Eclipsing binaries in open clusters. II. V453 Cyg in NGC 6871

By J. Southworth, P. Maxted, B. Smalley. 2004

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We derive absolute dimensions of the early B-type detached eclipsing binary V453Cygni (B0.4IV + B0.7IV, P = 3.89d), a member of the open cluster NGC6871. From the analysis of new, high-resolution, spectroscopy and the UBV light curves of Cohen (1974) we find the masses to be 14.36 ± 0.20Mfl and 11.11 ± 0.13Mfl, the radii to be 8.55 ± 0.06Rfl and 5.49 ± 0.06Rfl, and the eective temperatures to be

Subfields: Astronomy and Astrophysics, Education, Instrumentation

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Citations in the corpus

Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, methodology): “1σ errorbars are obtained using 1000 Monte Carlo simulations (Southworth et al. 2004c, 2005b).”
A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 (2015, methodology): “…Curve Fitting We analyze the photometry using standard Pythonbased minimizers, the emcee Markov Chain Monte-Carlo (MCMC) package (Foreman-Mackey et al. 2013), and the JKTEBOP lightcurve code (Southworth et al. 2004; Southworth 2011) using numerical integration to account for our ∼30-min cadence.”
High-precision photometry by telescope defocussing. I. The transiting planetary system WASP-5 (2009, methodology): “The transit light curves of WASP-5 were modelled using the jktebop6 code (Southworth et al. 2004a,b), which is based on the ebop program originally developed for eclipsing binary star systems (Popper & Etzel 1981; Etzel 1981; Nelson & Davis 1972).”
A PHOTOMETRIC VARIABILITY SURVEY OF FIELD K AND M DWARF STARS WITH HATNet (2009, methodology): “We model the light curve using the JKTEBOP program (Southworth et al. 2004a; Southworth et al. 2004b) which is based on the Eclipsing Binary Orbit Program (Popper & Etzel 1981; Etzel 1981; Nelson & Davis 1972), but includes more sophisticated minimization and error analysis routines.”
THE MASS–RADIUS(–ROTATION?) RELATION FOR LOW-MASS STARS (2010, methodology): “Several different software packages are commonly used to fit light curves (e.g. Wilson & Devinney 1971; Popper & Etzel 1981; Southworth et al. 2004; Prsa & Zwitter 2005), so it seems possible that the choice of algorithm could be significant.”
Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses (2008, methodology): “I use the jktebop code1, a heavily modified version of ebop (Southworth et al. 2004a,b) which incorporates the Levenberg-Marquardt optimisation algorithm (mrqmin; Press et al. 1992, p. 678), an improved treatment of limb darkening (LD), and extensive error analysis techniques.”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “I have modelled the light curves of each TEP using theJKTEBOP3 code (Southworth et al. 2004a,b).”