FLARE-LESS LONG GAMMA-RAY BURSTS AND THE PROPERTIES OF THEIR MASSIVE PROGENITOR STARS

AbstractWe discuss the role of mass loss for the evolution of the most massive stars, highlighting the role of the predicted bi-stability jump that might be relevant for the evolution of rotational velocities during or just after the main sequence. This mechanism is also proposed as an explanation for the mass-loss variations seen in the winds from Luminous Blue Variables (LBVs). These might be relevant for the quasi-sinusoidal modulations seen in a number of recent transitional supernovae (SNe), as well as for the double-throughed absorption profile recently discovered in the Hα line of SN 2005gj. Finally, we discuss the role of metallicity via the Z-dependent character of their winds, during both the initial and final (Wolf-Rayet) phases of evolution, with implications for the angular momentum evolution of the progenitor stars of long gamma-ray bursts (GRBs).

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Evolution of Progenitor Stars of Type Ibc Supernovae and Long Gamma-Ray Bursts

Proceedings of the International Astronomical Union ◽

10.1017/s174392130802053x ◽

2007 ◽

Vol 3 (S250) ◽

pp. 231-236

Author(s):

Sung-Chul Yoon ◽

Norbert Langer ◽

Matteo Cantiello ◽

Stan E. Woosley ◽

Gary A. Glatzmaier

Keyword(s):

Binary Stars ◽

Binary Systems ◽

Massive Star ◽

Gamma Ray ◽

Gamma Ray Bursts ◽

Evolutionary Models ◽

Single Star ◽

Solar Metallicity ◽

Progenitor Stars

AbstractWe discuss how rotation and binary interactions may be related to the diversity of type Ibc supernovae and long gamma-ray bursts. After presenting recent evolutionary models of massive single and binary stars including rotation, the Tayler-Spruit dynamo and binary interactions, we argue that the nature of SNe Ibc progenitors from binary systems may not significantly differ from that of single star progenitors in terms of rotation, and that most long GRB progenitors may be produced via the quasi-chemically homogeneous evolution at sub-solar metallicity. We also briefly discuss the possible role of magnetic fields generated in the convective core of a massive star for the transport of angular momentum, which is potentially important for future stellar evolution models of supernova and GRB progenitors.

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The Progenitor Stars of Gamma‐Ray Bursts

The Astrophysical Journal ◽

10.1086/498500 ◽

2006 ◽

Vol 637 (2) ◽

pp. 914-921 ◽

Cited By ~ 592

Author(s):

S. E. Woosley ◽

A. Heger

Keyword(s):

Gamma Ray ◽

Gamma Ray Bursts ◽

Progenitor Stars

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SN 1998bw and Other Hyperenergetic Type Ic Supernovae

International Astronomical Union Colloquium ◽

10.1017/s0252921100009465 ◽

2005 ◽

Vol 192 ◽

pp. 391-401

Author(s):

Paolo A. Mazzali ◽

Ken’ichi Nomoto ◽

Jinsong Deng ◽

Keiichi Maeda ◽

Koichi Iwamoto ◽

...

Keyword(s):

Kinetic Energy ◽

Gamma Ray ◽

Gamma Ray Bursts ◽

Light Curves ◽

Progenitor Stars

SummaryThe properties of the best-observed peculiar, SN 1998bw-like Type Ic supernovae (sometimes called “hypernovae” ) are reviewed, starting from SN 1998bw itself and including SNe 1997ef and 2002ap. Analysis of the light curves and the spectra shows that, while these SNe display a range of properties (kinetic energy, mass of the ejecta, mass of 56Ni synthesized in the explosion), they have in common a larger-than-normal explosion kinetic energy, giving rise to the characteristic broad-lined spectra. Also, they all come from the collapse of bare CO cores of massive ( ≳ 20M⊙) progenitor stars. Some of the properties of these SNe, such as kinetic energy and mass of 56Ni, are probably correlated with the mass of the progenitor. Evidence that these powerful events are intrinsically asymmetric, suggesting that a correlation with at least some gamma-ray bursts can be expected, is also discussed.

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Spatially-resolved imaging of stripped-envelope supernova environments

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316005305 ◽

2015 ◽

Vol 11 (A29B) ◽

pp. 270-271

Author(s):

Schuyler D. Van Dyk

Keyword(s):

Mass Transfer ◽

Stellar Wind ◽

Gamma Ray ◽

High Spatial Resolution ◽

Hubble Space Telescope ◽

Gamma Ray Bursts ◽

Spatially Resolved ◽

Long Duration ◽

Progenitor Stars ◽

Insight Into

AbstractStripped-envelope supernovae (SNe), i.e., those of Type Ib, Ic, and IIb, arise from massive progenitor stars which have had most or all of their outer hydrogen-rich layers removed before explosion by some process, either through a strong stellar wind or through binary mass transfer. The connection between some long-duration gamma-ray bursts (GRBs) and broad-lined Type Ic SNe makes a broader discussion of stripped-envelope SNe and their environments particularly relevant. If the SN progenitor itself cannot be directly identified, it is possible that examination of its immediate environment can provide some insight into the nature of the progenitor. It is also possible that revisiting the SN site sufficiently late enough after explosion could reveal the presence of a binary companion. I will present high-spatial-resolution observations obtained with the Hubble Space Telescope of the sites and environments of stripped-envelope supernovae, and I will discuss the implications of the resulting analysis. I will include here, e.g., the environments of the recent SN 2011dh, SN 2012au, SN 2013df, SN 2013dk, and iPTF13bvn.

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Probing the circumstellar medium of GRB afterglows through absorption-line observations

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2006.1972 ◽

2007 ◽

Vol 365 (1854) ◽

pp. 1247-1253 ◽

Cited By ~ 1

Author(s):

Hsiao-Wen Chen

Keyword(s):

Absorption Line ◽

Radiation Field ◽

High Velocity ◽

Column Density ◽

Gamma Ray ◽

Neutral Hydrogen ◽

Gamma Ray Bursts ◽

Host Galaxies ◽

Hydrogen Column Density ◽

Progenitor Stars

A systematic search of Wolf–Rayet wind signatures, as represented by blue-shifted, high-velocity (|Δ v |=1000–5000 km s −1 ) C IV λλ 1548, 1550 absorption doublet has yielded an estimate of 20% for the incidence of these C IV absorbers near the host galaxies of gamma-ray bursts (GRBs). This is consistent with what is observed near classical damped Ly α absorbers that have a comparable neutral hydrogen column density as the GRB host galaxies. A detailed ionization analysis of these absorbers, including the associated low-ionization species, shows that the majority in fact originate in foreground galaxies along the sightline, rather than in the vicinity of the GRB afterglows. Taking into account the enhanced afterglow radiation field, the lack of Wolf–Rayet signatures can be applied to constrain the C/He ratio and the density contrast of the winds in the vicinity of GRB progenitor stars.

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