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2 results

DIVISION VIII / WORKING GROUP SUPERNOVA
Wolfgang Hillebrandt, Brian P. Schmidt, Edward Baron, Stefano Benetti, Sergey I. Blinnikov, Sergey I. Blinnikov, David R. Branch, Enrico Cappellaro, Alexei V. Filippenko, Claes Fransson, Peter M. Garnavich, Daniel W. E. Green, Ariel M. Goobar, Mario Hamuy, Peter H. Hauschildt, Robert P. Kirshner, Bruno Leibundgut, Daniel J. Lennon, Eric J. Lentz, Peter Lundqvist, Robert McGraw, Paolo A. Mazzali, W. Peter S. Meikle, Anthony Mezzacappa, Jens C. Niemeyer, Ken'ichi Nomoto, Reynald Pain, Nino Panagia, Ferdinando Patat, Mark M. Phillips, Elena Pian, Guiliano Pignata, Philipp Podsiadlowski, María Pilar Ruiz-Lapuente, Elaine M. Sadler, Brian P. Schmidt, Peter O. Shull, Jason Spyromilio, Nicholas B. Suntzeff, Friedrich-Karl Thielemann, Christopher Tout, Virginia L. Trimble, James W. Truran, Dmitry Yu. Tsvetkov, Massimo Turatto, Massimo della Valle, Schuyler Van Dyk, Wolfgang H. Voges, Nicholas A. Walton, Lifan Wang, J. Craig Wheeler, Kurt W. Weiler, Patricia A. Whitelock, Stanford E. Woosley, Hitoshi Yamaoka, Gang Zhao
Journal: Proceedings of the International Astronomical Union / Volume 4 / Issue T27A / December 2008
Published online by Cambridge University Press: 01 December 2008, pp. 295-297
Print publication: December 2008
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The Supernova Working Group was re-established at the IAU XXV General Assembly in Sydney, 21 July 2003, sponsored by Commissions 28 (Galaxies) and 47 (Cosmology). Here we report on some of its activities since 2005.

Supernovae from Wolf-Rayet Stars
Norbert Langer, Stanford E. Woosley
Journal: Symposium - International Astronomical Union / Volume 143 / 1991
Published online by Cambridge University Press: 03 August 2017, p. 566
Print publication: 1991
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The complete evolution of a star with an initial mass of 60 M⊙ and Z = Z⊙ (i.e. a typical W R progenitor) from the ZAMS through the supernova phase has been investigated. Mass loss in the different evolutionary stages, especially mass dependent W R mass loss, leads to a WO star (surface mass fractions {He,C,O} = {0.14, 0.38, 0.48}; cf. Fig. 1) of 4 . 2 M⊙ as pre-SN configuration. The low final mass may be typical for a wide range of initial masses (cf. Langer, 1989, Astr. Ap. 220, 135).