EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 558 (October 2013) A&A, 558 (2013) A51 Full HTML
Free Access
Issue
A&A
Volume 558, October 2013
Article Number A51
Number of page(s) 12
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201322054
Published online 03 October 2013

© ESO, 2013

1. Introduction

Eccentric eclipsing binaries (EEB) with an apsidal motion can provide us with an important observational test of theoretical models of stellar structure and evolution. A long-term collecting the times of minima of EEBs observed throughout the apsidal motion cycle and consecutive detailed analysis of the period variations of EEB can be performed, yielding both the orbital eccentricity and the period of rotation of the apsidal line with high accuracy (Giménez 1994). Many different sets of stellar evolution models have been published in recent years, e.g. Maeder (1999), Claret (2004), or Claret (2006); however, to distinguish between them and to test which one is more suitable is still rather difficult. The internal structure constants as derived from the apsidal motion analysis could serve as one independent criterion. On the other hand, to discriminate between the models only stellar parameters for EEBs with an accuracy of 1% can be used.

The Magellanic Clouds are of prime importance in the context of stellar evolution theory. However, the chemical composition of the Magellanic Clouds differs from that of the solar neighborhood (e.g. Ribas 2004) and the study of these massive and metal-deficient stars in the LMC checks our evolutionary models for these abundances. All eclipsing binaries analysed here have properties that make them important astrophysical laboratories for studying the structure and evolution of massive stars (Ribas 2004).

Here we analyse the observational data and rates of apsidal motion for five LMC detached eclipsing systems. All these systems are early-type objects known to have eccentric orbits and to exhibit apsidal motion. Similar studies of LMC EEBs have been presented by Michalska & Pigulski (2005, hereafter MP05) and Michalska (2007).

Table 1

Apsidal motion elements for HV 982, HV 2274, MACHO 78.6097.13, MACHO 81.8881.47, and MACHO 79.5377.76.

2. Observations of minimum light

The monitoring of faint EEBs in external galaxies requires only moderate telescopes in the 1–2 m class range equipped with a modern CCD camera. However, a large amount of observing time is needed, which is unavailable at larger telescopes. During past observational seasons, we accumulated over 1600 photometric observations at selected phases during primary and secondary eclipses and derived 16 precise times of minimum light for selected eccentric systems. New CCD photometry was obtained at the La Silla Observatory in Chile, where the 1.54 m Danish telescope (hereafter DK154) with the CCD camera and RI filters was used.

All CCD measurements were dark-subtracted and then flat-fielded using sky exposures taken at either dusk or dawn. Several comparison stars were chosen in the same frame as the variables. A synthetic aperture photometry and astrometry software developed by Velen and Pravec called Aphot, was routinely used for data obtained. No correction for differential extinction was applied because of the proximity of the comparison stars to the variable and the resulting negligible differences in air mass and their similar spectral types.

The new times of primary and secondary minima and their errors were determined by the classical Kwee-van Woerden (1956) algorithm. All new times of minima are given in Table A.1, where epochs are calculated from the ephemeris given in Table 1; the other columns are self-evident.

3. Photometry

For all of the systems we harvested the Macho (Faccioli et al. 2007) and Ogle (Graczyk et al. 2011) photometry available online. These photometric data were used both for minima times analysis as well as for light curve analysis.

The analysis of the light curves for two of the systems was carried out using the program PHOEBE, ver. 0.31a (Prša & Zwitter 2005), which is based on the Wilson-Devinney algorithm (Wilson & Devinney 1971) and its later modifications, but some of the parameters had to be fixed during the fitting process. The albedo coefficient remained fixed at value 1.0 and the gravity darkening coefficients g = 1.0. The limb darkening coefficients were interpolated from the van Hamme tables (van Hamme 1993). A problem emerged with the synchronicity parameters (Fi) due to poor coverage of the RV data near the eclipses and low quality of the light curves used for the LC analysis, hence we fixed these values at Fi = 0. The temperature of the primary component was derived from the V − I photometric index, from MP05 and from the resulting masses derived from the combined LC+RV analysis.

