Cosmology

Close Binaries in the 21st Century: New Opportunities and by Alvaro Gimenez, Edward Guinan, Panagiotis Niarchos, Slavek

By Alvaro Gimenez, Edward Guinan, Panagiotis Niarchos, Slavek Rucinski

This ebook is the lawsuits of a global convention entitled "Close Binaries within the twenty first Century: New possibilities and Challenges", held in Syros island, Greece, June 27-30, 2005. The papers accumulated during this quantity aspect the most recent achievements within the box and mirror the cutting-edge of the dynamically evolving region of binary superstar study.

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O-type binaries . Eccentric 1. Overview V1007 Sco (HD 152248) is one of the earliest eclipsing binaries known; both components are of spectral type O7. According to visual as well as IUE spectra a luminosity classification of class I is suggested; however the solution of light curves gives radii corresponding to giants. 1) of the open cluster NGC 6231. It has been known as an SB2 system since the work of Struve (1944); its eclipsing nature was discovered by Mayer et al. 8160 days, S. Nesslinger ( ) · H.

It has been known as an SB2 system since the work of Struve (1944); its eclipsing nature was discovered by Mayer et al. 8160 days, S. Nesslinger ( ) · H. Drechsel · R. de P. Harmanec · P. Mayer · M. , 1996). The UBV photometry by Mayer et al. showed that the orbit is eccentric. Radial velocities of this star were published in several papers, the latest one being by Sana et al. (2001). Both values K 1,2 are close to 220 km/s. Penny et al. (1999) solved the V light curve by Mayer et al. and by HIPPARCOS (ESA, 1997.

E. smaller than would correspond to evolutionary models with Teff about 37000 K. The photometry of V1007 Sco is still rather scarce. Here we will discuss data consisting of the following sets of photoelectric observations and of far-UV magnitudes: 1. 2. 3. 4. 5. UBV observations obtained by Mayer et al. (1992) plus additional UBV observations secured by RL in 1993 and 1994. Hipparcos H p magnitudes, transformed into Johnson V using the transformation formula given by Harmanec (1998). V observations (derived from Str¨omgren photometry published by Manfroid et al.

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