Optimizing Reservoir Performance by Automatic Allocation of Well Rates

Zakirov, I. M.; Aanonsen, Sigurd Ivar; Zakirov, E. S.; Palatnik, B. M.

doi:10.3997/2214-4609.201406895

Cited by 76 publications

(37 citation statements)

References 5 publications

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“…Precise absolute dimensions of the components of V478 Cyg were derived spectroscopically by Popper & Hill (1991), who obtained components with identical mass and size M 1 = 16.6 ± 0.9 M , M 2 = 16.3 ± 0.9 M , R 1 = 7.43 ± 0.12 R , R 2 = 7.43 ± 0.12 R . Zakirov (1993) in his photometric study presented only a phase of the primary minimum as 0.0042 ± 2 according to the ephemeris of Popper & Etzel (1981). Finally, • 3873, Sp.…”

Section: V478 Cygmentioning

confidence: 96%

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Apsidal motion in eccentric eclipsing binaries: CW Cephei, V478 Cygni, AG Persei, and IQ Persei

Wolf¹,

Kučáková²,

Kolasa³

et al. 2006

A&A

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Aims. About thirty new times of minimum light recorded with photoelectric or CCD photometers were obtained for four earlytype eccentric-orbit eclipsing binaries CW Cep (P = 2. Their O−C diagrams were analysed using all reliable timings found in the literature, and elements of apsidal motion were improved. Results. We confirm relatively short periods of apsidal motion of about 46, 27, 76, and 124 years for CW Cep, V478 Cyg, AG Per, and IQ Per, respectively. The corresponding internal structure constants, log k 2 , are then found to be -2.12, -2.25, -2.15, and -2.36, under the assumption that the component stars rotate pseudosynchronously. The relativistic effects are negligible, being up to 8% of the total apsidal motion rate in all systems. Using the light-time effect solution, we have predicted a faint third component orbiting with a period of about 39 years for CW Cep.

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Section: V478 Cygmentioning

confidence: 96%

“…• 73, based on the photometric analysis (Zakirov 1993). The computed apsidal motion parameters and their internal errors of the least-squares fit are given in Table 2.…”

Section: V478 Cygmentioning

confidence: 99%

Apsidal motion in eccentric eclipsing binaries: CW Cephei, V478 Cygni, AG Persei, and IQ Persei

Wolf¹,

Kučáková²,

Kolasa³

et al. 2006

A&A

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show abstract

“…The earlier observations of EK Cep were mainly photometric and spectral observations of the variable, which yielded values for the system parameters and permitted some improvement in these values [7].…”

Section: Observationsmentioning

confidence: 99%

UBVRI photometry and polarimetry of the young eclipsing binary EK Cep

Antonyuk

Rostopchina

2009

Astrophysics

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Multicolor photometric and polarimetric observations of the eclipsing binary EK Cep at the Crimean Astrophysical Observatory in 1995 and 2006-2007 are reported. Polarimetric observations were made of stars in the neighborhood of EK Cep. It is shown that the observed linear polarization of EK Cep is determined by a variable circumstellar constituent, as well as by the interstellar component. Various possible mechanisms for formation of the intrinsic polarization of binary stars are discussed.

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“…22717.28 +0.12 [3] 23830.18 +0.08 [3] 30792.50 +0.07 [3] 31148.35 +0.04 [3] 40265.339 +0.001 [2] 42381.200 -0.013 [4] 49673.463 -0.080 [5] O …”

Section: The Star Bm Ori Has Been Studied By Many Researchersmentioning

confidence: 99%

The system Bm Ori. V. Improved photometric elements

Vitrichenko

2008

Astrophysics

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The times of individual minima taken from the literature are used to plot the dependence of O-C on revolution number for the eclipsing star BM Ori. A least squares fit of this plot yields the following photometric elements: Min I=JD2440265.331(5)+6.470524(3)·E. Determining the photometric elements of the eclipsing star BM Ori involves two difficultiesThe first is the instability of the light curve. BM Ori displays sporadic bursts with a characteristic duration of ~2 h [1]. The second difficulty is an excessively long duration of the minima, which makes it hard to determine the time of the minimum within a single night.The purpose of this paper is to collect all the available observations of the individual (or seasonal) times of the minima and to determine more precise photometric elements using them. The star BM Ori has been studied by many researchersSome of them have determined the times of minima, but in the overwhelming majority of cases, not for an individual minimum (This is essentially impossible to do because of its long duration.), but from an average light

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Optimizing Reservoir Performance by Automatic Allocation of Well Rates

Cited by 76 publications

References 5 publications

Apsidal motion in eccentric eclipsing binaries: CW Cephei, V478 Cygni, AG Persei, and IQ Persei

Apsidal motion in eccentric eclipsing binaries: CW Cephei, V478 Cygni, AG Persei, and IQ Persei

UBVRI photometry and polarimetry of the young eclipsing binary EK Cep

The system Bm Ori. V. Improved photometric elements

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