An improved ephemeris and physical elements of ER Vul

Harmanec, P.; Božić, H.; Thanjavur, Karun; Robb, R. M.; Ruždjak, Domagoj; Sudar, D.

doi:10.1051/0004-6361:20034614

Cited by 8 publications

(17 citation statements)

References 11 publications

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“…Harmanec et al (2004) b. Pop & Vamoş (2013) c. Gray et al (2001) d. Nordström et al (2004) demonstrated that the Doppler imaging code can be used for determining stellar parameters for both single and binary stars, and can avoid systematic errors caused by the effects of starspot distortions (Barnes et al 1998(Barnes et al , 2004.…”

Section: System Parametersmentioning

confidence: 99%

“…Fortunately, ER Vul has been extensively studied, and the physical and orbital parameters have been derived by many authors. We adopted the improved values of the radial velocity amplitude of the primary star (K1), mass ratio (q) and inclination (i) derived from both the photometric data and the radial velocities (Harmanec et al 2004). The first conjunction time (T0) and the orbital period (P) were from the paper by Pop & Vamoş (2013).…”

Section: System Parametersmentioning

confidence: 99%

“…The reflection effect was also considered by the imaging code, as described by . We adopted the values of the albedo coefficients from Harmanec et al (2004).…”

Section: System Parametersmentioning

confidence: 99%

“…ER Vul is an active eclipsing binary which is composed of two Sun-like stars, G0V primary and G5V secondary, in an orbital period of 0.698 d. According to Harmanec et al (2004), the masses of the primary and the secondary stars are 1.02 M⊙ and 0.97 M⊙, respectively. Hall (1976) classified ER Vul as a short-period RS CVn-type binary system.…”

Section: Introductionmentioning

confidence: 99%

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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 Parametersmentioning

confidence: 99%

Section: System Parametersmentioning

confidence: 99%

“…The reflection effect was also considered by the imaging code, as described by . We adopted the values of the albedo coefficients from Harmanec et al (2004).…”

Section: System Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Doppler images of the eclipsing binary ER Vulpeculae

Xiang

Cameron

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Applications on one side include Mayer et al (1991) [HJD 0 , P 0 , and dω/dt from RV 's and light curves of the EB V1765 Cygni]; Harmanec & Scholz (1993) [HJD 0 , P , and dP/dt from a century of RV 's for β Lyrae †]; Tarasov et al (1995) [HJD 0 and P from RV 's of the non-eclipsing triple system Persei]; Harmanec et al (2004) [P and dP/dt for ER Vulpeculae, a solar-type EB ]; Janik et al (2003) [dω/dt for the welldetached EB V436 Persei]; and Horn et al (1996) [HJD 0 ,dP/dt,dω/dt,HJD 0,3b ,and P 3b from RV 's of the non-eclipsing triple system 55 Ursae Majoris]. The Horn et al third body results for 55 UMa agree accurately with speckle (i.e.…”

Section: Whole Light and Velocity Curve Ephemerides And Extension To mentioning

confidence: 99%

Close Binary Star Observables: Modeling Innovations 2003-06

Wilson

2006

Proc. IAU

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Abstract. Innovative work on close binary models in 2003-06 improved upon synthesized line spectra, line profiles, and polarimetry; developed new ways of parameter estimation; and increased solution effectiveness and efficiency. Recent applications demonstrate the analytic power of binary system line spectrum models that pre-date the triennium. X-ray binary line profiles and radial velocity curves were refined by solution of the radiative transfer problem with specific inclusion of X-irradiation. Model polarization curves were generated by Monte Carlo experiments with multiple Thomson scattering in thin and thick binary system disks. In the parameter estimation area, independent developments by two groups now allow measurement of ephemerides, apsidal motion, and third body parameters from whole light and velocity curves, to supplement the traditional way of eclipse timings. Although the new route to those parameters is not well known within the ephemeris community, there are accuracy advantages and the number of applications is increasing. Numerical solution experiments on photometric mass ratios have checked two views of their intuitive basis, and show that mass ratios are well determined where star radii and limiting lobe radii are both well determined, which is for semi-detached or over-contact binaries with total-annular eclipses. Solution efficiency and automatic operation is needed for processing of light curves from large surveys, and will also be valuable for preliminary solutions of individually observed binaries. Neural networks have mainly been used for classification, and now a neural network program reliably finds preliminary solutions for W UMa binaries. Archived model light curves and Fourier fitting also are being pursued for classification and for preliminary solutions. Light curves in physical units such as erg · sec −1 · cm −3 now allow direct distance estimation by combining the absolute accuracy of model stellar atmospheres with the astrophysical detail of a physical close binary model, by means of rigorous scaling between surface emission and observable flux. A Temperature-distance (T-d) theorem specifies conditions under which temperatures of both stars and distance can be found from light and velocity curves.

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Secular period decreasing of detached chromospherically active binaries

Luo

Zhang

Deng

et al. 2010

Astrophys Space Sci

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The long-term orbital period changes of a large sample of detached chromospherically active binaries (CABs) were studied. Eleven such systems were found to be undergoing secular period decreases with the rates of −6.3 × 10 −9 to −1.1 × 10 −6 days per year. The period decreasing rates are found to vary depending on the orbital period. The longer the orbital period is, the more rapidly the period decreases. Following Stepien (Mon. Not. R. Astron. Soc. 274:1019, the period decreasing rate predicted by angular momentum loss (AML) caused by magnetic wind is computed for each system. A comparison between the observed and calculated period decreasing rates shows that the former values are obviously larger than the latter by 1-3 orders of magnitude. It suggests that the magnetic wind is not likely the determinant mechanism driving the AML in these systems. Finally, the orbital angular momentum (AM) and the rate of AML,J , are computed for each system. It shows that the AM have a similar change with the orbital period like dP /dt does, but logJ /J presents no strict changing with the kinematical ages.

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An improved ephemeris and physical elements of ER Vul

Cited by 8 publications

References 11 publications

Doppler images of the eclipsing binary ER Vulpeculae

Doppler images of the eclipsing binary ER Vulpeculae

Close Binary Star Observables: Modeling Innovations 2003-06

Secular period decreasing of detached chromospherically active binaries

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