A spectroscopic study of the eclipsing binaries SV Camelopardalis and XY Ursae Majoris

Özeren, Ferhat Fikri; Gunn, Alastair G.; Doyle, J. G.; Jevremović, D.

doi:10.1051/0004-6361:20000232

Cited by 16 publications

(14 citation statements)

References 29 publications

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“…The line profiles of SV Cam are considerably deeper at the second quadrature than at the first one. The same behavior of the H α profile of SV Cam was observed recently by Ozeren et al (2001). The explanation of the absorption established in AB Dor, HK Aqu, SS Boo by cool material in their co-rotating atmospheres (Collier Cameron et al 1990;Byrne et al 1996;Hall et al 1990) is not applicable to our case because the excess absorption for two other short-period RS CVn stars, namely, XY UMa (Kjurkchieva et al 2000b) and RT And (Kjurkchieva et al 2001) is visible also around the second quadrature.…”

Section: Discussionsupporting

confidence: 84%

“…In this way, our spectral observations show an enhanced emission of the secondary star of SV Cam in the H α line but not in the FeI 6678 line. The result of our analysis supports the conclusion of Ozeren et al (2001) about the H α emission excess from the secondary star of SV Cam obtained by spectral substraction technique as well as the more general conclusion of Frasca & Catalano (1994) about the H α emission in late-type active binaries. et al (1995) found that systems with H α emission above the continuum are all cooler than 5000 K. The temperature of the primary star of SV Cam is above this limit and there should be no emission excess expected from it.…”

Section: Emission From the Stellar Componentssupporting

confidence: 89%

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Spectroscopic observations of the short-period, RS CVn-type star SV Cam

Kjurkchieva

Marchev

Zoła

2002

A&A

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Abstract. Spectroscopic observations of the eclipsing, short-period RS CVn-star SV Cam in the range 6500-6700Å, covering the whole orbital period are presented. The absorption profiles of the lines Hα and FeI 6678 are doubled out of the eclipses. The relative contribution of the secondary star is stronger in the FeI 6678 line than in Hα. We determined K1 = 123.1 ± 1.2 km s and V 2 eq = 79 km s −1 corresponding to the measured rotational broadenings of the investigated lines coincide with the velocities calculated from the obtained stellar radii. The phase behavior of both Hα and FeI 6678 profiles of the primary star shows the presence of two cool spots with maximum visibilities at phases 0.27 and 0.86. The analysis of the two lines in the middle of the primary eclipse allows us to illustrate the excess of the Hα emission of the secondary star. The parameters of the stellar components of SV Cam derived from our spectroscopy and photometry are in very good agreement. The final result of our investigation is that there are three sources of activity in SV Cam: local active regions (photospheric spots) on its primary component, enhanced chromospheric emission from the secondary star and some additional emission originating from circumstellar gas.

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Section: Discussionsupporting

confidence: 84%

Section: Emission From the Stellar Componentssupporting

confidence: 89%

Spectroscopic observations of the short-period, RS CVn-type star SV Cam

Kjurkchieva

Marchev

Zoła

2002

A&A

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“…This is reported in literature as a mid-F to mid-G system with 0.6 day period and a light-curve of the β Lyrae type. There is a long history of observations and analyses of this system, with extensive photometry (e.g., Kjurkchieva et al 2000;Patkós 1982;Zeilik et al 1988), and spectroscopy (e.g., Hempelmann et al 1997;Kjurkchieva et al 2002;Lehmann et al 2002;Özeren et al 2001;Pojmański 1998;Popper 1996;Rainger et al 1991;Rucinski et al 2002). Most authors have interpreted asymmetries in the light curves and the variation in them as due to spots.…”

Section: The Targetsmentioning

confidence: 99%

Evaluating Gaia performances on eclipsing binaries

Milone¹,

Munari²,

Marrese³

et al. 2005

A&A

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Abstract. This is the fourth in a series of papers that aim both to provide reasonable orbits for a number of eclipsing binaries and to evaluate the expected performance of Gaia of these objects and the accuracy that is achievable in the determination of such fundamental stellar parameters as mass and radius. In this paper, we attempt to derive the orbits and physical parameters for three eclipsing binaries in the mid-F to mid-G spectral range. As for previous papers, only the H P , V T , B T photometry from the Hipparcos/Tycho mission and ground-based radial velocities from spectroscopy in the region 8480−8740 Å are used in the analyses. These data sets simulate the photometric and spectroscopic data that are expected to be obtained by Gaia, the approved ESA Cornerstone mission to be launched in 2011. The systems targeted in this paper are SV Cam, BS Dra and HP Dra. SV Cam and BS Dra have been studied previously, allowing comparisons of the derived parameters with those from full scale and devoted ground-based investigations. HP Dra has no published orbital solution. SV Cam has a β Lyrae type light curve and the others have Algol-like light curves. SV Cam has the complication of light curve anomalies, usually attributed to spots; BS Dra has non-solar metallicity, and HP Dra appears to have a small eccentricity and a sizeable time derivative in the argument of the periastron. Thus all three provide interesting and different test cases.

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“…These authors found that active stars, and RS CVn stars in particular, have substantially broader lines than normal stars and that, in spite of the large spread, the line widths are well correlated with the visual absolute magnitudes (r = 0.80 to 0.93). We wish to stress that in Overlayed to the data points we show the WB relationship for normal stars form Paper I (full line), and for RS CVn stars (dashed line) from Ozeren et al (1999). all the above analyses, the mean values for the line widths were used instead of the individual determinations.…”

Section: The Wb Diagram For Rs Cvn Starsmentioning

confidence: 99%

A study of the Mg II 2796.34 Å emission line in late–type normal and RS CVn stars

Cardini

Cassatella

Badiali

et al. 2003

A&A

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Abstract.We carry out an analysis of the Mg  2796.34 Å emission line in RS CVn stars and make a comparison with the normal stars studied in a previous paper (Paper I). The sample of RS CVn stars consists of 34 objects with known HIPPARCOS parallaxes and observed at high resolution with IUE. We confirm that RS CVn stars tend to possess wider Mg  lines than normal stars having the same absolute visual magnitude. However, we could not find any correlation between the logarithmic line width log W • and the absolute visual magnitude M V (the Wilson-Bappu relationship) for these active stars, contrary to the case of normal stars addressed in Paper I. On the contrary, we find that a strong correlation exists in the (M V , log L Mg ii ) plane (L Mg ii is the absolute flux in the line). In this plane, normal and RS CVn stars are distributed along two nearly parallel straight lines with RS CVn stars being systematically brighter by ≈1 dex. Such a diagram provides an interesting tool to discriminate active from normal stars. We finally analyse the distribution of RS CVn and of normal stars in the (log L Mg ii , log W • ) plane, and find a strong linear correlation for normal stars, which can be used for distance determinations.

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A spectroscopic study of the eclipsing binaries SV Camelopardalis and XY Ursae Majoris

Cited by 16 publications

References 29 publications

Spectroscopic observations of the short-period, RS CVn-type star SV Cam

Spectroscopic observations of the short-period, RS CVn-type star SV Cam

Evaluating Gaia performances on eclipsing binaries

A study of the Mg II 2796.34 Å emission line in late–type normal and RS CVn stars

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