atlases and catalogues, and spectroscopic data sources, primarily VALD and the global VAMDC framework for the maintenance and distribution of atomic and molecular data. We describe collection, analysis, and dissemination of astronomical data on minor bodies of the Solar System and on variable stars. Also described is the project joining data for all observational types of binary and multiple stars, Binary star DataBase (BDB).

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“…In addition to the BSC, MSC and HIP we also used used the Eighth Spectroscopic Binary Catalog (BFM; Batten, Fletcher & McCarthy 1989), the Ninth... (SB9; Pourbaix et al2004), the Sixth USNO Catalog of Visual Binary Orbits (Hartkopf et al 2000), the CCDM catalog (Dommanget & Nys 2002) of close multiples (many of which however are optical rather than physical multiples), the GCVS (Samus et al 2004) on eclipsers and ellipsoidal variables, and the CHARA survey of speckle observations (McAlister et al 1989).…”

Section: Multiplicitymentioning

confidence: 99%

The Incidence of Multiplicity Among Bright Stellar Systems

2006

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Abstract.We consider the multiplicity of stellar systems with (combined) magnitude brighter than 6.00 in Hipparcos magnitudes. We identify 4555 such bright systems, and the frequencies of multiplicities 1, 2, . . . , 7 are found to be 2722, 1412, 299, 86, 22, 12 and 2. We also consider the distributions of periods of orbits and sub-orbits. For the even more restricted set of 474 systems with VH 4.00 the proportions of higher multiples up to sextuple are progressively larger, suggesting incompleteness in even the relatively well-studied larger sample.We construct a Monte-Carlo algorithm that will generate systems with roughly the observed multiplicities and orbital parameters, taking account of selection effects.

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The General Catalog of Variable Stars (GCVS)

Cited by 239 publications

References 1 publication

TheWISEview of RV Tauri stars

TheWISEview of RV Tauri stars

Russian Virtual Observatory: Data Sources

The Incidence of Multiplicity Among Bright Stellar Systems

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