The triple system DM Persei revisited

Hilditch, R. W.; Hill, Graham; Khalesseh, B.

doi:10.1093/mnras/254.1.82

Cited by 6 publications

(9 citation statements)

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“…The 3b period was found to be very close to 98 days by Hilditch et al (1992), who discuss how they arrived at that period after considering alternatives. DM Per's early history is covered in those papers and in others such as Colacevich (1950) and Scaltriti (1976).…”

Section: Dm Perseimentioning

confidence: 92%

“…Our period explorations applied power spectral analysis via Lomb-Scargle, as did Hilditch et al (1986) and also CLEAN periodograms, while parameter estimation applied our ideas of the foregoing sections on simultaneous solutions of whole light and velocity curves. The 3b orbit was assumed circular, as Figure 2 of Hilditch et al (1992) (residuals from two-body motion) appears to be essentially a cosine wave.…”

Section: Dm Perseimentioning

confidence: 99%

“…The spherical and rectifiable models applied in the early papers operate only graphically and have great difficulty finding l 3 quantitatively for partially eclipsing systems. The two Hilditch et al contributions (Hilditch et al 1986(Hilditch et al , 1992 utilized the Hill (1979) physical model, but third-light experiments were limited to l 3 ¼ 0 and one other fixed value. Their very brief comments in those papers essentially say that l 3 had little effect on solutions, in disagreement with our experience.…”

Section: Dm Per Solutionsmentioning

confidence: 99%

“…However, we looked without success for reports of spectral lines of the third object, which should be seen if l 3 is as large as the solution indicates. Hilditch et al (1992) looked for evidence of a third star in their velocity cross-correlation diagrams and found none. Chambliss (1992) suggested that the third object may itself be a binary and thereby have as much as roughly a factor of 10 lower light-tomass ratio than if it were one star, an explanation that would seem plausible in the absence of our solution that does find substantial third light.…”

Section: Dm Per Solutionsmentioning

confidence: 99%

“…One reason is that the relative 3b information content of light and RV data is not always obvious at the start of work, while another is the ease of adding new or newly found data of either type as work proceeds, and a third is the capability to access whatever subtle 3b information may be in the other kind of data even when that information is not sufficient for a stand-alone determination of 3b parameters. Still another advantage is that corrections to the observations, such as the intricate iterative ones described by Hilditch et al (1986Hilditch et al ( , 1992, are no longer needed: all phenomena are intrinsic to the model and the observations are used just as they are. Statistics of multiple systems that are needed to check star formation and orbital evolution theories are not well established due to glare of primaries and companion faintness, but they can sometimes be measured for a system that includes an EB.…”

Section: Introductionmentioning

confidence: 99%

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Third‐Body Parameters from Whole Light and Velocity Curves

Hamme

Wilson

2007

ApJ

234

145

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Eclipsing binaries can improve multiple system statistics via the light-time effect and radial velocity shifts. Here an algorithm operates on data of mixed type to exploit these opportunities. Main reasons for enhanced reliability are that (1) combined light and velocity curves give better timewise coverage than either type alone, (2) properly weighted solutions impersonally balance light and velocity information, and (3) the entire theory is within the computer model, so observations are used directly without corrections. A brief history of mixed whole-curve solutions is given and the relative importance of light-time and radial velocity input for third-body parameters is discussed and quantified. Period sifting by power spectral analysis is essentially indispensable in preliminary work. Applications are to the Algol-type system DM Persei and the detached system VV Orionis. An assumption of coplanarity for DM Per's inner and outer orbits is tested and quantified by dynamical experiments. Derived third-body parameters for DM Per are mainly reasonable and self-consistent. For comparison with whole-curve results, we also investigated DM Per's ephemeris in terms of eclipse timings and found whole-curve solutions to give smaller standard errors in reference epoch (T 0 ), binary orbit period (P), and dP/dt, over a similar baseline in time. An astonishing outcome is lack of evidence that can pass reasonable validity tests for VV Ori's well-accepted third star with P % 120 days. Estimates of third light do indicate a third star, but the correct period cannot now be established, so the star cannot be identified as the one heretofore recognized from radial velocity evidence. The much cited 120 day period appears to be an artifact of the window function for VV Ori's historical velocity observations.

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Section: Dm Perseimentioning

confidence: 92%

Section: Dm Perseimentioning

confidence: 99%

Section: Dm Per Solutionsmentioning

confidence: 99%

Section: Dm Per Solutionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Third‐Body Parameters from Whole Light and Velocity Curves

Hamme

Wilson

2007

ApJ

234

145

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Spectroscopic Orbit of the Eclipsing Binary BD +52°2009

Khalesseh

1999

International Astronomical Union Colloquium

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Abstract. New radial velocity measurements of the Algol-type eclipsing binary BD +52 °2009, based on Reticon observations, are presented. The velocity measures are based on fitting theoretical profiles, generated by a physical model of the binary, to the observed cross-correlation function (ccf). Such profiles match this function very well, much better in fact than Gaussian profiles, which are generally used. Measuring the ccf's with Gaussian profiles yields the following results: m p sin 3 i = 2.55 ± 0.05m @ , m s sin 3 i = 1.14 ± 0.03m @ , (a p + a s ) sin i = 7.34 ± O.O5i? 0 , and m p /m s = 2.23 ± 0.05. However, measuring the ccf's with theoretical profiles yields a mass ratio of 2.33 and following results: m p sin 3 i = 2.84 ± 0.05m®, m s sin 3 i = 1.22 ± O.O3m 0 , (a p + a s ) sin i = 7.56 ± 0.05R @ . The system has a semi-detached configuration. By combining the solution of a previously published light curve with the spectroscopic orbit, one can obtain the following physical parameters: m p = 2.99m @ , m 3 = 1.28m0, < T p >= 9600K, < T s >= 5400K, < R p >= 2.35i? 0 , < R s >= 2.12R®. The system consists of an A0 primary and a G2 secondary.

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Automatic classification of eclipsing binaries light curves using neural networks

Sarro¹,

Sánchez–Fernández

Giménez³

2006

A&A

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In this work we present a system for the automatic classification of the light curves of eclipsing binaries. This system is based on a classification scheme that aims to separate eclipsing binary systems according to their geometrical configuration in a modified version of the traditional classification scheme. The classification is performed by a Bayesian ensemble of neural networks trained with Hipparcos data of seven different categories including eccentric binary systems and two types of pulsating light curve morphologies.

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The triple system DM Persei revisited

Cited by 6 publications

References 0 publications

Third‐Body Parameters from Whole Light and Velocity Curves

Third‐Body Parameters from Whole Light and Velocity Curves

Spectroscopic Orbit of the Eclipsing Binary BD +52°2009

Automatic classification of eclipsing binaries light curves using neural networks

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