TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS

Journal Article · Fri Dec 10 00:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/725/1/940· OSTI ID:21474394

Yoon, S -C; Woosley, S E ^[1]; Langer, N ^[2]

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1. UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States)
2. Argelander Institut fuer Astronomie, University of Bonn, Auf dem Huegel 71, D-53121, Bonn (Germany)

We investigate the evolution of Type Ib/c supernova (SN Ib/c) progenitors in close binary systems, using new evolutionary models that include the effects of rotation, with initial masses of 12-25 M{sub sun} for the primary components, and of single helium stars with initial masses of 2.8-20 M{sub sun}. We find that, despite the impact of tidal interaction on the rotation of primary stars, the amount of angular momentum retained in the core at the presupernova stage in different binary model sequences converges to a value similar to those found in previous single star models. This amount is large enough to produce millisecond pulsars, but too small to produce magnetars or long gamma-ray bursts. We employ the most up-to-date estimate for the Wolf-Rayet mass-loss rate, and its implications for SN Ib/c progenitors are discussed in detail. In terms of stellar structure, SN Ib/c progenitors in binary systems at solar metallicity are predicted to have a wide range of final masses up to about 7 M{sub sun}, with helium envelopes of M{sub He} {approx_equal} 0.16-1.5 M{sub sun}. Our results indicate that, if the lack of helium lines in the spectra of SNe Ic were due to small amounts of helium (e.g., M{sub He} {approx}< 0.5), the distribution of both initial and final masses of SN Ic progenitors should be bimodal. Furthermore, we find that a thin hydrogen layer (0.001 M{sub sun} {approx}< M{sub H} {approx}< 0.01 M{sub sun}) is expected to be present in many SN Ib progenitors at the presupernova stage. We show that the presence of hydrogen, together with a rather thick helium envelope, can lead to a significant expansion of some SN Ib/c progenitors by the time of supernova explosion. This may have important consequences for the shock break-out and supernova light curve. We also argue that some SN progenitors with thin hydrogen layers produced via Case AB/B transfer might be related to Type IIb supernova progenitors with relatively small radii of about 10 R{sub sun}.

• OSTI ID: 21474394
• Journal Information: Astrophysical Journal, Vol. 725, Issue 1; Other Information: DOI: 10.1088/0004-637X/725/1/940; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ANGULAR MOMENTUM
COSMIC GAMMA BURSTS
EXPLOSIONS
HELIUM
HYDROGEN
MASS
PULSARS
ROTATION
STAR EVOLUTION
STAR MODELS
SUPERNOVAE
BINARY STARS
COSMIC RADIATION
COSMIC RADIO SOURCES
ELEMENTS
ERUPTIVE VARIABLE STARS
EVOLUTION
FLUIDS
GASES
IONIZING RADIATIONS
MATHEMATICAL MODELS
MOTION
NONMETALS
PRIMARY COSMIC RADIATION
RADIATIONS
RARE GASES
STARS
VARIABLE STARS