4. Spectroscopy

The spectroscopic data for two of the systems (MACHO 81.8881.47, MACHO 79.5377.76) were found in the ESO Archive of the UV-Visual Echelle Spectrograph (UVES) at the Very Large Telescope (VLT). The spectra were obtained during the ESO Period 68 program “Precise distances to the LMC and SMC from double-lined eclipsing binaries”; the PI of the project was A. Clausen. Typical exposure times were about 1500 seconds, while the spectra typically have a signal-to-noise ratio (S/N) of about 50. The original data were reduced using the standard ESO routines. The final radial velocities (hereafter RV) used for the analysis were derived via a manual cross-correlation technique (i.e. the direct and flipped profile of spectral lines manually shifted on the computer screen to achieve the best match) using program SPEFO (Horn et al. 1996; Škoda 1996) on several absorbtion lines in the measured spectral region (usually Hβ to Hϑ). The derived radial velocities are given in Table B.1. We estimate the error of individual data points to be about 5 km s-1.

5. An approach for the analysis

For the analysis we used the approach presented below. For the systems where the inclination of the orbit is known, the first two steps can be skipped.

  • First, all of the available photometric data were analysed,resulting in a set of minima times. Preliminary apsidal motionparameters were derived (with the assumption i = 90°).

  • Second, the eccentricity (e), argument of periastron (ω), and apsidal motion rate (\hbox{$\dot \omega$}) derived from the apsidal motion analysis were used for the preliminary light curve (hereafter LC) analysis.

  • Third, the inclination (i) from the LC analysis was used for the final apsidal motion analysis.

  • And finally, the resulting e, ω, and \hbox{$\dot \omega$} values from the apsidal motion analysis were used for the final LC + RV analysis.

6. Apsidal motion analysis

The apsidal motion in all eccentric systems was studied by means of an O–C diagram analysis. All available times of minima, both published in the literature and newly measured, were analysed using the method presented by Giménez & García-Pelayo (1983). This is a weighted least-squares iterative procedure, including terms in the eccentricity up to the fifth order. There are five independent variables \hbox{$(T_0, P_{\rm s}, e, \dot{\omega}, \omega_0)$} determined in this procedure. The periastron position ω is given by the linear equation ω=ω0+ω̇E\begin{eqnarray*} \omega = \omega_0 + \dot{\omega}\ E \end{eqnarray*}where \hbox{$\dot{\omega}$} is the rate of periastron advance, and the position of periastron for the zero epoch T0 is denoted as ω0. The relation between the sidereal and the anomalistic period, Ps and Pa, is given by Ps=Pa (1−ω̇/360◦),\begin{eqnarray*} P_{\rm s} = P_{\rm a} \,(1 - \dot{\omega}/360^\circ), \end{eqnarray*}and the period of apsidal motion by U=360◦Pa/ω̇.\begin{eqnarray*} U = 360^\circ P_{\rm a}/\dot{\omega} . \end{eqnarray*}All new precise CCD times of minima were used with a weight of 10 or 20 in our computation. Some of our less precise measurements were weighted by a factor of 5, while the earlier visual and photographic times (esp. the times of the mid-exposure of a photographic plate) were given a weight of one or nought because of the large scatter in these data.

7. Analysis of the systems

7.1. HV 982

The detached eclipsing binary HV 982 (also known as MACHO 82.8043.26, LMV110; Vmax = 14m.65; Sp. B5V) is a relatively well-known LMC binary with an eccentric orbit (e = 0.15) and a moderate orbital period of 5.3 days. It was discovered to be a variable star by Gaposhkin (1970), who published the first photographic light curve.

Pritchard et al. (1994, 1998) in their photometric study derived high surface temperatures (~28 000 K) and masses (~8 M⊙) of components. They also derived the apsidal motion period U = 205 ± 7 years. The precise stellar parameters of components of HV 982 were derived spectroscopically by Fitzpatrick et al. (2002), who found components with similar mass and size, M1=11.28±0.46 M⊙,M2=11.61±0.47 M⊙,R1=7.15±0.12 R⊙,R2=7.92±0.13 R⊙.\begin{eqnarray*} && M_1 = 11.28 \pm 0.46\, M_{\odot},\ M_2 = 11.61 \pm 0.47\, M_{\odot}, \\ && R_1 = 7.15 \pm 0.12\, R_{\odot},\ R_2 = 7.92 \pm 0.13\, R_{\odot}. \end{eqnarray*}The following linear light elements were given in that paper: Pri.Min.=HJD2 449 340.d7172+5.d33522×E.\begin{eqnarray*} \rm Pri.\ Min. = HJD\ 2\,449\,340\fd7172 + 5\fd33522 \times E. \end{eqnarray*}Using the complete analyses of HV 982 they also found the distance to the center of the LMC dLMC = 50.7 ± 1.2 kpc. Later, Clausen et al. (2003) presented a new accurate CCD uvby light curve obtained at the Danish 1.54 m telescope at La Silla and derived the precise photometric elements with apsidal motion period U = 208 ± 15 years.

