Results 11 to 20 of about 2,489,433 (294)

Small Mass Ratio Contact Binary [PDF]

Journal of Astronomy and Space Sciences, 2003
The contact binary system has been classified in five different types according to their physical properties.
Kyu-Dong Oh, Chun-Hwey Kim, Young Woon Kang, Yonggi Kim   +3 more
doaj   +6 more sources

Low Mass Ratio Contact Binary V410 Aur and V776 Cas - II [PDF]

Journal of Astronomy and Space Sciences, 2005
New BVR CCD light curves of the low mass ratio contact binaries, V410 Aur and V776 Cas, were observed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Astronomical Observatory.
Kyu-Dong Oh, Chun-Hwey Kim, Ho-iL Kim
doaj   +3 more sources

Statistical Survey for the Physical Characteristic of Near Contact Binary(NCBs) [PDF]

Journal of Astronomy and Space Sciences, 2005
The absolute dimensions and orbital elements of 66 near contact binaries, collected from literatures, have been analyzed to investigate the physical characteristics of the near contact binaries as well as co-relations among physical parameters.
Kyu-Dong Oh
doaj   +3 more sources

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

CCD Photometry of Low Mass Ratio Contact Binary FP Boo - IV [PDF]

Journal of Astronomy and Space Sciences, 2009
We present new B, V, and R CCD photometric light curves for the low mass ratio contact binary FP Boo. A new photometric solution and absolute physical dimensions of the system were derived by applying the Wilson-Devinney program to our observed light ...
Kyu-Dong Oh, Woo-Baik Lee
doaj   +3 more sources

Low Mass Ratio Contact Binary Systems HN UMa and II UMa - III [PDF]

Journal of Astronomy and Space Sciences, 2006
We present newly observed BVRI CCD light curves for low mass ratio contact binaries, HN UMa and II UMa. The absolute dimensions of these objects were obtained by applying the Wilson-Devinney program to previously published spectroscopic analysis and to ...
Woo-Baik Lee, Ho-il Kim, Young Woon Kang, Kyu-Dong Oh   +3 more
doaj   +3 more sources

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
doaj   +3 more sources

Mass-ratio distribution of contact binary stars [PDF]

, 2023
The mass ratio $q$ of a contact binary star evolves due to mass transfer, magnetic braking, and thermal relaxation oscillations to small values until it crosses a critical threshold $q_\text{min}$. When that happens, the binary undergoes the tidal Darwin
Pešta, Milan, Ondřej Pejcha, Pejcha, Ondřej, Milan Pešta   +3 more
core   +2 more sources

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
  +13 more sources

CCD Photometry of Contact Binary WZ Cephei [PDF]

Journal of Astronomy and Space Sciences, 2008
We present the full BVR light curves and five times of minima of WZ Cep to provides a complete photometric solution and to confirm the long term variation of the light curves.
Woo-Baik Lee, Young-Woon Kang, Kyu-Dong Oh   +2 more
doaj   +1 more source