Close Binary Star Observables: Modeling Innovations 2003-06

Abstract

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.

Asiago eclipsing binaries program IV. SZ Camelopardalis, aβ Cephei pulsator in a quadruple, eclipsing system

“…A photometric solution for SZ Cam was obtained with the WD code (Wilson & Devinney 1971;Wilson 1998) in its WD98K93d version as developed by Milone et al (1992), by adopting the MODE-2 option, appropriate for detached binary stars, which implements Roche geometry and a detailed treatment of reflection and other physical phenomena. It adopted the mass ratio as provided by the spectral disentangling.…”

Asiago eclipsing binaries program

“…Wilson 1998). Orbital solutions were carried out by testing various combinations of these parameters in the range 0.5 ≤ A 1,2 ≤ 1.0 and 0.3 ≤ g 1,2 ≤ 1.0 (A and g are expected to be unity for radiative envelopes), without improving accuracy.…”

Asiago eclipsing binaries program

“…The adopted bolometric albedos and exponents in the bolometric gravity brightening law were set to A 1 = A 2 = 0.5 and g 1 = g 2 = 0.3, respectively, as appropriate for convective atmospheres (Wilson 1998). As in Paper II, full orbital solution runs were also carried out with logarithmic and square-root limb darkening laws, as well as with various combinations of A 1,2 and g 1,2 in the range 0.5 ≤ A 1,2 ≤ 1.0 and 0.3 ≤ g 1,2 ≤ 1.0 (A and g are expected to be close to unity for radiative envelopes).…”