All CCD times of minimum light given in Pritchard et al. (1998) and Clausen et al. (2003) were incorporated into our analysis. Using Macho (Faccioli et al. 2007) and Ogle (Graczyk et al. 2011) photometry, we were able to derive additional times of minimum light. A total of 68 times of minimum light were used in our analysis (see Table A.1). The orbital inclination adopted was , based on the analysis of Fitzpatrick et al. (2002). The computed apsidal motion parameters and their internal errors of the least-squares fit are given in Table 1. In this table, Ps denotes the sidereal period, Pa the anomalistic period, e represents the eccentricity, and \hbox{$\dot{\omega}$} is the rate of periastron advance (in degrees per cycle and in degrees per year). The zero epoch is given by T0, and the corresponding position of the periastron is represented by ω0. The O–C residuals for all times of minimum with respect to the linear part of the apsidal motion equation (Min = T0 + P × E) are shown in Fig. 1. The non-linear predictions, corresponding to the fitted parameters, are plotted for primary and secondary eclipses.

7.2. HV 2274

thumbnail Fig. 1

O–C diagram for the times of minima of HV 982. The continuous and dashed curves represent predictions for the primary and secondary eclipses, respectively. The individual primary and secondary minima are denoted by dots and open circles, respectively. Larger symbols correspond to the photoelectric or CCD measurements that were given higher weights in the calculations.

The detached and double-lined eclipsing binary HV 2274 (also known as MACHO 19.3577.7, 2MASS J05024076-6824212, LMV 182, FL 3556; Vmax = 14m.13; Sp. B1-2 IV-III) is a relatively bright and well-studied LMC eclipsing binary with an eccentric orbit (e = 0.17) and a moderate orbital period of 5.7 days. It was discovered to be a variable star by Leavitt (1908). Later, Shapley & Nail (1953) recognized its eclipsing nature and classified it as a β Lyrae type. The eccentric orbit and apsidal motion of HV 2274 was first announced by Watson et al. (1992), who obtained the BVIc CCD photometry at the Mount John University Observatory. See also the history of HV 2274 in the last paper mentioned. Later Claret (1996) found the masses and evolutionary status of this system: Pri.Min.=HJD2 448 099.d818+5.d726006×E.\begin{eqnarray*} \rm Pri.\ Min. = HJD\ 2\,448\,099\fd818 + 5\fd726006 \times E. \end{eqnarray*}The fundamental properties of HV 2274 were most recently given in Ribas et al. (2000) who determined the precise absolute parameters of both eclipsing components to be M1=12.2±0.7M⊙,M2=11.4±0.7M⊙,R1=9.86±0.24R⊙,R2=9.03±0.24R⊙.\begin{eqnarray*} &&M_1 = 12.2 \pm 0.7\ M_{\odot},\ M_2 = 11.4 \pm 0.7\ M_{\odot}, \\ && R_1 = 9.86 \pm 0.24\ R_{\odot},\ R_2 = 9.03 \pm 0.24\ R_{\odot}. \end{eqnarray*}They also derived the improved apsidal motion period U = 123 ± 3 years and the value of internal structure constant log k2,obs = −2.56. Since the above-mentioned papers were published, new times of minima have been obtained, which allowed us to reduce the uncertainties in the derived parameters. We collected all times of minimum light given in the literature together with new ones derived from Macho, Ogle, and our new photometry obtained in Chile. All of these values are listed in Table A.1. In total, 58 precise times of minimum light were used in our analysis, including 29 secondary eclipses. The orbital inclination adopted was , based on the analysis of Ribas et al. (2000).

