Absolute Dimensions of the Metallic-Line Eclipsing Binary V501 Monocerotis

Torres, Guillermo; Lacy, Claud H.; Pavlovski, K.; Fekel, Francis C.; Muterspaugh, Matthew W.

doi:10.1088/0004-6256/150/5/154

Cited by 17 publications

(21 citation statements)

References 58 publications

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“…( 7) (Giménez & Bastero 1995). With the value of the eccentricity e = 0.1339 ± 0.0006, this ∆P value yields an apsidal motion rate of ω = 0.00046 ± 0.00011 deg cycle −1 , which is in excellent agreement with the value published by Torres et al (2015) but with a reduced uncertainty. Figure 5 displays the linear best fit to primary and secondary individual timings.…”

Section: V501 Monsupporting

confidence: 87%

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

Baroch,

Giménez,

Ribas

et al. 2021

Preprint

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Context. The change in the argument of periastron of eclipsing binaries, that is, the apsidal motion caused by classical and relativistic effects, can be measured from variations in the difference between the time of minimum light of the primary and secondary eclipses. Poor apsidal motion rate determinations and large uncertainties in the classical term have hampered previous attempts to determine the general relativistic term with sufficient precision to test general relativity predictions. Aims. As a product of the TESS mission, thousands of high-precision light curves from eclipsing binaries are now available. Using a selection of suitable well-studied eccentric eclipsing binary systems, we aim to determine their apsidal motion rates and place constraints on key gravitational parameters. Methods. We compute the time of minimum light from the TESS light curves of 15 eclipsing binaries with precise absolute parameters and with an expected general relativistic contribution to the total apsidal motion rate of greater than 60%. We use the changing primary and secondary eclipse timing differences over time to compute the apsidal motion rate, when possible, or the difference between the linear periods as computed from primary and secondary eclipses. For a greater time baseline we carefully combine the high-precision TESS timings with archival reliable timings. Results. We determine the apsidal motion rate of 9 eclipsing binaries, 5 of which are reported for the first time. From these, we are able to measure the general relativistic apsidal motion rate of 6 systems with sufficient precision to test general relativity for the first time using this method. This test explores a regime of gravitational forces and potentials that had not been probed before. We find perfect agreement with theoretical predictions, and we are able to set stringent constraints on two parameters of the parametrised post-Newtonian formalism.

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Section: V501 Monsupporting

confidence: 87%

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

Baroch,

Giménez,

Ribas

et al. 2021

Preprint

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“…We have examined the literature on other eclipsing Am stars, but have not found as clear a case as this. V501 Mon (Torres et al 2015) is a system with parameters similar to KIC 9777062, and would be a good candidate to further study this effect.…”

Section: Binary Star Modelingmentioning

confidence: 99%

THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY^∗

Sandquist

Jessen-Hansen

Shetrone³

et al. 2016

ApJ

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We present the analysis of an eccentric, partially eclipsing long-period (P = 19.23 d) binary system KIC 9777062 that contains main sequence stars near the turnoff of the intermediate age open cluster NGC 6811. The primary is a metal-lined Am star with a possible convective blueshift to its radial velocities, and one star (probably the secondary) is likely to be a γ Dor pulsator. The component masses are 1.603 ± 0.006(stat.)±0.016(sys.) and 1.419 ± 0.003 ± 0.008M , and the radii are 1.744 ± 0.004 ± 0.002 and 1.544 ± 0.002 ± 0.002R . The isochrone ages of the stars are mildly inconsistent: the age from the mass-radius combination for the primary (1.05±0.05±0.09 Gyr, where the last quote was systematic uncertainty from models and metallicity) is smaller than that from the secondary (1.21 ± 0.05 ± 0.15 Gyr) and is consistent with the inference from the color-magnitude diagram (1.00 ± 0.05 Gyr). We have improved the measurements of the asteroseismic parameters ∆ν and ν max for helium-burning stars in the cluster. The masses of the stars appear to be larger (or alternately, the radii appear to be smaller) than predicted from isochrones using the ages derived from the eclipsing stars. The majority of stars near the cluster turnoff are pulsating stars: we identify a sample of 28 δ Sct, 15 γ Dor, and 5 hybrid types. We used the period-luminosity relation for high-amplitude δ Sct stars to fit the ensemble of the strongest frequencies for the cluster members, finding (m − M ) V = 10.37 ± 0.03. This is larger than most previous determinations, but smaller than values derived from the eclipsing binary (10.47 ± 0.05).

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“…Radial velocities (RVs) for the two components were measured as described by Torres et al (2015) with the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994), using templates taken from a precomputed library of synthetic spectra based on model atmospheres by R. L. Kurucz for solar metallicity (see Nordström et al 1994;Latham et al 2002). The optimal template for each star was found by running grids of cross-correlations over a wide range of effective temperatures (T eff ) and rotational broadenings (v sin i) following Torres et al (2002), and selecting the combination giving the highest cross-correlation value averaged over all observations, with weights set by the strength of each exposure.…”

Section: Hjdmentioning

confidence: 99%

The detached, evolved post-mass-exchange binary V643 Orionis

Andersen,

Torres,

Clausen

2019

Preprint

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Context. One of the greatest uncertainties in modelling the mass-exchange phases during the evolution of a binary system is the amount of mass and angular momentum that has been lost from the system. In order to constrain this problem, a favourable, evolved and detached real binary system is valuable as an example of the end result of this process.Aims. We study the 52-day post-mass-exchange eclipsing binary V643 Ori from complete uvby light curves and highresolution spectra. V643 Ori is double-lined and shows total primary eclipses. The orbit is accurately circular and the rotation of both stars synchronised with the orbit, but the photometry from a single year (1993) shows signs of weak spot activity (0.02 mag) around the primary eclipse. Methods. We determine accurate masses of 3.3 and 1.9 M⊙ from the spectroscopic orbit and solve the four light curves to determine radii of 16 and 21 R⊙, using the Wilson-Devinney photometric code. The rotational velocities from the cross-correlation profiles agree well with those computed from the known radii and orbital parameters. All observable parameters are thus very precisely determined, but the masses and radii of V643 Ori are incompatible with undisturbed post-main-sequence evolution.Results. We have attempted to simulate the past evolutionary history of V643 Ori under both conservative and nonconservative Case B mass transfer scenarios. In the non-conservative case we varied the amounts of mass and angular momentum loss needed to arrive at the present masses in a circular 52-day orbit, keeping the two stars detached and synchronized as now observed, but without following the evolution of other stellar properties in any detail. Multiple possible solutions were found. Further attempts were made using both the BSE formalism and the binary MESA code in order to track stellar evolution more closely, and make use of the measured radii and temperatures as important additional constraints. Those efforts did not yield satisfactory solutions, possibly due to limitations in handling mass transfer in evolved stars such as these. We remain hopeful that future theoreticians can more fully model the system under realistic conditions. Conclusions.

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Absolute Dimensions of the Metallic-Line Eclipsing Binary V501 Monocerotis

Cited by 17 publications

References 58 publications

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY^∗

The detached, evolved post-mass-exchange binary V643 Orionis

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Absolute Dimensions of the Metallic-Line Eclipsing Binary V501 Monocerotis

Cited by 17 publications

References 58 publications

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

Analysis of apsidal motion in eclipsing binaries using TESS data: I. A test of gravitational theories

THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY∗

The detached, evolved post-mass-exchange binary V643 Orionis

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THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY^∗