Results 11 to 20 of about 806,657 (286)

The Strength and Shapes of Contact Binary Objects

The Astrophysical Journal Letters
While contact binary objects are common in the solar system, their formation mechanism is unclear. In this work we examine several contact binaries and calculate the necessary strength parameters that allow the two lobes to merge without the smaller of ...
Alex J. Meyer, Daniel J. Scheeres
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Modeling contact binaries

Astronomy & Astrophysics, 2023
Context. Among massive stars, binary interaction is the rule rather than the exception. The closest binaries – those with periods of less than ∼10 days – undergo mass transfer during core-hydrogen burning, with many of them experiencing a nuclear-timescale contact phase.
Fabry, M., Marchant, P., Langer, N., Sana, H.   +3 more
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Determinations of its Absolute Dimensions and Distance by the Analyses of Light and Radial-Velocity Curves of the Contact Binary -I. V417 Aquilae [PDF]

Journal of Astronomy and Space Sciences, 2004
New photometric and spectroscopic solutions of W-type overcontact binary V417 Aql were obtained by solving the UBV light curves of Samec et al. (1997) and radial-velocity ones of Lu & Rucinski (1999) with the 2003 version of the Wilson-Devinney binary ...
Jae Woo Lee, Chun-Hwey Kim, Chung-Uk Lee, Kyu-Dong Oh   +3 more
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Activity of Contact Binaries [PDF]

International Astronomical Union Colloquium, 1983
We discuss observational results for indicators of elevated activity of contact (W UMa-type) binaries. References are made to results for fast rotating single and detached binary (MS) stars: they are discussed in the accompanying paper by Vilhu and Rucinski.
S.M. Rucinski, O. Vilhu, J. Kaluzny
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The Evolution of a Contact Binary [PDF]

International Astronomical Union Colloquium, 1971
Test calculations have been made to study the effects of central hydrogen depletion, luminosity exchange and mass exchange on the evolution of a contact binary. The Munich Henyey programme was adapted to allow the study of both components in a time-dependent way.The first model considered was that of LUCY (Ap. J.
J. Hazlehurst, E. Meyer-Hofmeister
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A contact binary satellite of the asteroid (152830) Dinkinesh. [PDF]

Nature
Abstract Asteroids with diameters less than about 5 km have complex histories because they are small enough for radiative torques (that is, YORP, short for the Yarkovsky–O’Keefe–Radzievskii–Paddack effect) 1 to be a notable factor in their evolution 2
Levison HF, Marchi S, Noll KS, Spencer JR, Statler TS, Bell JF, Bierhaus EB, Binzel R, Bottke WF, Britt D, Brown ME, Buie MW, Christensen PR, Dello Russo N, Emery JP, Grundy WM, Hahn M, Hamilton VE, Howett C, Kaplan H, Kretke K, Lauer TR, Manzoni C, Marschall R, Martin AC, May BH, Mottola S, Olkin CB, Pätzold M, Parker JW, Porter S, Preusker F, Protopapa S, Reuter DC, Robbins SJ, Salmon J, Simon AA, Stern SA, Sunshine JM, Wong I, Weaver HA, Adam C, Ancheta S, Andrews J, Anwar S, Barnouin OS, Beasley M, Berry KE, Birath E, Bolin B, Booco M, Burns R, Campbell P, Carpenter R, Crombie K, Effertz M, Eifert E, Ellis C, Faiks P, Fischetti J, Fleming P, Francis K, Franco R, Freund S, Gallagher C, Geeraert J, Gobat C, Gorgas D, Granat C, Gray S, Haas P, Harch A, Hegedus K, Isabelle C, Jackson B, Jacob T, Jennings S, Kaufmann D, Keeney BA, Kennedy T, Lauffer K, Lessac-Chenen E, Leonard R, Levine A, Lunsford A, Martin T, McAdams J, Mehall G, Merkley T, Miller G, Montanaro M, Montgomery A, Murphy G, Myers M, Nelson DS, Ocampo A, Olds R, Pelgrift JY, Perkins T, Pineau J, Poland D, Ramanan V, Rose D, Sahr E, Short O, Solanki I, Stanbridge D, Sutter B, Talpas Z, Taylor H, Treiu B, Vermeer N, Vincent M, Wallace M, Weigle G, Wibben DR, Wiens Z, Wilson JP, Zhao Y.   +118 more
europepmc   +7 more sources

Models for Contact Binaries [PDF]

International Astronomical Union Colloquium, 1971
The well-known problem one has in constructing zero age contact binaries stems from the fact that given two mass values, the ratio of the radii for zero age stellar models differs from that derived from the Roche model (KUIPER 1941). Therefore one cannot achieve contact by adjusting just the distance of the two stars, since if for instance the distance
Peter Biermann, H.-C. Thomas
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Detection and Seismic Study of Gravity and Rossby Mode Pulsations in Four Contact Binaries

The Astrophysical Journal, 2023
We report the detection of gravity ( g ) and Rossby ( r ) mode pulsations of four short-period eclipsing binaries, KIC 5439790, KIC 7501230, KIC 9350889, and KIC 9453192 based on the 4 yr Kepler high-precision photometry.
X. B. Zhang, Xinghao Chen, Jianning Fu, Yan Li   +3 more
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Contact Binaries [PDF]

Symposium - International Astronomical Union, 1986
The most promising mechanism for the formation of contact binaries involves the orbital angular momentum loss (AML) and the resulting orbital decay of detached but close synchronized binaries. The efficiency of magnetic wind braking should abruptly decrease upon formation of a contact binary because of the transformation into a system of earlier ...
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The lifetime of contact binaries [PDF]

Proceedings of the International Astronomical Union, 2012
AbstractThe lifetime of contact binaries is an important parameter for studying the evolution of contact binaries. By reproducing the relative frequency of occurrence for contact binaries, we found that the lifetime of contact binaries decreases with increasing mass of the primaries. The lifetime of contact binaries is about 4%–10% of the main sequence
D. K. Jiang, Z. W. Han, L. H. Yang, L. F. Li   +3 more
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