Analysing the available data using the apsidal motion hypothesis, we found an additional variation superimposed on the apsidal motion. Hence, we used a different code computing the apsidal motion parameters together with the third-body orbit (a so-called light travel time effect), see e.g. Irwin (1959). Altogether, ten parameters were fitted (five from apsidal motion, five from the third body hypothesis), thus this approach led to an acceptable solution. The resulting parameters of the fit are given in Tables 1 and 2, the complete O–C diagrams are shown in Figs. 2 and 3. From the third-body parameters we were also able to compute the mass function of the distant component, which resulted in f(m3) = 0.053 ± 0.008 M⊙. From this value, we calculated the predicted minimal mass of the third body (i.e. assuming coplanar orbits i3 = 90°), which resulted in m3,min = 3.4 M⊙. If we propose this body in the system, one can ask whether it is detectable somehow in the already-obtained data. The period is rather long for continuous monitoring of the radial velocity changes, but detecting the third light in the light curve solution is difficult. Assuming a normal main sequence star, its luminosity is about only 1% of the total system luminosity. Such a weak third light could be detectable only in extremely precise photometric data for the light curve solution.

7.3. MACHO 78.6097.13

Table 2

Third-body orbit parameters for HV 2274.

thumbnail Fig. 2

O–C diagram for the times of minima of HV 2274. See legend to Fig. 1. The final fit is composed from two effects: the apsidal motion together with the third-body hypothesis.

thumbnail Fig. 3

O–C residuals for HV 2274 after subtraction of the apsidal motion term. Only the third body effect is plotted.

thumbnail Fig. 4

O–C graph for the times of minimum of MACHO 78.6097.13. See legend to Fig. 1.

The detached eclipsing binary MACHO 78.6097.13 (also known as OGLE J051804.81-694818.9, LMC MP#5; Vmax = 14m.37, sp O9V+O9V) is an eccentric binary system (e = 0.046) with a short orbital period (P = 3.1 d) discovered by MP05 in the Ogle field LMC-SC7.

Our analysis gives the following ephemeris: Pri.Min.=HJD2 452 424.d6888+3.d1070278×E.\begin{eqnarray*} \rm Pri.\ Min. = HJD\ 2\,452\,424\fd6888 + 3\fd1070278 \times E. \end{eqnarray*}The most detailed analysis of the system was published by González et al. (2005), which was based on the ESO spectral observations together with the MACHO data. They also derived the masses and radii of both components that were used in the present analysis. Both components are of O9 spectral types, which makes this system the earliest in our sample.

Our new times of minimum light, as well as the timings derived from Macho and Ogle photometry are given in Table A.1. All of these data (31 minima times) were used in our calculations. Using the parameters presented by González et al. (2005), we analysed the system on apsidal motion, deriving the parameters given in Table 1. As one can see, this system has the lowest eccentricity in our sample and the apsidal advance is rather fast: almost one half of the period has been covered with observations so far.

7.4. MACHO 81.8881.47

The detached eclipsing binary MACHO 81.8881.47 (also known as OGLE J053517.75-694318.7, LMC MP#7; Vmax = 14m.9; Sp. B) is a relatively bright binary system with an eccentric orbit (e = 0.2) and a moderate orbital period P ≃ 3.9 days. Its variability was discovered by MP05 in the OGLE field LMC-SC16. Most recently, Graczyk et al. (2011) included this star in their catalogue of eclipsing binaries in the LMC. They also gave the preliminary ephemeris: Pri.Min.=HJD2 453 571.d1063+3.d881980×E.\begin{eqnarray*} \rm Pri.\ Min. = HJD\ 2\,453\,571\fd1063 + 3\fd881980 \times E. \end{eqnarray*}Using Ogle and Macho photometry, we were also able to derive additional times of minimum light; two more minima were derived from our observations. Only 30 times of minimum light were used in our analysis (see Table A.1). As one can clearly see from the shape of the light curve and the different duration of both the primary and secondary eclipse, this is the system with the highest value of eccentricity in our sample.

We used the ESO data for deriving the radial velocities of the components. Ten UVES spectra were found, of which nine were usable for the analysis. The derived RVs of both components are given in Table B.1. Together with these radial velocities, the MACHO light curve was used for the subsequent combined LC+RV analysis. The final parameters of the solution are given in Table 3, while the fits are plotted in Figs. 5 and 6. Our results show the rather noticeable property that the more massive component (the primary) is smaller and less luminous (i.e. has a lower temperature). However, this is still a preliminary result based on only nine RVs and a poor fit. Although the scenario is possible, the more probable explanation is that the mass ratio is inverse, and the primary and secondary components are interchanged. This can be allowed for within the uncertainties of the mass ratio. A more detailed analysis is needed, based on more precise spectral observations. The orbital inclination was about , which was later used for the apsidal motion analysis. The resulting parameters of apsidal motion are found in Table 1, and the current O–C diagram is shown in Fig. 7. As one can see, the period is rather long and only about 1/5 has been covered so far.

