共查询到20条相似文献，搜索用时 265 毫秒
1.
BP Vulpeculae is a bright eclipsing binary system showing apsidal motion. It was found in an earlier study that it shows retrograde apsidal motion which contradicts theory. In this paper we present the first BV light curve of the system and its light curve solution as well as seven new times of the minima from the years 1959–1963. This way we could expanded the baseline of the investigation to five decades. Based on this longer baseline we concluded that the apsidal motion is prograde agreeing with the theoretical expectations and its period is about 365 years and the determined internal structure constant is close to the theoretically expected one. 相似文献
2.
The DI Herculis system has been extensively studied over the past few decades because its observed rate of apsidal advance is less than a quarter of that which is expected from its physical and orbital properties. Work by Khaliullin et al. (1991) proposed that this slow rate of apsidal advance is a result of the presence of a third (stellar mass) body orbiting the system, however, observations by Guinan et al. (1994) severely restrict the orbital properties of such a solution. We show that a planetary mass object in a highly inclined orbit relative to the binary is capable of producing the observed apsidal motion, while remaining within the bounds of the most recent set of observations. A wide range of stable solutions are possible. 相似文献
3.
Necdet Güdür 《Astrophysics and Space Science》1978,57(1):17-39
The detached eclipsing binary system AG Per was observed at Ege University Observatory on 12 nights from December 1974 to December 1975. Approximately 460 observations were obtained in each yellow and blue. AG Per has long been known to have an apsidal motion and eccentricities. New apsidal motion parameters based on the author's observations and all of the other minima are given. Solutions for its orbital elements were carried out using three different procedures: the Kitamura method, Wood triaxial ellipsoid model and Kopal's Fourier analysis method in the frequency-domain. By use of the available spectroscopic data for AG Per, the observational apsidal motion constant has been calculated. 相似文献
4.
M. Wolf L. Šmelcer H. Kučáková T. Hynek K. Onderková P. Svoboda M. Chrastina 《New Astronomy》2010,15(6):530-532
V381 Cas is a relatively bright and early-type eclipsing binary system. Several new times of its eclipses were measured as part of our long-term observational project of eccentric eclipsing binaries. Based on a current O–C diagram solution, we found for the first time that its orbit is slightly eccentric (e = 0.025) and shows a very rapid apsidal advance with short period of about 20 years only. The relativistic and third body effects are negligible, being about 3% of the total apsidal motion rate. 相似文献
5.
Igor M. Volkov 《Astrophysics and Space Science》2005,296(1-4):105-108
We present a new photoelectric light curve of α Coronae Borealis. The derived rate of apsidal motion differs from the theoretical
prediction. A possible solution of the problem is suggested. 相似文献
6.
Basing on recent and old photoelectric times of minimum, a new slightly longer period of the apsidal motion for an eclipsing binary PV Cas has been obtained. A difference between observed and theoretical periods of the apsidal motion estimated on the base of Claret and Gimenez models growed up to 30 years is found. 相似文献
7.
Z. Bozkurt Ö. L. De&#;irmenci 《Monthly notices of the Royal Astronomical Society》2007,379(1):370-378
Binary systems showing both apsidal motion and light travel time (LTT) effects which cause orbital period changes in close binaries were studied. 15 triple systems showing apsidal motion were found by searching the literature, and a table including the important parameters of these systems was constructed. Six of the systems given in this table were selected and observed photometrically. Existence of both apsidal motion and LTT effects in all selected systems was investigated by means of the analysis of their eclipse times. The mean observed internal structure constants, log = k 2,obs , and contributions to the apsidal motion from the theory of General Relativity and the third/fourth bodies were calculated. The masses of the third/fourth bodies and some characteristics of their orbits were also calculated. 相似文献
8.
William Tobin 《Experimental Astronomy》1994,5(1-2):67-74
This paper reviews recent progress in CCD photometry of eclipsing binary systems in the crowded fields of the Magellanic Clouds. Some preliminary findings are given. The interesting eccentric system HV2274 is noted as important for follow-up studies, particularly concerning its apsidal motion. Some further developments are anticipated. 相似文献
9.
B and V photometry of the eccentric eclipsing binary DI Her is reported, with the aim of contributing to a more accurate determination
of the timings required for the ongoing apsidal motion studies. The resulting apsidal motion rate is close to the one reported
earlier by Khodykin and Volkov (1989), Guinan, Marshal and Maloney (IBVS 4101), and Yildiz et al. (2000).
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
10.
İ. Bulut 《New Astronomy》2009,14(7):604-606
The apsidal motion analysis of the eccentric eclipsing binaries: V397 Cep, V493 Car and BW Aqr have been presented. The method described by Lacy (1992) [Lacy, C.H S., 1992. AJ 104, 2213] has been used for the apsidal motion analysis. The apsidal motion periods have been found to be 174.2 ± 1.4, 277.3 ± 21.3 and 7195 ± 174 years for V397 Cep, V493 Car and BW Aqr, respectively. 相似文献
11.
