The triple system DM Persei

Hilditch, R. W.; Skillen, I.; Carr, D. M.; Aikman, G. C. L.

doi:10.1093/mnras/222.1.167

Cited by 10 publications

(13 citation statements)

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“…DM Persei is an Algol-type binary with P % 2:73 days and one of the better known multiple systems that contain an EB, a condition discovered by Hilditch in 1970(Hilditch et al 1986). 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.…”

Section: Dm Perseimentioning

confidence: 99%

“…Aims were to explore DM Per's 3b period space and measure the 3b orbit parameters reliably, with tests of our assumptions by dynamical experiments. 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%

“…Hilditch et al (1986) speculate that ''it is probable that the third body spectrum could be detected on highresolution, high signal-to-noise spectra.'' However, they were thinking of a smaller amount of l 3 than we find, so their nondetection by cross-correlation remains problematic.…”

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: 99%

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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Stellar and Dynamical Evolution within Triple Stars

Eggleton¹,

Kiseleva²

1996

Evolutionary Processes in Binary Stars

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About 5-15% of stellar systems are at least triple. About 1% of systems with a primary of > 1 M are triple with a longer period that is less than 30y, and so may in principle be capable of Roche-lobe over ow in both the inner and the outer orbits, at di erent times. We discuss possible evolutionary paths for these systems, some of which may lead to objects that are di cult to understand in the context of purely binary evolution. An example is OW Gem, a binary containing two supergiants (spectral types F and G) with masses that di fer by a factor of 1.5. There is also a triple-star pathway which could lead rather naturally to low-mass X-ray binaries; whereas binary pathways often appear rather contrived. We also discuss some dynamical processes involved in the 3-body problem. A number of triple stars are found in clusters. Similar systems can be created by gravitational capture during N-body simulations of Galactic clusters, especially if there is an assumed primordial binary population. We discuss the properties of these triples, and note that many can be quite long-lived.

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Angular momenta in binary systems

Quiroga¹,

Vaz²

1988

Astrophys Space Sci

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The triple system DM Persei

Cited by 10 publications

References 0 publications

Third‐Body Parameters from Whole Light and Velocity Curves

Third‐Body Parameters from Whole Light and Velocity Curves

Stellar and Dynamical Evolution within Triple Stars

Angular momenta in binary systems

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