N

Fig. 6.5 More complex models: Three-dimensional representatives of the interacting X-Ray system SS433. Courtesy, A. M. Cherepashchuk

The mass ratio of the SS433 system is not directly observed. Instead, the mass function

m3 sin3

has been determined to be somewhere between 2 M0 (cf. D'Odorico et al. 1991) and 10 M0 (Crampton & Hutchings, 1981), with a third determination of 7.7 M0 (Fabrica & Bychkova, 1990). X-ray systems are among the principal binaries studied by the "Russian School." Goncharsky et al. (1991) and Antokhina et al. (1992, 1993) discuss the more recent studies. A more recent review on this field is by Cherepashchuk (2005).

6.5 Other Approaches

Et sic de similibus (And so of like kind)

6.5.1 Budding's Eclipsing Binary Model

Budding (1993, Chap. 8) discusses in didactic detail his "Standard Eclipsing Binary Star Model" (SEBM) to analyze circular orbit systems. It is basically a spherical model including circular spots, and thus, often applied to analyze spotted stars; cf. Budding & Zeilik (1987). Note that the original light curves are "cleaned" of the effects of spots.

6.5.2 Kopal's Frequency Domain Method

Kopal's contributions to the field of modern light curve analysis were crucial; his early works prepared the way for the new era. Here, however, we discuss a technique that he developed in his later years, the "Frequency Domain Method."

The basic aspects of this technique are described in Kopal (1979) and also in Kopal (1990, pp. 41-69). Kopal discusses, in great mathematical depth, the representation of the fractional light loss in symmetric EB light curves in terms of integral transforms, especially Hankel and Fourier transforms, and the asymptotic properties of finite sums of the latter.

The method concentrates on the determination of quantities such as the area, A2m, under the function of measured light, I, plotted against sin2m 0. A2m is the moment of the eclipse of index m. This empirically determined quantity, A2m, may be defined as

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