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Relevant bibliographies by topics / Roche-equipotential

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Journal articles

Academic literature on the topic 'Roche-equipotential'

Author: Grafiati

Published: 3 June 2025

Last updated: 31 July 2025

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Journal articles on the topic "Roche-equipotential"

1

Pathania, A., and T. Medupe. "Radius of the Roche equipotential surfaces." Astrophysics and Space Science 338, no. 1 (2011): 127–45. http://dx.doi.org/10.1007/s10509-011-0928-y.

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2

Pathania, A., A. K. Lal, and C. Mohan. "Structures and oscillations of rotationally and tidally distorted polytropic models of stars in the presence of the Coriolis force." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 468, no. 2138 (2011): 448–66. http://dx.doi.org/10.1098/rspa.2011.0182.

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The problems of equilibrium structures and periods of oscillations of rotationally and/or tidally distorted polytropic models of stars in binary systems have been studied previously. In the studies, only the effects of gravitational and centrifugal forces while obtaining the Roche equipotential of such stars were considered. The Coriolis force were not considered. In the present study, we have included the effects of the Coriolis force also. The objective of this study is to investigate as to how the inclusion of the Coriolis force in the Roche equipotential affects the equilibrium structures

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3

Pourmand, Ali, and Natalia Ivanova. "Properties of Binary Systems in a One-dimensional Approximation." Astrophysical Journal 952, no. 2 (2023): 126. http://dx.doi.org/10.3847/1538-4357/acd4c1.

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Abstract Evolutionary calculations for stars in close binary systems are in high demand to obtain better constraints on gravitational-wave source progenitors, understand transient events from stellar interactions, and more. Modern one-dimensional (1D) stellar codes make use of the Roche lobe radius R L concept in order to treat stars in binary systems. If the stellar companion is approaching its R L, mass transfer treatment is initiated. However, the effective acceleration also affects the evolution of a star in a close binary system. This is different from the gravity inside a single star, wh

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4

Kamal, Krishan Singh*1 Seema Saini2 Sunil Kumar3 V. P. Singh4 &. Rajendra Kumar5. "THEORETICAL ESTIMATION OF STRUCTURES: DIFFERENTIALLY ROTATING STELLAR MODELS OF NON-UNIFORM MASSES." INTERNATIONAL JOURNAL OF ENGINEERING SCIENCES & RESEARCH TECHNOLOGY 6, no. 7 (2017): 589–95. https://doi.org/10.5281/zenodo.829782.

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A method is proposed to compute equilibrium structures of differentially rotating polytropic stars. The law of differential rotation is assumed to be the form of.The angular velocity of rotation (ω) is a function of distance (s) of a fluid element from the axis of rotation.Kippenhahn and Thomas'saveraging approach and concepts of Roche-equipotential areutilised to incorporate the effects of differential rotation on the equilibrium structures of differentially rotating polytropic stellar models having non-uniform masses. The proposed mathematical modelling can be used to determine structures, o

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5

Saini, Seema, Sunil Kumar, Vineet Bhatt, and Pradeep Bedi. "Non-Radial Pulsations of Distorted Stellar Structures: Effect of Mass Variation." International Journal of Mathematical, Engineering and Management Sciences 6, no. 5 (2021): 1391–405. http://dx.doi.org/10.33889/ijmems.2021.6.5.084.

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Eigen-frequencies (EF) of non–radial modes (NRM) of pulsations of differentially rotating (D R) and tidally distorted (T D) stellar models by considering the effect of mass variation (MV) on its equi-potentials surfaces inside a star. The method utilizes an averaging proposal of Kippenhahn and Thomas (K and T) with conjunction of the concept of Roche-equipotential. The study accolades and corrects earlier studies of non-radial (NR) pulsations of DR and TD stellar structures of different natures such as radial and non-radial oscillations, X-ray, gamma ray and other electromagnetic disturbances.

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6

Lal, A. K., S. Saini, C. Mohan, and V. P. Singh. "On the validity of series expansion being used for the position of a point on a Roche equipotential." Astrophysics and Space Science 310, no. 3-4 (2007): 317–20. http://dx.doi.org/10.1007/s10509-007-9535-3.

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7

Vanbeveren, D. "From LBV Binary to WR+OB Binary." Symposium - International Astronomical Union 143 (1991): 556. http://dx.doi.org/10.1017/s0074180900045812.

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The LBV phase is generally identified with the hydrogen shell burning phase of a star with initial mass larger than 40-50 M⊙ (see also Humphreys, this volume) and therefore in binaries with ZAMS component masses larger than 40-50 M⊙ and periods larger than 4-7 days the primary may experience a LBV mass loss phase before it reaches its critical equipotential surface (the Roche lobe). I then define the ‘LBV scenario’ of massive close binaries as follows:when a binary component (initial mass larger than 40-50 M⊙) reaches the LBV phase prior to its Roche lobe overflow phase (RLOF), a stellar wind

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8

Kazem Ghamsari, Amin K., Trevor Michael Braun, and Christopher Lewis Alexander. "On the Importance of Geometry in Open Bipolar Electrochemistry Configurations for Corrosion Studies." ECS Meeting Abstracts MA2022-02, no. 13 (2022): 781. http://dx.doi.org/10.1149/ma2022-0213781mtgabs.

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This work aims to optimize cell geometry with finite element modeling to ameliorate open Bipolar electrochemistry (BPE) and split BPE setups, increase the faradaic current through the bipolar electrode to trigger localized corrosion on the anodic region, and study the corrosion behavior of anodic films when activated as bipolar electrodes under thermostatic condition. The advent of Bipolar electrochemistry (BPE) stems from a series of investigations on fluidized bed electrodes conducted by Fleischmann et al. in the 1970s.[1] Since then, and mainly in the recent decade, BPE has been profoundly

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9

Wei, Yunzhu, Song-Bai Chen, and Ji-Liang Jing. "Thick accretion disk configurations around a compact object in the brane-world scenario." Communications in Theoretical Physics, August 24, 2023. http://dx.doi.org/10.1088/1572-9494/acf36e.

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Abstract We have studied equipotential surfaces of a thick accretion disk around a Casadio-Fabbri-Mazzacurati (CFM) compact object in the brane-world scenario, which owns a mass parameter together with a parameterized post-newtonian (PPN) parameter. With the increase of the PPN parameter, the size of the thick accretion disk decreases, but the corresponding Roche lobe size increases. Thus, the larger PPN parameter yields the larger region of existing bound disk structures where the fluid is not accreted into the central wormhole. Moreover, with the increase of the PPN parameter, the position o

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10

Ziółkowski, Janusz, and Andrzej A. Zdziarski. "A comment on the properties of the matter flow through the first Langrangian point." Monthly Notices of the Royal Astronomical Society, October 1, 2021. http://dx.doi.org/10.1093/mnras/stab2826.

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Abstract We analyse properties of the mass outflow from the Roche lobe filling component of a semi-detached binary system. We follow the approaches published by Paczyński & Sienkiewicz and by Lubow & Shu, which we compare with other simplified approaches. We find that the density of the flow at L1 is orders of magnitude lower than the density on the same equipotential but away from L1. Furthermore, the effective cross-section of the flow, after averaging over its profile of the momentum density, is much lower than some published estimates done without accounting for the averaging. Thus

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