Results 1 - 10 of 77

FIRST VISUAL ORBIT FOR THE PROTOTYPICAL COLLIDING-WIND BINARY WR 140

by J. D. Monnier, Ming Zhao, E. Pedretti, R. Millan-gabet, J. -p. Berger, W. Traub, F. P. Schloerb, T. Ten Brummelaar, H. Mcalister, S. Ridgway, L. Sturmann, J. Sturmann, N. Turner, F. Baron, S. Kraus, A. Tannirkulam, P. M. Williams - THE ASTROPHYSICAL JOURNAL LETTERS, 742:L1 (6PP), 2011 , 2011
"... Wolf–Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively little is known about this short-lived phase and we currently lack reliable mass, distance, and binarity determinations for a representative sample. Here we report the first visual orbit for WR 140 ( = H ..."
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( = HD193793), a WC7 + O5 binary system known for its periodic dust production episodes triggered by intense colliding winds near periastron passage. The Infrared-Optical Telescope Array and Center for High Angular Resolution Astronomy interferometers resolved the pair of stars in each year from 2003

The Astrophysical Journal Letters, 742:L1 (6pp), 2011 November 20 doi:10.1088/2041-8205/742/1/L1 C © 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. FIRST VISUAL ORBIT FOR THE PROTOTYPICAL COLLIDING-WIND BINARY WR 140

by J. D. Monnier, Ming Zhao, E. Pedretti, R. Millan-gabet, J. -p. Berger, W. Traub, F. P. Schloerb, T. Ten Brummelaar, H. Mcalister, S. Ridgway, L. Sturmann, J. Sturmann, N. Turner, F. Baron, S. Kraus, A. Tannirkulam, P. M. Williams
"... Wolf–Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively little is known about this short-lived phase and we currently lack reliable mass, distance, and binarity determinations for a representative sample. Here we report the first visual orbit for WR 140 ( = H ..."
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( = HD193793), a WC7 + O5 binary system known for its periodic dust production episodes triggered by intense colliding winds near periastron passage. The Infrared-Optical Telescope Array and Center for High Angular Resolution Astronomy interferometers resolved the pair of stars in each year from 2003

colliding-wind binary WR140

by P. M. Williams, S. V. Marchenko, A. P. Marston, A. F. J. Moffat, W. P. Varricatt, S. M. Dougherty, M. R. Kidger, L. Morbidelli, M. Tapia
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The Prototype Colliding-Wind Pinwheel WR 104,” Astrophys

by Peter G. Tuthill, John D. Monnier, Nicholas Lawrance, William C. Danchi, Stan P. Owocki, Kenneth G. Gayley - Proc. of SPIE Vol. 7735 77351O-10 Downloaded from SPIE Digital Library on 13 Oct 2010 to 129.94.163.103. Terms of Use: http://spiedl.org/terms , 2008
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Radio emission models of colliding-wind binary systems

by S M Dougherty , J M Pittard , R Coker , P M Williams , L Kasian , H M Lloyd - Inclusion of IC cooling, A&A 446 , 2006
"... Instituto de Astronomía México Dougherty, S. M.; Pittard, J. M.; Coker, R.; Williams, P. M.; Kasian, L.; Lloyd, H. M. Radio emission models of Colliding-Wind Binaries Revista Mexicana de Astronomía y Astrofísica, vol. 15, septiembre, 2003, pp. 56-58 Instituto de Astronomía Distrito Federal, Méxi ..."
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Instituto de Astronomía México Dougherty, S. M.; Pittard, J. M.; Coker, R.; Williams, P. M.; Kasian, L.; Lloyd, H. M. Radio emission models of Colliding-Wind Binaries Revista Mexicana de Astronomía y Astrofísica, vol. 15, septiembre, 2003, pp. 56-58 Instituto de Astronomía Distrito Federal

The colliding-wind binary WR140: the particle acceleration laboratory

by S. M. Dougherty, J. M. Pittard , 2005
"... The 7.9-year period WR+O system WR 140 is the archetype CWB. It exhibits dramatic variations in its emission from near-IR to radio wavelengths (Williams et al. 1990; White & Becker 1995), and at X-ray energies (Pollock et al. 2005), ..."
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The 7.9-year period WR+O system WR 140 is the archetype CWB. It exhibits dramatic variations in its emission from near-IR to radio wavelengths (Williams et al. 1990; White & Becker 1995), and at X-ray energies (Pollock et al. 2005),

High resolution radio studies of WR colliding-wind systems

by Sean M. Dougherty
"... High resolution radio observations with MERLIN and the VLA spatially resolve the thermal and non-thermal emission in WR147 and WR146. In both of these systems, the WR stars have massive companions. The relative positions of the radio emission and the stellar components is consistent with the non-the ..."
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-thermal emission originating in the region where the two stellar winds in the system collide. In total eleven WR star systems are known to be non-thermal emitters, of which ten have massive companions, strongly supporting the hypothesis that nonthermal emission in WR stars requires a massive binary system. VLBI

Are WC9 Wolf-Rayet stars in colliding-wind binaries? ∗

by P. M. Williams, K. A. Van Der Hucht, G. Rauw , 2005
"... Abstract: We present results from a spectroscopic search for massive companions to dust-making Galactic WC9 stars as a step to testing the paradigm that dust formation in these systems requires colliding winds to produce over densities. We find evidence for OB companions to the WC9 stars WR 59 and W ..."
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, but the mechanism for this is still not understood. Studies have shown that dust formation by WR stars requires that their winds contain regions of significantly higher density. These can be provided by shocks in colliding stellar winds (Usov 1991) if the WR stars are members of massive binary systems

Astronomy Astrophysics Radio emission models of colliding-wind binary systems

by S. M. Dougherty, J. M. Pittard, L. Kasian, R. F. Coker, P. M. Williams, H. M. Lloyd , 2003
"... Abstract. We present calculations of the spatial and spectral distribution of the radio emission from a wide WR+OB collidingwind binary system based on high-resolution hydrodynamical simulations and solutions to the radiative transfer equation. We account for both thermal and synchrotron radio emiss ..."
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Abstract. We present calculations of the spatial and spectral distribution of the radio emission from a wide WR+OB collidingwind binary system based on high-resolution hydrodynamical simulations and solutions to the radiative transfer equation. We account for both thermal and synchrotron radio

Multi-frequency observations of the Wolf-Rayet star WR146: another colliding-wind binary?

by Dougherty Williams Van, S. M. Dougherty, P. M. Williams, K. A. Van Der Hucht, M. F. Bode, R. J. Davis
"... We present the first high spatial resolution radio observations of the Wolf-Rayet star WR146, obtained at 1.6 and 5 GHz with the MERLIN array. The 5-GHz observations resolve the source into two components separated by 116 \Sigma 14 milli-arcseconds (mas). The weaker (southern) source is identified a ..."
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(WR125 and WR140) known to be non-thermal emitters. We suggest that the non-thermal emission arises from the interaction of the WR wind and that of its newly detected luminous companion. The observed size of the non-thermal radio emitting region is consistent with that expected from colliding wind
Results 1 - 10 of 77