Table 3

Light and radial velocity curve fit parameters for MACHO 81.8881.47 and MACHO 79.5377.76.

thumbnail Fig. 5

Radial velocity curve for MACHO 81.8881.47.

thumbnail Fig. 6

Light curve for MACHO 81.8881.47.

thumbnail Fig. 7

O–C graph of MACHO 81.8881.47. See legend for Fig. 1.

7.5. MACHO 79.5377.76

The detached eclipsing binary MACHO 79.5377.76 (also known as OGLE J051323.98-692249.2, Vmax = 15m.8; Sp. B) is a fairly neglected binary system with a moderate eccentric orbit (e = 0.06) and a short orbital period (P ≃ 2.64 day): Pri.Min.=HJD2 452 262.d6776+2.d6365767×E.\begin{eqnarray*} \rm Pri.\ Min. = HJD\ 2\,452\,262\fd6776 + 2\fd6365767 \times E. \end{eqnarray*}We used the MACHO and OGLE photometry together with our new observations from Chile to derive the times of minima, the ESO spectral observations to derive the radial velocities, and the MACHO photometry to model the light curve of the system. Our results are plotted in Figs. 8 and 9. The resulting parameters are given in Table 3. As one can see, both components are of equal mass and their spectral type was estimated to be about B0-B1. Radial velocities used for our analysis are also given in Table B.1. The coverage of the radial velocity curve is better than for MACHO 81.8881.47; however, it was rather difficult to derive the synchronicity parameters Fi, and so we fixed them at Fi = 0. A total of 34 reliable times of minimum light were used in our analysis including 16 secondary eclipses (see tables in the Appendices). The final apsidal motion elements are given in Table 1, and the O–C graph is shown in Fig. 10. The apsidal period is the shortest among systems studied here, only 42 years.

thumbnail Fig. 8

Radial velocity curve for MACHO 79.5377.76.

thumbnail Fig. 9

Light curve for MACHO 79.5377.76.

thumbnail Fig. 10

O–C diagram for MACHO 79.5377.76. See legend to Fig. 1.

Table 4

Basic physical properties of HV 982, HV 2284, MACHO 78.6097.13, MACHO 81.8881.47, and MACHO 79.5377.76 and their internal structure constants.

8. Discussion

The detection of apsidal motion in EEB provides the opportunity to test models of stellar internal structure. The internal structure constant (ISC) k2,obs is related to the variation in the density inside the star and can be derived using the expression k2,obs=1c21+c22 PaU=1c21+c22 ω̇360,\begin{equation} k_\mathrm{2, obs} = \frac{1}{c_{21} + c_{22}} \, \frac{P_{\rm a}}{U} = \frac{1}{c_{21} + c_{22}} \, \frac{\dot{\omega}}{360} , \end{equation}(1)where c21 and c22 are functions of the orbital eccentricity, fractional radii, the masses of the components, and the ratio between rotational velocity of the stars and Keplerian velocity (Kopal 1978). We also assume that the component stars rotate pseudosynchronously with the same angular velocity as the maximum orbital value at periastron (see e.g. Kopal 1978). Another possible approach is to use the value of vsini as derived from the combined LC+RV analysis published earlier. However, there could be a problem with the inclination of the rotation axis (as in the case of DI Her) and, moreover, the error of the internal structure constants is by far dominated by the term ri5\hbox{$r_i^5$} in the equations. In addition to the classical Newtonian contribution, the observed rate of rotation of the apses includes the contribution from General Relativity (Giménez 1985), ω̇rel=5.45×10-411−e2(M1+M2P)2/3,\begin{equation} \dot{\omega}_\mathrm{rel} = \; 5.45 \times 10^{-4} \: \frac{1}{1-e^2} \:\Biggl( \frac{M_1 + M_2}{P} \Biggr) ^{2/3}, \end{equation}(2)where Mi denotes the individual masses of the components in solar units and P is the orbital period in days.

The values of \hbox{$\dot{\omega}_\mathrm{rel}$} and the resulting mean internal structure constants k2,obs for the systems studied are given in Table 4. Theoretical values k2,theo according to available theoretical models for the internal stellar structure computed by Claret (2006) for given masses of components are presented in Table 4.

thumbnail Fig. 11

Position and systemic velocities (see the colour scale on the right) of eclipsing binaries located in the LMC and its vicinity, see Table 5. The larger the symbol, the higher the precision. The background image of the LMC is used with the permission of the author Robert Gendler (http://www.robgendlerastropics.com).

