Browsing by Subject "binaries: close"
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- ItemOpen AccessExploring inside-out Doppler tomography: non-magnetic cataclysmic variables(2015) Kotze, E J; Potter, S B; McBride, V AContext. Doppler tomography is a technique that has revolutionised the interpretation of the phase-resolved spectroscopic observations of interacting binary systems.
- ItemOpen AccessHigh-speed photometry of SDSS J013701.06 − 091234.9(2004) Pretorius, M L; Woudt, P A; Warner, B; Bolt, G; Patterson, J; Armstrong, EWe present high speed photometry of the Sloan Digital Sky Survey cataclysmic variable SDSS J013701.06-091234.9 in quiescence and during its 2003 December superoutburst. The orbital modulation at 79.71pm0.01 min is double humped; the superhump period is 81.702pm0.007 min. Towards the end of the outburst late superhumps with a period of 81.29pm0.01 min were observed. We argue that this is a system of very low mass transfer rate, and that it probably has a long outburst interval.
- ItemOpen AccessMulti-epoch VLTI-PIONIER imaging of the supergiant V766 Cen: Image of the close companion in front of the primary(2017) Wittkowski, M; Abellán, F J; Arroyo-Torres, B; Chiavassa, A; Guirado, J C; Marcaide, J M; Alberdi, A; de Wit, W J; Hofmann, K-H; Meilland, A; Millour, F; Mohamed, S; Sanchez-Bermudez, JContext. The star V766 Cen (=HR 5171A) was originally classified as a yellow hypergiant but lately found to more likely be a 27−36 M⊙ red supergiant (RSG). Recent observations indicated a close eclipsing companion in the contact or common-envelope phase.
- ItemOpen AccessThe yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase(2014) Chesneau, O; Meilland, A; Chapellier, E; Millour, F; van Genderen, A M; Nazé, Y; Smith, N; Spang, A; Smoker, J V; Dessart, L; Kanaan, S; Bendjoya, Ph; Feast, M W; Groh, J H; Lobel, A; Nardetto, N; Otero, S; Oudmaijer, R D; Tekola, A G; Whitelock, P A; Arcos, C; Curé, M; Vanzi, LContext. Only a few stars are caught in the very brief and often crucial stages when they quickly traverse the Hertzsprung-Russell diagram, and none has yet been spatially resolved in the mass transfer phase.