Mitteilungen über Veränderliche der Bamberger Himmelsüberwachung (Veröffentlichungen der Remeis‐Sternwarte Bamberg, Band V, Nr. 10)

Strohmeier, W.; Knigge, R.

doi:10.1002/asna.19612860312

Cited by 54 publications

(57 citation statements)

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“…A1V+A1V) is a known close binary system with a slightly eccentric orbit (e = 0.024) and a longer orbital period of about 8.5 days. It was discovered to be variable by Strohmeier (1955). The first light elements were measured by Meinunger & Wenzel (1967), who also recognized that the orbit is eccentric.…”

Section: V459 Casmentioning

confidence: 99%

Relativistic apsidal motion in eccentric eclipsing binaries

Wolf¹,

Claret²,

Kotková

et al. 2010

A&A

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Context. The study of apsidal motion in detached eclipsing binary systems is known to be an important source of information about stellar internal structure as well as the possibility of verifying of General Relativity outside the Solar System. Aims. As part of the long-term Ondřejov and Ostrava observational projects, we aim to measure precise times of minima for eccentric eclipsing binaries, needed for the accurate determination of apsidal motion, providing a suitable test of the effects of General Relativity. Methods. About seventy new times of minimum light recorded with photoelectric or CCD photometers were obtained for ten eccentric-orbit eclipsing binaries with significant relativistic apsidal motion. Their O-C diagrams were analysed using all reliable timings found in the literature, and new or improved elements of apsidal motion were obtained. Results. We confirm very long periods of apsidal motion for all systems. For BF Dra and V1094 Tau, we present the first apsidalmotion solution. The relativistic effects are dominant, representing up to 100% of the total observable apsidal-motion rate in several systems. The theoretical and observed values of the internal structure constant k 2 were compared for systems with lower relativistic contribution. Using the light-time effect solution, we predict a faint third component for V1094 Tau orbiting with a short period of about 8 years.

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Section: V459 Casmentioning

confidence: 99%

Relativistic apsidal motion in eccentric eclipsing binaries

Wolf¹,

Claret²,

Kotková

et al. 2010

A&A

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“…A0) is a seldom studied binary system with a short orbital period (P = 1.5 d) and a slightly eccentric orbit (e = 0.07). It was discovered to be variable by Hoffmeister (1949) at Sonneberg and later independently by Strohmeier (1961) at Bamberg observatory. Busch & Haussler (1966) derived the first ephemeris with the correct orbital period:…”

Section: V796 Cygnimentioning

confidence: 99%

“…All prevous times of minimum light are collected in the O−C Gateway database. Only those given in Table A.3 were taken into consideration, and other numerous photographic times obtained by Busch & Haussler (1966), Strohmeier (1966), and Strohmeier & Bauernfeind (1968) were not used in our analysis due to large scatter of these data. A total of 18 reliable times of minimum light were included in our analysis, with 9 secondary eclipses among them.…”

Section: V796 Cygnimentioning

confidence: 99%

Apsidal motion in five eccentric eclipsing binaries

Wolf

Zasche

Kučáková³

et al. 2013

A&A

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Aims. As part of the long-term Ondřejov and Ostrava observational projects, we aim to measure the precise times of minimum light for eccentric eclipsing binaries, needed for accurate determination of apsidal motion. Over fifty new times of minimum light recorded with CCD photometers were obtained for five early-type and eccentric-orbit eclipsing binaries: V785 Cas (P = 2. Methods. O−C diagrams of binaries were analysed using all reliable timings found in the literature, and new elements of apsidal motion were obtained. Results. We derived for the first time or improved the relatively short periods of apsidal motion of about 83, 140, 33, 440, and 70 years for V785 Cas, V821 Cas, V796 Cyg, V398 Lac, and V871 Per, respectively. The internal structure constants, log k 2 , for V821 Cas and V398 Lac are then found to be -2.70 and -2.35, under the assumption that the component stars rotate pseudosynchronously. The relativistic effects are weak, up to 7% of the total apsidal motion rate.

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“…The binary system EE Aqr (HD213863, BD-20 • 6454, SAO 191236, α 2000 = 22 h 34 m 41 s .87, δ 2000 = 19 • 51 ′ 34 ′′ ) was discovered to be variable by Strohmeier & Knigge (1960). Strohmeier et al (1962) derived its eclipsing behavior with a orbital period of 0.51 d and classified it as an Algol (EA) type eclipsing binary.…”

Section: Ee Aqrmentioning

confidence: 99%

Reanalysis of two eclipsing binaries: EE Aqr and Z Vul

Ghoreyshi

Ghanbari

Salehi

2008

Astrophys Space Sci

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We study the radial-velocity and light curves of the two eclipsing binaries EE Aqr and Z V ul. Using the latest version of the Wilson & Van Hamme (2003) model, absolute parameters for the systems are determined. We find that EE Aqr and Z V ul are nearcontact and semi-detached systems, respectively. The primary component of EE Aqr fills about 96% of its 'Roche lobe', while its secondary one appears close to completely filling this limiting volume. In a similar way, we find fill-out proportions of about 72 and 100% of these volumes for the primary and secondary components of Z V ul respectively. We compare our results with those of previous authors.

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Mitteilungen über Veränderliche der Bamberger Himmelsüberwachung (Veröffentlichungen der Remeis‐Sternwarte Bamberg, Band V, Nr. 10)

Cited by 54 publications

References 0 publications

Relativistic apsidal motion in eccentric eclipsing binaries

Relativistic apsidal motion in eccentric eclipsing binaries

Apsidal motion in five eccentric eclipsing binaries

Reanalysis of two eclipsing binaries: EE Aqr and Z Vul

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