Anglomathics.

Hazlehurst, Thomas H.

doi:10.1021/ed025p353

Cited by 3 publications

(5 citation statements)

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“…The secular instability of the secondary component of a W UMa type binary arises because they obtain the luminosity transferred from the primary component (Lucy & Wilson 1979;Hazlehurst 1985;Wang 1994). So it could be suggested that decrease in the period of V 781 Tau is caused by the contraction of the secondary component, then its shrinking velocity can be calculated from the decrease rate in the orbital period.…”

Section: Change In the Period And Explanationmentioning

confidence: 99%

A period study of the W UMa type contact binary V 781 Tauri

Liu

Yang

2000

Astron. Astrophys. Suppl. Ser.

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Abstract. New times of minimum light determined from the observations of the W UMa type contact binary V 781 Tau are presented. According to these times of minima and those collected from the references, the change in the orbital period of the system is analyzed. The result reveals that the orbital period of V 781 Tau decreased continually from 1949 to 1998 and the change rate in the period is δp/p = −5.0 10 −11 . The decrease in the period of the binary is explained by a model of the contracting secondary component of the system. The shrinking velocity of 6.77 10 −5 cm s −1 as responsible for the change in the orbital period of the system is obtained, which is in agreement with the results shown in the study of the thermal relaxation oscillation of contact binaries by Wang (1994).

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Section: Change In the Period And Explanationmentioning

confidence: 99%

A period study of the W UMa type contact binary V 781 Tauri

Liu

Yang

2000

Astron. Astrophys. Suppl. Ser.

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“…Note that Lx = 4, but only the range |x| ≤ 2.5 is shown. 100 2 × 50 meshpoints, ∆s = 0.5, R0 = 1.0 factor in understanding contact binaries (Hazlehurst 1985(Hazlehurst , 1996.…”

Section: Discussionmentioning

confidence: 99%

“…The initial entropy excess of the bubble is given by the parameter ∆s. [In all cases presented we take ∆s = 0.5, which corresponds to the value used by Hazlehurst (1985), who adopts units where the nondimensional specific entropy is larger by a factor of 5. We note that larger values of ∆s make the bubble rise faster, but we found that even for ∆s = 2 the motion remained subsonic.…”

Section: Initial and Boundary Conditionsmentioning

confidence: 99%

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Evolution of highly buoyant thermals in a stratified layer

Brandenburg

Hazlehurst

2001

A&A

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Abstract. The buoyant rise of thermals (i.e. bubbles of enhanced entropy, but initially in pressure equilibrium) is investigated numerically in three dimensions for the case of an adiabatically stratified layer covering 6-9 pressure scale heights. It is found that these bubbles can travel to large heights before being braked by the excess pressure that builds up in order to drive the gas sideways in the head of the bubble. Until this happens, the momentum of the bubble grows as described by the time-integrated buoyancy force. This validates the simple theory of bubble dynamics whereby the mass entrainment of the bubble provides an effective braking force well before the bubble stops ascending. This is quantified by an entrainment parameter alpha which is calculated from the simulations and is found to be in good agreement with the experimental measurements. This work is discussed in the context of contact binaries whose secondaries could be subject to dissipative heating in the outermost layers.

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“…Secular instability of the secondary component of a W UMa type contact binary arises as it obtains the luminosity transferred from the primary component (Lucy & Wilson 1979;Hazlehurst 1985;Wang 1994). Wang (1994) studied the interaction between the secondary and the common convective envelope in contact binaries, and suggested that the two subtypes of W UMa type binaries may be in two different states of thermal relaxation oscillation: in the W-subtypes, the secondary is shrinking; while in the A-subtypes, the secondary is swelling.…”

Section: Contraction Of the Secondary And Mass Transfermentioning

confidence: 99%

On the Period Variation of the W UMa-type Contact Binary V502 Ophiuchi

Liu

Yang

2006

Chin. J. Astron. Astrophys.

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The variation in the orbital period of the W UMa type contact binary V502 Oph is analyzed. The orbital period exhibits a wavelike variation with a periodicity of 23.0 years and an amplitude of ∆P = 1.24 × 10 −6 days superimposed on secular decrease of dP/dt = 1.68 × 10 −7 day per year. The long-term decrease may be accompanied by the contraction of the secondary at a rate of 83 m per year and a mass transfer rate from the primary to the secondary of 4.28 × 10 −8 M per year. The short-term oscillation may be explained by the presence of a third component. Orbital elements of the third body and its possible mass are presented.

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Anglomathics.

Abstract: The title of this paper was proposed to the writer with the explanation that it signifies "translating the sense of problems and relationships among factors into mathematics.

Cited by 3 publications

References 0 publications

A period study of the W UMa type contact binary V 781 Tauri

A period study of the W UMa type contact binary V 781 Tauri

Evolution of highly buoyant thermals in a stratified layer

On the Period Variation of the W UMa-type Contact Binary V502 Ophiuchi

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