排序方式： 共有55条查询结果，搜索用时 234 毫秒
1.
我们于1989年11月30日晚对PG0027+260进行了时间分辨率为108秒的高速CCD测光,得到了一条完整的光变曲线,从而确认其为激变食变星系统,轨道周期0.146~d 相似文献
2.
J. Pritchard J. B. Marquette Patrick Tisserand J. P. Beaulieu E. Lesquoy A. Milsztajn 《Astrophysics and Space Science》2006,304(1-4):227-229
More than 10 years of microlensing survey observations by the EROS Collaboration have monitored several million stars, amongst them several thousand eclipsing binary stars. In this poster we present some of the difficulties and rewards of the study of this immense database.Based on observations made at ESO by the EROS collaboration 相似文献
3.
Shaukat Goderya 《Astrophysics and Space Science》2002,282(1):121-130
Astronomical research with a small telescope (20 cm – 40 cm) has always been a challenging problem. The invention of CCD cameras
and personal computers has now put this question to past as small telescopes can do good and practicle science. This paper
describes the use of small telescope in the study of eclipsing binary stars. Binary stars play an important role as astrophysical
laboratories in our quest to understand the evolution and structure of stars. The most useful aspects of research with a small
telescope in binary star research is; 1) as a viable teaching laboratory for begining students 2) to teach and learn the fundamental
observational techniques that are common to many types of astronomical research areas 3) as a starting point to initiate research
programs in observational astronomy, optics, instrumentation, computational astrophysics and 4) as a foundation to develop
an infrastructure and technical know how for larger telescope facility.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
4.
《New Astronomy》2015
A photometric CCD study of EQ Tauris was carried out in the R, V and B bands. These new data were analyzed by using the PHOEBE and Binary Marker 3 programs, which yielded the geometrical system parameters and mass and radius of both stars. We find these to confirm the results of Pribulla and Vanko (2002). Using these new data together with data from the literature, the orbital period variations were studied by using the Kalimeris method. We find the same timescale of variability of the orbital period as Pribulla and Vanko (2002), namely about 49 years. 相似文献
5.
D. Chochol T. Pribulla M. Vaňko P. Mayer M. Wolf P. G. Niarchos K. D. Gazeas V. N. Manimanis L. Brát M. Zejda 《Astrophysics and Space Science》2006,304(1-4):93-96
Orbital period changes of the eclipsing binaries GO Cyg and GW Cep are explained by the light-time effect for the first time. New minima of the eclipsing binary AR Aur improve the predicted light-time orbit. The light-time orbit with the quadratic ephemeris of the binary matches the new observations of V505 Sgr better than the linear one. As the light-time effect fits in corresponding O − C diagrams of all four systems have been reaching extreme values, the observations of minima times in forthcoming years are highly desirable. 相似文献
6.
In this study complete BV light curves of the W Ursae Majoris binary V1073 Cygni obtained in 2005 are presented. We have used the spectroscopic data of V1073 Cyg obtained by Ahn et al. (1992) for analysis. The analysis of radial velocity and light curves was made with Wilson} program (1998) and the geometric and physical elements} of the system were derived. By searching the simultaneous} solutions of the system, we have determined the masses and radii of the components: 1.64M⊙, 2.275R⊙ for the primary component and 0.55M⊙, 1.397R⊙ for the secondary component respectively. The effective temperature of 6494 ± 53 K for the secondary component was also estimated. 相似文献
7.
Davood Manzoori 《Astrophysics and Space Science》2008,313(4):339-344
This paper describes how a new photometric V light curve solution of Algol type binary U Sge was obtained using Wilson–Devinney
code. I also discuss how the physical and orbital parameters, along with absolute dimensions of the system, were determined.
The Roche lobe configurations of the system indicate that the secondary component has filled its Roche lobe and therefore
is losing mass at the rate of 6.15×10−7
M
sun yr−1. The conservative mass flow is the most likely process in this system. 相似文献
8.
In 2007, the asteroid Kalliope will reach one of its annual equinoxes. As a consequence, its small satellite Linus orbiting in the equatorial plane will undergo a season of mutual eclipses and occultations very similar to the one that the Galilean satellites undergo every 6 years. This paper is aimed at preparing a campaign of observations of these mutual events occurring from February to May 2007. This opportunity occurs only under favorable geometric conditions when the Sun and/or the Earth are close to the orbital plane of the system. This is the first international campaign devoted to the observation of photometric events within an asynchronous asteroidal binary system. We took advantage of a reliable orbit solution of Linus to predict a series of 24 mutual eclipses and 12 mutual occultations observable in the spring of 2007. Thanks to the brightness of Kalliope (mv?11), these observations are easy to perform even with a small telescope. Anomalous attenuation events could be observed lasting for about 1-3 h with amplitude up to 0.09 mag. The attenuations are of two distinct types that can clearly be identified as primary and secondary eclipses similar to those that have been previously observed in other minor planet binary systems [Pravec, P., Scheirich, P., Kusnirák, P., Sarounová, L., Mottola, S., Hahn, G., Brown, P., Esquerdo, G., Kaiser, N., Krzeminski, Z., Pray, D.P., Warner, B.D., Harris, A.W., Nolan, M.C., Howell, E.S., Benner, L.A.M., Margot, J.-L., Galád, A., Holliday, W., Hicks, M.D., Krugly, Yu.N., Tholen, D., Whiteley, R., Marchis, F., Degraff, D.R., Grauer, A., Larson, S., Velichko, F.P., Cooney, W.R., Stephens, R., Zhu, J., Kirsch, K., Dyvig, R., Snyder, L., Reddy, V., Moore, S., Gajdos, S., Világi, J., Masi, G., Higgins, D., Funkhouser, G., Knight, B., Slivan, S., Behrend, R., Grenon, M., Burki, G., Roy, R., Demeautis, C., Matter, D., Waelchli, N., Revaz, Y., Klotz, A., Rieugné, M., Thierry, P., Cotrez, V., Brunetto, L., Kober, G., 2006. Photometric survey of binary near-Earth asteroids. Icarus 181, 63-93]. With these favorable circumstances, such photometric observations will provide us tight constraints regarding physical properties of Linus such as the size, shape and synodic spin period. 相似文献
10.
Photometric study of the newly discovered short period eclipsing binary 1SWASP J133105.91 + 121538.0
《New Astronomy》2014
A total of 311 BVRI observations were carried out on 4 May 2013 for the new short period W UMa system 1SWASP J133105.91 + 121538.0 using the 1.88 m reflector telescope of Kottamia Astronomical Observatory (KAO) at NRIAG. A photometric solution of these light curves was obtained by means of Wilson–Devinney (WD) code. A spotted model was applied to treat the asymmetry of the light curve. The results show that the more massive component is hotter than the less massive one with about ΔT ∼ 300 K. The system is at a distance of 89 ± 3.6 pc. Based on the physical parameters of the system, we investigate the evolutionary state of the components. Both components are above the zero age main sequence (ZAMS) track by about 0.2 magnitudes. 相似文献