We tried to compare our resulting systemic velocities with other published values of eclipsing binaries in the LMC, see Table 5 and Fig. 11. There are still only a few such systems studied in detail (i.e. LC+RV analysis). Therefore, reliable analysis of different velocities within the LMC is still very difficult. We can only compare our Fig. 11 with other kinematic studies of the LMC published earlier, e.g. that by Reid & Parker (2006) or Rohlfs et al. (1984), that were based on much larger radial-velocity data sets. Nevertheless, we can conclude that our two new systemic velocities roughly fit the overall picture and the total velocity dispersion within the LMC is more than 30 km s-1.

Table 5

Radial velocities of eclipsing binaries in the LMC derived from various analyses.

9. Conclusions

The apsidal motion in EEB has been used for decades to test evolutionary stellar models. This study provides accurate information on the apsidal motion rates of five main-sequence early-type binary systems in the LMC: HV 982, HV 2274, MACHO 78.6097.13, MACHO 81.8881.47, and MACHO 79.5377.76. In our Galaxy there are known a few hundreds of apsidal motion EEBs, however in the LMC there are still only a few dozen of these systems (Michalska & Pigulski 2005). Hence this study still presents an important contribution to the topic. The relativistic effects are weak, being up to 6% of the total apsidal motion rate. For the systems MACHO 79.5377.76 and MACHO 81.8881.47, their light and radial velocity curves were analysed for the first time yielding the stellar parameters of both components given in Table 4. Moreover, when the MACHO 79.5377.76 internal structure constant and the theoretical model are compared the system appears to be very young (~2 × 106 yr).

In spite of the considerable amount of observational data that has been collected for decades, the absolute dimensions of massive binary components are only known with an accuracy of about 1–3% (e.g. Clausen 2004). More detailed study based on more precise radial velocities would be very profitable to derive the physical properties of components with higher accuracy. The most promising system for further detailed analysis seems to be HV 2274 because of the putative third component in the system. We still know only a few such systems nowadays, see e.g. Bozkurt & Deǧirmenci (2007), while HV 2274 is the first to be discovered out of our Galaxy. Only precise spectral observations and their disentangling should reveal its true nature.

Online material

Appendix A: Table of minima

Table A.1

List of the minima timings used for the analysis.

Appendix B: Table of radial velocities

Table B.1

List of the radial velocities used for the analysis.

Acknowledgments

We do thank the MACHO and OGLE teams for making all of the observations easily and publicly available. This work was supported by the Research Program MSM0021620860 Physical Study of objects and processes in the Solar System and in Astrophysics of the Ministry of Education of the Czech Republic, by the Czech Science Foundation grant no. P209/10/0715, by the grant UNCE 12 of the Charles University in Prague, and by the grant LG12001 of the Ministry of Education of the Czech Republic. We are also grateful to the ESO team at the La Silla Observatory for their help in maintaining and operating the Danish telescope. The authors would like to thank M. Zejda, J. Liška, J. Janík, and M. Skarka for their important help with photometric observations. G.Michalska is also acknowledged for sending us the unpublished times of minima for selected binaries. The following internet-based resources were used in research for this paper: the SIMBAD database and the VizieR service operated at the CDS, Strasbourg, France, the NASA Astrophysics Data System Bibliographic Services, and the ESO Science Archive Facility.

