Spectroscopic and photometric observations of the short-period RS CVn-type star ER Vulpeculae

Kjurkchieva, D.; Marchev, D.; Zoła, S.

doi:10.1051/0004-6361:20030489

Cited by 14 publications

(12 citation statements)

References 20 publications

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“…v sin i was determined by using the dataset obtained in 2008 November, which had the best phase coverage in three observing runs. The final values we adopted are 83.9 km s −1 and 77.9 km s −1 , which are between the ones derived by Hill, Fisher & Holmgren (1990) (81 km s −1 and 71 km s −1 ) and Kjurkchieva et al (2003) (90 km s −1 and 80 km s −1 ). The value of γ was determined for each dataset, because of the different instrumental radial velocity zero-points of three observing runs.…”

Section: System Parameterssupporting

confidence: 67%

Doppler images of the eclipsing binary ER Vulpeculae

Xiang

Cameron

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present Doppler images of both components of the eclipsing binary system ER Vul, based on the spectra obtained in November, 2006 September and 2008 November. The least-squares deconvolution technique is used for enhancing the signal-to-noise ratios of the observed profiles. The new surface images reveal that both stars of ER Vul show strong starspot activities and the starspots appear at various latitudes. The surface maps of 2006 and 2008 both show the presence of large high-latitude starspots on each component of ER Vul. We find no obvious phase shift of the active regions during our observations. The longitude distributions of starspots are non-uniform on both stars. At low-to-mid latitudes, the active regions are almost exclusively found in the hemisphere facing the other star. However, we find no pronounced concentration of spots at the sub-stellar points.

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Section: System Parameterssupporting

confidence: 67%

Doppler images of the eclipsing binary ER Vulpeculae

Xiang

Cameron

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…In contrast to the H α line the depths of the 6495 Å line at the two eclipses are equal and the relative difference of the depths of the profiles of the two stellar components is smaller (they are even equal in strength at some phases). We also found orbital variability of this line in the short-period RS CVn-stars: CG Cyg (Kjurkchieva et al 2003a), ER Vul (Kjurkchieva et al 2003b), and WY Cnc (Kjurkchieva et al 2004). Profiles of the latter had wide wings and filled-in cores.…”

Section: Orbital Variability Of the Spectral Linessupporting

confidence: 53%

Spectroscopic and photometric observations of the short-period RS CVn-type star BH Virginis

Kjurkchieva

Marchev

Heckert

et al. 2004

A&A

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Abstract. High-resolution spectroscopic observations around the H α line and BVRI photometry from 1993 to 2003 of the eclipsing short-period RS CVn star BH Vir are presented. The simultaneous solution of our radial velocity curves and light curves yielded the following values for global parameters of the components:The measured rotational broadening of the spectral lines corresponds to equatorial velocities V 1 = 79.8 km s −1 and V 2 = 68.4 km s −1 . Our data reveal considerable H α emission excess of the two stellar components. We modelled the photometric data to find the size and location of the starspots for each year. The established decreasing trend of the spot latitudes may indicate a latitudinal cycle of at least a decade.

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“…Source 8: Kjurkchieva et al (2003). These RVs come also from the Rozhen 2.0 m reflector coudé spectra.…”

Section: Ephemeris Inmentioning

confidence: 97%

“…Conceivably -in addition to the non-uniform and variable brightness of the stellar disks -there could be some more or less permanent, phase-locked circumstellar structures, partly responsible for the observed Balmer emission. Note that Kjurkchieva et al (2003) argue in favour of the presence of circumstellar matter in the system on the basis of their Hα observations.…”

Section: Character Of the Light Curvementioning

confidence: 99%

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An improved ephemeris and physical elements of ER Vul

Harmanec

Božić²,

Thanjavur³

et al. 2004

A&A

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Abstract. New photoelectric UBV and BVRI observations, secured during August−November of 2002 at two observatories distant in local time are analyzed together with two earlier photometric data sets and all available radial velocities to derive the most accurate ephemeris of the binary and to set limits on its basic physical elements. These observations were obtained as a support for a high-dispersion spectroscopic study, results of which will be published separately. It was found that radial velocities and photometric observations spanning 53 years can be reconciled with the linear ephemeris T prim.min. = HJD 2 440 182.25628(46) + 0 .d 698095113 (29) × E, where the rms errors of the last digits are given in brackets. Masses of the stars are 1.02 M and 0.97 M and the binary separation is 4.170 R . There is still a large uncertainty in the stellar radii. We also report the discovery of rapid light variations on a time scale of hours seen in the U band light curve and offer a few thoughts on the future investigation of this binary.

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Spectroscopic and photometric observations of the short-period RS CVn-type star ER Vulpeculae

Cited by 14 publications

References 20 publications

Doppler images of the eclipsing binary ER Vulpeculae

Doppler images of the eclipsing binary ER Vulpeculae

Spectroscopic and photometric observations of the short-period RS CVn-type star BH Virginis

An improved ephemeris and physical elements of ER Vul

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