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A. Schwarzenberg-Czerny & J. Kaluzny 《Monthly notices of the Royal Astronomical Society》1998,300(1):251-256
The stability of massive stars is re-examined with respect to an adiabatic dynamical instability discovered by Stothers & Chin. An adiabatic stability analysis is performed, its validity for the objects being considered is discussed, and the relation between the mean adiabatic index and adiabatic stability is commented on. As the results of Stothers & Chin could not be confirmed, we suspect that luminous blue variable instability is due to non-adiabatic effects. 相似文献
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A. Olech P. R. Wo&#;niak C. Alard J. Kaluzny I. B. Thompson 《Monthly notices of the Royal Astronomical Society》1999,310(3):759-764
We present V -band light curves of 61 variables from the core of the globular cluster M5 obtained using a newly developed image subtraction method (ISM). Four of these variables were previously unknown. Only 26 variables were found in the same field using photometry obtained with dophot software. Fourier parameters of the ISM light curves have relative errors up to 11 times smaller than parameters measured from dophot photometry. We conclude that the new method is very promising for searching for variable stars in the cores of the globular clusters and gives very accurate relative photometry with quality comparable to photometry obtained by the Hubble Space Telescope . We also show that the variable V104 is not an eclipsing star as has been suggested, but is an RRc star showing non-radial pulsations. 相似文献
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A. Z. Bonanos K. Z. Stanek R. P. Kudritzki L. Macri D. D. Sasselov J. Kaluzny D. Bersier F. Bresolin T. Matheson B. J. Mochejska N. Przybilla A. H. Szentgyorgyi J. Tonry G. Torres 《Astrophysics and Space Science》2006,304(1-4):207-209
We present the first direct distance determination to a detached eclipsing binary in M33, which was found by the DIRECT Project. Located in the OB 66 association, it was one of the most suitable detached eclipsing binaries found by DIRECT for distance determination, given its 4.8938 day period. We obtained follow-up BV photometry and spectroscopy from which we determined the parameters of the system. It contains two O7 main sequence stars with masses of and and radii of and , respectively. We derive temperatures of K and K and determine the reddening . Using HST photometry for flux calibration in the V band, we obtain a preliminary distance modulus of mag ( kpc). The photometry and thus distance is subject to revision in the final paper. 相似文献
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J. Kaluzny I. B. Thompson W. Krzeminski A. Schwarzenberg-Czerny 《Monthly notices of the Royal Astronomical Society》2006,365(2):548-554
We present the results of a photometric survey for variable stars in the central region of the nearby globular cluster NGC 6397. Time-series photometry was obtained for 30 variable objects. The sample includes 12 new objects, of which six show periodic light curves and two are eclipsing binaries of unknown period. Six variables possess certain and three possess likely X-ray counterparts detected with the Chandra observatory. Among them, four are cataclysmic variables and one is a foreground eclipsing binary. The cataclysmic variable CV2 exhibited a likely dwarf nova type outburst in 2003 May. The cataclysmic variable CV3 was observed at 18.5 < V < 20.0 during five observing runs, but went into a low state in 2003 May when it reached V > 22 . We have found that the light curve of the optical companion to the millisecond pulsar PSR J1740−5340 exhibits noticeable changes of its amplitude on a time-scale of a few months. A shallow eclipse with Δ V = 0.03 mag was detected in one of the cluster turn-off stars suggesting the presence of a large planet or brown dwarf in orbit. 相似文献
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Beata Mazur Janusz Kaluzny Wojciech Krzemi&#;ski 《Monthly notices of the Royal Astronomical Society》1999,306(3):727-735
We report the results of a CCD search for short-period variables in the field of a southern globular cluster NGC 6362. We identified 19 new candidate variables, five of which are cluster RR Lyraes, four are probable SX Phe-type stars and eight are eclipsing binaries. Of the discovered binaries, three are EA-type systems, two of which are located on the cluster CMD in the turn-off region and the third 1 mag above the turn-off point, in the yellow straggler region. Five other systems are of W UMa type, three of which are foreground objects and two are likely cluster members. The remaining two candidates exhibit a modulation of the brightness level with an amplitude of 0.1–0.2 mag; further observations are needed to reveal the nature of their variability. Phased VI light curves for 20 variables (18 RR Lyrae stars and two blue stragglers) located in the central region of the cluster are presented. 相似文献
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P. Pietrukowicz J. Kaluzny A. Schwarzenberg-Czerny I. B. Thompson W. Pych W. Krzeminski B. Mazur 《Monthly notices of the Royal Astronomical Society》2008,388(3):1111-1126
We present the results of a search for dwarf novae (DNe) in globular clusters (GCs). It is based on the largest available homogeneous sample of observations, in terms of the time-span, number of observations and number of clusters. It includes 16 Galactic GCs and yielded two new certain DNe: M55-CV1 and M22-CV2. All previously known systems located in our fields were recovered, too. We surveyed M4, M5, M10, M12, M22, M30, M55, NGC 288, NGC 362, NGC 2808, NGC 3201, NGC 4372, NGC 6362, NGC 6752, ω Centauri (NGC 5139) and 47 Tucanae (NGC 104). The discovery of two DNe, namely M55-CV1 and M22-CV2, was already reported by Kaluzny et al. and Pietrukowicz et al., respectively. In the remaining 14 GCs, we found no certain new DNe. Our result raises the total number of known DNe in the Galactic GCs to 12 DNe, distributed among seven clusters. Our survey recovered all three already known erupting cataclysmic variables (CVs) located in our fields, namely M5-V101, M22-CV1, and V4 in the foreground of M30. To assess the efficiency of the survey, we analysed images with inserted artificial stars mimicking outbursts of the prototype DNe SS Cygni and U Geminorum. Depending on the conditions, we recovered between 16–100 per cent of these artificial stars. The efficiency seems to be predominantly affected by duty cycle/time-sampling and much less by distance/magnitude. Except for saturated tiny collapsed cores of M30, NGC 362 and NGC 6752 (and also the dense core of NGC 2808), crowding effects in the V band were avoided by our image subtraction technique augmented with auxiliary unsaturated B -band images. Our results clearly demonstrate that in GCs common types of DNe are very rare indeed. However, great care must be taken before these conclusions can be extended to the CV population in GCs. 相似文献
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A. Olech J. Kaluzny I. B. Thompson A. Schwarzenberg-Czerny 《Monthly notices of the Royal Astronomical Society》2003,345(1):86-96
New photometry of RRab and RRc stars in ω Centauri is used to calibrate their absolute magnitudes MV as a function of (a) metallicity and (b) the Fourier parameters of light curves in the V band. The zero point of both calibrations relies on the distance modulus to the cluster derived earlier by the Cluster AgeS Experiment (CASE) project based on observations of the detached eclipsing binary OGLE GC17. For RRab variables, we obtained a relation of MV = (0.26 ± 0.08)[ Fe/H ] + (0.91 ± 0.13) . A dereddened distance modulus to the Large Magellanic Cloud (LMC) based on that formula is μ0 = 18.56 ± 0.14 mag . The second calibration of MV , which is based on Fourier coefficients of decomposed light curves, results in the LMC distance of μ0 = 18.51 ± 0.07 mag . 相似文献
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