References

  1. Bonanos, A. Z. 2009, ApJ, 691, 407 [NASA ADS] [CrossRef] [Google Scholar]
  2. Bozkurt, Z., & Deǧirmenci, Ö. L. 2007, MNRAS, 379, 370 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
  3. Claret, A. 1996, A&A, 315, 415 [NASA ADS] [Google Scholar]
  4. Claret, A. 2004, A&A, 424, 919 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  5. Claret, A. 2006, A&A, 453, 769 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  6. Clausen, J. V. 2004, New A Rev., 48, 679 [Google Scholar]
  7. Clausen, A., Storm, J., Larsen, S. S., & Giménez, A. 2003, A&A, 402, 509 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  8. Cowley, A. P., Crampton, D., Hutchings, J. B., Remillard, R., & Penfold, J. E. 1983, ApJ, 272, 118 [NASA ADS] [CrossRef] [Google Scholar]
  9. Faccioli, L., Alcock, C., Cook, K., et al. 2007, AJ, 134, 1963 [NASA ADS] [CrossRef] [Google Scholar]
  10. Fitzpatrick, E. L., Ribas, I., Guinan, E. F., et al. 2002, ApJ, 564, 260 [NASA ADS] [CrossRef] [Google Scholar]
  11. Fitzpatrick, E. L., Ribas, I., Guinan, E. F., Maloney, F. P., & Claret, A. 2003, ApJ, 587, 685 [NASA ADS] [CrossRef] [Google Scholar]
  12. Gaposhkin, S. 1970, SAO Special Report, 310 [Google Scholar]
  13. Gaposhkin, S. I. 1977, SAO Special Report, 380 [Google Scholar]
  14. Giménez, A. 1985, ApJ, 297, 405 [NASA ADS] [CrossRef] [Google Scholar]
  15. Giménez, A. 1994, Exp. Astron., 5, 91 [Google Scholar]
  16. Giménez, A., & García-Pelayo, J. M. 1983, Ap&SS, 92, 203 [NASA ADS] [CrossRef] [Google Scholar]
  17. González, J. F., Ostrov, P., Morrell, N., & Minniti, D. 2005, ApJ, 624, 946 [NASA ADS] [CrossRef] [Google Scholar]
  18. Graczyk, D., Soszyński, I., Poleski, R., et al. 2011, AcA, 61, 103 [Google Scholar]
  19. Horn, J., Kubát, J., Harmanec, et al. 1996, A&A, 309, 521 [NASA ADS] [Google Scholar]
  20. Hutchings, J. B., Crampton, D., & Cowley, A. P. 1978, ApJ, 225, 548 [NASA ADS] [CrossRef] [Google Scholar]
  21. Hutchings, J. B., Crampton, D., Cowley, A. P., Bianchi, L., & Thompson, I. B. 1987, AJ, 94, 340 [NASA ADS] [CrossRef] [Google Scholar]
  22. Irwin, J. B. 1959, AJ, 64, 149 [NASA ADS] [CrossRef] [Google Scholar]
  23. Kopal, Z. 1978, Dynamics of Close Binary Systems (Dordrecht: Reidel), Astrophys. Space Sci. Lib., 68, 524 [NASA ADS] [Google Scholar]
  24. Kwee, K. K., & van Woerden, H. 1956, Bull. Astron. Inst. Netherlands, 12, 327 [Google Scholar]
  25. Leavitt, H. S. 1908, Annals of Harvard College Observatory, 60, 87 [Google Scholar]
  26. Massey, P., Penny, L. R., & Vukovich, J. 2002, ApJ, 565, 982 [NASA ADS] [CrossRef] [Google Scholar]
  27. Massey, P., Morrell, N. I., Neugent, K. F., et al. 2012, ApJ, 748, 96 [NASA ADS] [CrossRef] [Google Scholar]
  28. Maeder, A. 1999, A&A, 347, 185 [NASA ADS] [Google Scholar]
  29. Michalska, G. 2007, IBVS No. 5759 [Google Scholar]
  30. Michalska, G., & Pigulski, A. 2005, A&A, 434, 89 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  31. Ostrov, P. G. 2001, MNRAS, 321, L25 [NASA ADS] [CrossRef] [Google Scholar]
  32. Ostrov, P. G., & Lapasset, E. 2003, MNRAS, 338, 141 [NASA ADS] [CrossRef] [Google Scholar]
  33. Ostrov, P. G., Lapasset, E., & Morrell, N. I. 2000, A&A, 356, 935 [NASA ADS] [Google Scholar]
  34. Ostrov, P. G., Morrell, N. I., & Lapasset, E. 2001, A&A, 377, 972 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  35. Pietrzyński, G., Graczyk, D., Gieren, W., et al. 2013, Nature, 495, 76 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  36. Pritchard, J. D., Tobin, W., & Clark, M. 1994, Exp. Astron., 5, 43 [NASA ADS] [CrossRef] [Google Scholar]
  37. Pritchard, J. D., Tobin, W., Clark, M., & Guinan, E. F. 1998, MNRAS, 299, 1087 [NASA ADS] [CrossRef] [Google Scholar]
  38. Prša, A., & Zwitter, T. 2005, ApJ, 628, 426 [NASA ADS] [CrossRef] [Google Scholar]
  39. Reid, W. A., & Parker, Q. A. 2006, MNRAS, 373, 521 [NASA ADS] [CrossRef] [Google Scholar]
  40. Ribas, I. 2004, New Astron. Rev., 48, 731 [Google Scholar]
  41. Ribas, I., Guinan, E. F., Fitzpatrick, E. L. et al. 2000, ApJ, 528, 692 [NASA ADS] [CrossRef] [Google Scholar]
  42. Ribas, I., Fitzpatrick, E. L., Maloney, F. P., Guinan, E. F., & Udalski, A. 2002, ApJ, 574, 771 [NASA ADS] [CrossRef] [Google Scholar]
  43. Rohlfs, K., Kreitschmann, J., Feitzinger, J. V., & Siegman, B. C. 1984, A&A, 137, 343 [NASA ADS] [Google Scholar]
  44. Shapley, H., & Nail, V. McK. 1953, Proc. Nat. Acad. Sci., 39, 1 [Google Scholar]
  45. Škoda, P. 1996, in Astronomical Data Analysis Software and Systems V, eds. G. H. Jacoby, & J. Barnes, ASP Conf. Ser., 101, 187 [Google Scholar]
  46. van Hamme, W. 1993, AJ, 106, 2096 [NASA ADS] [CrossRef] [Google Scholar]
  47. Watson, R. D., West, S. R. D., Tobin, W., & Gilmore, A. C. 1992, MNRAS, 528, 527 [NASA ADS] [CrossRef] [Google Scholar]
  48. Williams, S. J., Gies, D. R., Henry, T. J., et al. 2008, ApJ, 682, 492 [NASA ADS] [CrossRef] [Google Scholar]
  49. Wilson, R. E., & Devinney, E. J. 1971, ApJ, 166, 605 [NASA ADS] [CrossRef] [Google Scholar]
  50. Wozniak, P. R., Vestrand, W. T., Akerlof, C. W., et al. 2004, AJ, 127, 2436 [NASA ADS] [CrossRef] [Google Scholar]

