The Supernova Gamma-Ray Burst Connection

By Stan Woosley, Alexander Heger. 2006

977 citations recorded by the source corpus.

The chief distinction between ordinary supernovae and long-soft gamma-ray bursts (GRBs) is the degree of differential rotation in the inner several solar masses when a massive star dies, and GRBs are rare mainly because of the difficulty achieving the necessary high rotation rate. Models that do provide the necessary angular momentum are discussed, with emphasis on a new single star model whose rapid rotation leads to complete mixing on the main sequence and avoids red giant formation. This channel of progenitor evolution also gives a broader range of masses than previous models, and allows the copious production of bursts outside of binaries and at high redshifts. However, even the production of a bare helium core rotating nearly at break up is not, by itself, a sufficient condition to make a gamma-ray burst. Wolf-Rayet mass loss must be low, and will be low in regions of low metallicity. This suggests that bursts at high redshift (low metallicity) will, on the average, be more energetic, have more time structure, and last longer than bursts nearby. Every burst consists of three components: a polar jet (~0.1 radian), high energy, subrelativistic mass ejection (~1 radian), and low velocity equatorial mass that can fall back after the initial explosion. The relative proportions of these three components can give a diverse assortment of supernovae and high energy transients whose properties may vary with redshift.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3cb0dbd5eb00fedf5ab2af1734aafb94fe95707c

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In Astronomy and Astrophysics

1. Bing Zhang
2. E. Berger
3. B. Metzger
4. S. Smartt
5. Stan Woosley
6. N. Smith
7. Christian D. Ott
8. Hans-Thomas Janka

Citations in the corpus

• Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, background): “…of some of the synthesized elements could produce a supernova-like light curve in the optical; Woosley has suggested that the production of 56Ni in the disc wind could give rise to a bright supernova (MacFadyen & Woosley 1999; Pruet, Guiles & Fuller 2002; see Woosley & Bloom 2006, for a review).”
• Fluctuations in the high-redshift Lyman–Werner background: close halo pairs as the origin of supermassive black holes (2008, background): “Long-duration GRBs are thought to be associated with massive (M >∼10 − 30M⊙) young stars, and are therefore thought to occur within star forming regions of galaxies (see e.g. Woosley & Bloom 2006).”
• FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “The connection between long-duration gamma-ray bursts (GRBs) and broad-lined Type Ic supernovae (SNe Ic-bl) has recently piqued interest in certain SNe as GRB progenitors (see Woosley & Bloom 2006 for a review).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, neutral): “Secondly, for a GRB-SN to be observed there are several stringent requirements [11], including AGs that fade at a reliably determined rate (e.”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “…in pre-explosion data.3 The known stars that most naturally fit the bill for progenitors of SNe Ib and Ic are the Wolf–Rayet (WR) stars of the WN and WC subclasses, respectively, because of their relatively H-free surface composition and their small stellar radii (e.g. Woosley & Bloom 2006).”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “Most recently, the connection between long-duration GRBs and broad-lined SNe Ic (see Woosley & Bloom 2006; Hjorth & Bloom 2011; Modjaz 2011 for reviews) has sparked interest in the nature and progenitors of SNe Ic with and without GRBs. Broad-lined SNe Ic are a class of SNe Ic that exhibit very…”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “Indeed the statement that “the data and models are consistent with, though not conclusive proof of, the hypothesis that ALL long-soft GRBs are accompanied by SNe of Type Ic” was made right before the discovery of GRB 060614 and GRB 060505 (Woosley & Bloom 2006).”
• Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “These conditions are those needed to obtain a collapsar (Woosley 1993), and to the observational association of broad-lined Type Ic SNe with several nearby (z ≤ 0.5) LGRB events (Woosley & Bloom 2006; Berger et al. 2011, and references therein).”
• The spin of the second-born black hole in coalescing binary black holes (2018, background): “Massive He-rich stars are also widely accepted as the progenitors of Type Ib/c supernovae (e.g. Filippenko 1997; Woosley & Bloom 2006, and references therein).”
• The unusual X-ray emission of the short Swift GRB 090515: evidence for the formation of a magnetar? (2010, background): “Multiwavelength observations have associated LGRBs with type Ibc core collapse supernovae at cosmological distances (e.g. Hjorth et al. 2003; Stanek et al. 2003), although not all such supernovae produce long GRBs (Woosley & Bloom 2006).”
• Spectropolarimetry of Supernovae (2008, background): “…et al. 2006, 2007; Mezzacappa & Blondin 2007; Moiseenko & BisnovatyiKogan 2007; Komissarov & Barkov 2007; and references therein) and established a strong tie to cosmic long gamma-ray bursts that also involve the collapse of massive stars and highly directed energy output (Woosley & Bloom 2006).”
• THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016 GHz (2013, background): “…to massive stellar death, since at z 0.4 optical observations are capable of unambiguously recognizing an accompanying supernova (SN) signature and classifying it spectroscopically (see Woosley & Bloom 2006 for a review), whereas at high redshifts this task is very challenging or impossible.”
• A Comprehensive Analysis of Swift XRT Data. III. Jet Break Candidates in X-Ray and Optical Afterglow Light Curves (2007, background): “The progenitors of the two classes are distinctly different: type II GRBs are related to the deaths of massive stars (Woosley & Bloom 2006 and references therein), and type I GRBs are likely related to mergers of compact objects (Gehrels et al. 2005; Fox et al. 2005; Barthelmy et al. 2005; Berger…”
• Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “Another challenge to the conventional stellar evolution and supernova models is the establishment of the gamma-ray burst (GRB)-supernova connection (e.g., Woosley & Bloom 2006).”