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Jílové u Prahy, Czech Republic

Zasche P.,Charles University | Svoboda P.,Private Observatory | Uhlar R.,Private Observatory
Astronomy and Astrophysics | Year: 2012

Context. A study of late-type low-mass eclipsing binaries provides us with important information about the most common stars in the Universe. Aims. We obtain the first light curves and perform period analyses of two neglected eclipsing binaries GK Boo and AE For to reveal their basic physical properties. Methods. We performed both a period analysis of the times of the minima and a BVR light curve analysis. Many new times of minima for both the systems were derived and collected from the data obtained by automatic and robotic telescopes. This allowed us to study the long-term period changes in these systems for the first time. From the light curve analysis, we derived the first rough estimates of the physical properties of these systems. Results. We find that the analyzed systems are somewhat similar to each other. Both contain low-mass components of similar types, both are close to the Sun, both have short orbital period, and both contain another low-mass companions on longer orbits of a few years. In the case of GK Boo, both components are probably of K3 spectral type, while the distant companion is probably a late M star. The light curve of GK Boo is asymmetric, which probably causes the shift in the secondary minima in the O-C diagram. System AE For comprises two K7 stars, and the third body is a possible brown dwarf with a minimal mass of only about 47 M Jup. Conclusions. We succeed in completing period and light curve analyses of both systems, although a more detailed spectroscopic analysis is needed to confirm the physical parameters of the components to a higher accuracy. © 2012 ESO. Source


Zasche P.,Charles University | Uhlar R.,Private Observatory
Monthly Notices of the Royal Astronomical Society | Year: 2013

More than three hundred years ago, Ole Rømer measured the speed of light purely by observing the periodic shift of the observed eclipse arrival times of Jupiter's moons arising from the varying Earth-Jupiter distance. The same method of measuring the periodic modulation of delays is still used in astrophysics. The ideal laboratories for this effect are eclipsing binaries. The unique system V994 Her consists of two eclipsing binaries orbiting each other. However, until now it was not certain whether these were gravitationally bound and what their orbital period was. We show that the system is in fact quintuple and the two eclipsing binaries are orbiting each other with a period of about 6.3 yr. This analysis was performed only through studying the periodic modulation of the two periods: during the periastron passage one binary has an apparently shorter period, while the other one is longer, exactly as required by theory. Additionally, it was found that both inner eclipsing pairs orbit with slightly eccentric orbits, undergoing slow apsidal motion with a period of the order of centuries. © 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Source


Zasche P.,Charles University | Uhlar R.,Private Observatory
Astronomy and Astrophysics | Year: 2010

Aims. We present the detailed analysis of triple system KR Com with different observational techniques - photometry, interferometry, and period variation. Methods. The use of BVR photometry of the close-contact binary KR Com, which is the primary component of a triple system, helps us to better describe the properties of the components. The interferometric data obtained during the last 30 years sufficiently determine the visual orbit, but the use of minima timings of KR Com for the study of period variation together with the visual orbit is a novel approach in this system. Results. Basic physical parameters resulting from the light curve analysis agree well with the previous results from spectroscopy. The temperatures for the primary and secondary component resulted in 5549 and 6072 K, respectively, and the amount of the third light in all filters is about 1/3 of the total luminosity. The distant third component revolves around the common barycenter on 11 yr orbit with a very high eccentricity (0.934) and this movement is also detectable via the period variation, which is clearly visible in the O-C diagram of times of minima observations. The use of minima times for the combined analysis helps us to independently determine the distance to the system (64.02 ± 9.42 pc) and also to confirm the orientation of the orbit in space. Conclusions. New minima observations and also spectroscopy would be very profitable, especially during the next periastron passage in the year 2017. © 2010 ESO. Source


Wolf M.,Charles University | Kotkova L.,Czech Republic Astronomical Institute | Kocian R.,VSB - Technical University of Ostrava | Dreven R.,Private Observatory | Hanzl D.,Private Observatory
Astronomical Journal | Year: 2010

WW Camelopardalis is a relatively bright eclipsing binary system with a slightly eccentric orbit. A dozen of its new eclipse times were measured as part of our long-term observational project of eccentric eclipsing binaries. Based on a new solution of the current O - C diagram, we found for the first time an apsidal motion in good agreement with theory. Its period is about 370 ± 50 years. The determined internal structure constant is close to the theoretically expected value. The relativistic effect is significant, being about 13% of the total apsidal motion rate. © 2010. The American Astronomical Society. Source


Zasche P.,Charles University | Svoboda P.,Private Observatory | Slechta M.,Czech Republic Astronomical Institute
Monthly Notices of the Royal Astronomical Society | Year: 2012

The main aim of this paper is the first detailed analysis of multiple system V2083 Cyg, to reveal its basic physical properties. The system was studied using the methods of light-curve and radial-velocity curve analysis, together with interferometric data from the visual pair obtained during the last century. It was found that the close subsystem contains two very similar stars of spectral type A7-8. Moreover, a third body is orbiting around this pair with a period of about 177yr. Due to the discrepancy in the total mass derived with the two methods, the possibility arises that the third body is perhaps also a binary, or some object with lower luminosity but higher mass than a normal main-sequence star. Another explanation is that the Hipparcos value of parallax is incorrect and the system is much closer to the Sun. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS. Source

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