Supernova hosts for gamma-ray burst jets: dynamical constraints

By C. Matzner. 2002

176 citations recorded by the source corpus.

I constrain a possible supernova origin for gamma-ray bursts (GRBs) by modelling the dynamical interaction between a relativistic jet and a stellar envelope surrounding it. The delay in observer time introduced by the jet traversing the envelope should not be long compared with the duration of gamma-ray emission; also, the jet should not be swallowed by the spherical explosion it powers. The only stellar progenitors that comfortably satisfy these constraints, if one assumes that jets move ballistically within their host stars, are compact carbon–oxygen or helium post-Wolf–Rayet stars (type Ic or Ib supernovae); type II supernovae are ruled out. Notably, very massive stars do not appear to be capable of producing the observed bursts at any redshift unless the stellar envelope is stripped prior to collapse. The presence of a dense stellar wind places an upper limit on the Lorentz factor of the jet in the internal shock model; however, this constraint may be evaded if the wind is swept forward by a photon precursor. Shock breakout and cocoon blowout are considered individually; neither presents a likely source of precursors for cosmological GRBs. These envelope constraints could conceivably be circumvented if jets are laterally pressure-confined while traversing the outer stellar envelope. If so, jets responsible for observed GRBs must have been launched from a region several hundred kilometres wide, have been crossed by strong shocks, or have mixed with envelope material as they travel. A phase of pressure confinement and mixing would imprint correlations among jets that may explain observed GRB variability–luminosity and lag–luminosity correlations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/48b5210ead71acb2878e98c9a7b0e7c6bad461d0

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In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Quataert
4. E. Nakar
5. Pawan Kumar
6. E. Berger
7. T. Piran
8. T. Thompson

Citations in the corpus

• THE PROPAGATION OF RELATIVISTIC JETS IN EXTERNAL MEDIA (2011, methodology): “(2) can be linearized (Matzner 2003): When L̃ ≪ 1 βh ≃ L̃1/2, (4a) corresponding to a non-relativistic head velocity.”
• SUPERNOVA LIGHT CURVES POWERED BY FALLBACK ACCRETION (2012, unknown): “The propagation of the outflow through the remaining bound fallback is similar to the propagation of a jet through a host star during a long GRB (e.g., Begelman & Cioffi 1989; Matzner 2003).”
• RELATIVISTIC SHOCK BREAKOUTS—A VARIETY OF GAMMA-RAY FLARES: FROM LOW-LUMINOSITY GAMMA-RAY BURSTS TO TYPE Ia SUPERNOVAE (2011, background): “…their propagation the jets drive mildly relativistic bow shocks into the envelope and inflate a cocoon that collimates the jets to an even narrower angle than their initial launching opening angle (e.g., MacFadyen & Woosley 1999; Matzner 2003; Morsony, Lazzati & Begelman 2007; Mizuta & Aloy 2009).”
• The cocoon emission - an electromagnetic counterpart to gravitational waves from neutron star mergers (2017, background): “As the jet interacts with the ejecta it forms a double shock structure at its head (Matzner 2003; Bromberg et al. 2011).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “When the cocoon erupts at the stellar surface it makes a wider, weaker, and less relativistic jet surrounding the central narrow, stronger, and highly relativistic jet (Ramirez-Ruiz et al., 2002; Matzner, 2003; Zhang et al., 2003b, 2004b).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “This is because in such stars, a stellar envelope will remain to impede the advance of the jet (MacFadyen and Woosley 1999, MacFadyen et al. 2001, Mészáros and Rees 2001, Aloy et al. 2000, Ramirez-Ruiz et al. 2002a, Matzner 2003, Zhang et al. 2004, Proga et al. 2003).”
• Temporal and Angular Properties of Gamma-Ray Burst Jets Emerging from Massive Stars (2006, methodology): “MORSONY, LAZZATI, & BEGELMAN584 Vol. 665 To compute the cocoon pressure we develop the approximations of Begelman & Cioffi (1989) and the jet propagation description of Matzner (2003).”
• Off-axis emission of short γ-ray bursts and the detectability of electromagnetic counterparts of gravitational-wave-detected binary mergers (2016, background): “They first define the quantity (see also Matzner 2003): L̃ = L2 jρac3 , (4) the ratio between the energy density of the jet and the energy density of the surrounding medium, where L2 is the luminosity of the two jets and j = R2a 2 is the cross-sectional area of the jet at breakout.”
• Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “(A1), we get (up to integration constants, which can be calculated posteriorly): pc ≈ √ ρ̄ac2Lj(βj − βh) 3πβht2 , (A2) Following Matzner (2003); Bromberg et al. (2011) we define a dimensionless parameter L̃ ≡ Lj πR2j ρac 3 = ( βj − βh βh )2 , (A3) where Rj is the cylindrical radius of the jet.”
• The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “…by accretion, or via the accretion-mediated extraction of the black hole’s spin (Blandford & Znajek 1977), then powers a relativistic jet, which burrows through the star and ultimately powers the GRB at larger radii (MacFadyen & Woosley 1999; Proga et al. 2003; Matzner 2003; Morsony et al. 2007).”
• Hyper-Eddington accretion flows on to massive black holes (2015, background): “The outflows and jets possibly penetrate through the inflow in a narrow conical region as in gamma-ray bursts (e.g. Matzner 2003; Bromberg et al. 2011; Suwa & Ioka 2011; Matsumoto et al. 2015) and carry away a large fraction of the gas and radiation energy.”
• Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation (2011, result): “The true threshold for a choked jet in the LGRB case thus occurs at lower luminosities ∼ > 1049 erg s−1, more consistent with previous estimates in the literature (Matzner 2003).”
• THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, background): “…Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel As the GRB jet carves its way through the stellar envelope it dissipates its energy in a double shock (forwardreverse) structure that forms at its head (Matzner 2003; Lazzati & Begelman 2005; Bromberg et al. 2011b).”