All Tables

Table 1

Apsidal motion elements for HV 982, HV 2274, MACHO 78.6097.13, MACHO 81.8881.47, and MACHO 79.5377.76.

In the text
Table 2

Third-body orbit parameters for HV 2274.

In the text
Table 3

Light and radial velocity curve fit parameters for MACHO 81.8881.47 and MACHO 79.5377.76.

In the text
Table 4

Basic physical properties of HV 982, HV 2284, MACHO 78.6097.13, MACHO 81.8881.47, and MACHO 79.5377.76 and their internal structure constants.

In the text
Table 5

Radial velocities of eclipsing binaries in the LMC derived from various analyses.

In the text
Table A.1

List of the minima timings used for the analysis.

In the text
Table B.1

List of the radial velocities used for the analysis.

In the text

All Figures

thumbnail Fig. 1

O–C diagram for the times of minima of HV 982. The continuous and dashed curves represent predictions for the primary and secondary eclipses, respectively. The individual primary and secondary minima are denoted by dots and open circles, respectively. Larger symbols correspond to the photoelectric or CCD measurements that were given higher weights in the calculations.
In the text
thumbnail Fig. 2

O–C diagram for the times of minima of HV 2274. See legend to Fig. 1. The final fit is composed from two effects: the apsidal motion together with the third-body hypothesis.
In the text
thumbnail Fig. 3

O–C residuals for HV 2274 after subtraction of the apsidal motion term. Only the third body effect is plotted.
In the text
thumbnail Fig. 4

O–C graph for the times of minimum of MACHO 78.6097.13. See legend to Fig. 1.
In the text
thumbnail Fig. 5

Radial velocity curve for MACHO 81.8881.47.
In the text
thumbnail Fig. 6

Light curve for MACHO 81.8881.47.
In the text
thumbnail Fig. 7

O–C graph of MACHO 81.8881.47. See legend for Fig. 1.
In the text
thumbnail Fig. 8

Radial velocity curve for MACHO 79.5377.76.
In the text
thumbnail Fig. 9

Light curve for MACHO 79.5377.76.
In the text
thumbnail Fig. 10

O–C diagram for MACHO 79.5377.76. See legend to Fig. 1.
In the text
thumbnail Fig. 11

Position and systemic velocities (see the colour scale on the right) of eclipsing binaries located in the LMC and its vicinity, see Table 5. The larger the symbol, the higher the precision. The background image of the LMC is used with the permission of the author Robert Gendler (http://www.robgendlerastropics.com).
In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.