ö.L. Değirmenci 《Astrophysics and Space Science》1997,253(2):237-252
Photoelectric observations of the eclipsing binary IQ Persei have been carried out in B and V colours at Ege University Observatory.
The corresponding light curves were analyzed by synthesis techniques. The absolute physical parameters and apsidal motion
period (122 yr) of the system were obtained. The results have been compared with theoretical evolutionary models which include
both mass loss and convective overshooting. Theoretical evolutionary tracks of the component stars indicate an age of 1.3
× 108 years and an apsidal motion constant of 0.0040 which is greater than its observed value by only about 5%. The A7 secondary
of the eclipsing pair is still close to the zero-age main sequence but B7 primary is about halfway through its main sequence
life-time.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
12.
Photometric observation of the eccentric eclipsing binary V459 Cas (e = 0.0244) was performed to find a new rate of apsidal motion. Also the advance of the periastron is calculated theoretically by taking into account the Newtonian (classical) and general-relativistic effects according to physical and orbital parameters of the system. A new observed rate of apsidal motion of 19∘.8/100 yr is computed which is not in agreement with the one reported earlier. Meanwhile a theoretical value of 2∘.64/100 yr is obtained which is 7.49 times smaller than the observed one. 相似文献
13.
Several new times of minimum light recorded with photoelectric or CCD means have been gathered for the eccentric eclipsing
binary V889 Aql (P = 11.1 days, e = 0.37). Its O–C diagram is presented, and improved elements of the apsidal motion and the light-time effect (LITE) are given. We found a
long apsidal motion period of about 24 400 ± 2400 years and a period of the third body of about 52 ± 2 years. 相似文献
14.
In this paper, a new method for the determination of apsidal motion parameters in eccentric eclipsing binaries is presented. A sequential procedure has been followed throughout allowing an automatized on-line computation of the elements and their accuracies as well as a more realistic fit to the observed times of minima. A determination of individual mean errors for the parameters of fit give us the possibility to compare the results with available theoretical models of stellar structure. In the procedure, we have introduced a determination of preliminary elements by means of Fourier transform and extended the practical equations to terms up to the fifth power of the eccentricity. An application to the well-known case of the eclipsing binary GL Car has been made. Our analysis shows an apsidal motion period of 25.3 years with a value of 0.152 for the orbital eccentricity. 相似文献
15.
This paper is devoted to binary stars belonging to the class of eclipsing-variable systems.Photometric and spectroscopic analysis of eclipses allows us to determine geometric parameters of the orbit and physical characteristics of stellar components as well as inclinations of stellar equators to the orbital plane. Estimations of inclinations can be obtained from measurement of the Rossiter-McLaughlin effect, which is discussed using examples of some eccentric binaries with an anomalous apsidal effect. Our task is to find the complete spectrum of solutions of the equation of apsidal motion, depending on the inclinations of the polar axes of the components to the orbital one for these systems, based on their individual spectroscopic and photometric observational data. The matrix of solutions allows us to select those pairs of polar inclinations that provide agreement with the observational apsidal period. 相似文献
16.
An analysis of fifteen-year photoelectric observations of DI Herculis shows that the upper estimate for the relativistic part of apsidal motion in this binary system is almost three times lower than the theoretical value. The total observed angular velocity of apsidal rotation is 0
.
°
0124 yr–1. The relativistic part is less than 0
.
°
008 yr–1 instead of 0
.
°
023 yr–1 required by the theory. 相似文献
17.
Multi-colourWBVR photoelectric observations of the eclipsing binaries IT Cas, CO Cep, and AI Hya were carried out. The photometric elements and the absolute parameters of the orbits and components were obtained. The valuation of the angular rate of the apsidal motion of AI Hya based on the comparison of our observations with the previous photoelectric light curve of this system was derived. 相似文献
18.
Multi-colourWBVR photoelectric observations of the eclipsing binary OX Cas were carried out. The photometric elements, absolute parameters and the angular rate of the apsidal motion (
= 9.1 deg yr–1 were obtained. The apsidal parameterk
2 derived for this system is by 15–25% smaller than the theoretical parameterk
2. 相似文献
19.
Photometric observations of the eccentric eclipsing binary V1143 Cyg were performed during Aug.–Sep. 2000 and July 2002, in
Johnson B and V bands. The analysis of both light curves was made separately using the 1998 version of Wilson’s LC code. In order to find
a new observed rate of apsidal motion, we followed the procedure described by Guinan and Maloney (1985). A new observed rate
of apsidal motion of 3∘.72/100 yr was computed, which is close to the one reported earlier by Khaliullin (1983), Gimenez and Margrave (1985), and
Burns et al. (1996). 相似文献
20.
《Chinese Astronomy and Astrophysics》1982,6(3):233-242
We solve by an appropriate method the difficulty of near-commensurability, , in the motion of Hyperion (Saturn VII) and give a first-order solution of its motion. Our result explains two interesting observed features, the regression of the apsidal line and the exclusive occurrence of apocentre C conjunction of SVII and SVI. 相似文献