Results 31 to 40 of about 2,931,024 (350)
The solar nebula origin of (486958) Arrokoth, a primordial contact binary in the Kuiper Belt [PDF]
Science, 2020 Examining Arrokoth The New Horizons spacecraft flew past the Kuiper Belt object (486958) Arrokoth (also known as 2014 MU69) in January 2019. Because of the great distance to the outer Solar System and limited bandwidth, it will take until late 2020 to ...
W. McKinnon +27 more
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ZZ Piscis Austrinus (ZZ PsA): a bright red nova progenitor and the instability mass ratio of contact binary stars [PDF]
Monthly notices of the Royal Astronomical Society, 2020 ZZ Piscis Austrinus (ZZ PsA) is a neglected bright southern contact binary system with maximum V magnitude of 9.26. We present the first multiband photometric analysis and find the system to be in deep contact (>95 per cent) with an extremely low mass ...
S. Wadhwa +6 more
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Photometric Solutions of W UMa Type Stars: GSC2576-0319 and GSC2584-1731 [PDF]
Journal of Astronomy and Space Sciences, 2006 High-precision photometric observations were performed in BVI bandpasses using 1m robotic telescope at Mt. Lemmon Observatory for two binary stars, which are reclassified as W UMa-type systems from ROTSE(Robotic Optical Transient Search Experiment ...
Chung-Uk Lee, Jae Woo Lee, Chun-Hwey Kim
doaj +1 more source
Fast Derivation of Contact Binary Parameters for Large Photometric Surveys
Astronomical Journal, 2022 Thanks to an enormous release of light curves of contact binaries, it is a challenge to derive the parameters of contact binaries using the Phoebe program and the Wilson–Devinney program with the Markov chain Monte Carlo (MCMC) algorithm.
Xu Ding +6 more
semanticscholar +1 more source
Determinations of its Absolute Dimensions and Distance by the Analyses of Light and Radial-Velocity Curves [PDF]
Journal of Astronomy and Space Sciences, 2004 We completed the light curves of the contact binary CK Boo for 13 nights from June to July in 2004 using the 1-m reflector and BVR filters at Mt. Lemmon Optical Astronomy Observatory, and determined four new times of minimum light (three timings for ...
Jae Woo Lee +4 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 +3 more
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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
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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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Chromospheric activity in bright contact binary stars [PDF]
Astronomy & Astrophysics, 2020 Context. Studying chromospheric activity of contact binaries is an effective way of revealing the magnetic activity processes of these systems. One efficient but somewhat neglected method for this purpose is to follow the changes of the Hα line profiles ...
T. Mitnyan +9 more
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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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