Stellar evolution with rotation - XIII. Predicted GRB rates at various Z

By R. Hirschi, G. Meynet, A. M. U. O. Basel, G. Observatory, Switzerland.. 2005

145 citations recorded by the source corpus.

We present the evolution of rotation in models of massive single stars covering a wide range of masses and metallicities. These models reproduce observations during the early stages of the evolution very well, in particular Wolf-Rayet (WR) populations and ratio between type II and type Ib,c supernovae at different metallicities. Our models predict the production of fast-rotating black holes. Models with large initial masses or high metallicity end their lives with less angular momentum in their central remnant with respect to the break-up limit for the remnant. Many WR star models satisfy the three main criteria (black hole formation, loss of hydrogen-rich envelope, and enough angular momentum to form an accretion disk around the black hole) for gamma-ray bursts (GRB) production via Woosley's collapsar model. If we consider all types of WR stars as GRB progenitors, there would be too many GRBs compared to observations but if we consider only WO stars (type Ic supernovae as is the case for SN2003dh/GRB030329) as GRB progenitors, the GRB production rates are in much better agreement with observations. WO stars are produced only at low metallicities in the present series of models. This prediction can be tested by future observations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7df8749f4081c56e7b5ebc59e459f96dd778eb33

How researchers see this paper

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In Astronomy and Astrophysics

1. Stan Woosley
2. S. Smartt
3. Ilya Mandel
4. N. Langer
5. N. Smith
6. G. Meynet
7. Michela Mapelli
8. R. Hirschi

Citations in the corpus

• Very low-metallicity massive stars: - Pre-SN evolution models and primary nitrogen production (2006, methodology): “This figure shows that the core has enough angular momentum to produce a GRB (see Yoon & Langer 2005; Woosley & Heger 2006; Hirschi et al. 2005a, for more details on GRB progenitors).”
• Binary star progenitors of long gamma-ray bursts (2007, background): “While single star evolution models without internal magnetic fields can produce such configurations (Petrovic et al. 2005b; Hirschi et al. 2005), only models including magnetic fields are capable of reproducing the slow spins of young Galactic neutron stars (Heger et al. 2005; Ott et al. 2006) and…”
• Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals (2007, background): “For themostmassive stars, GRB progenitors in the collapsarmodel (e.g., MacFadyen & Woosley 1999; Yoon & Langer 2005), the interplay between metallicity-dependent mass loss through winds and rotation may be crucial (e.g., Hirschi et al. 2005).”
• Evolution and fate of very massive stars (2013, background): “…is predicted to explode as a PCSN, we thus do not expect the models presented in this grid to produce GRBs or magnetars but such energetic asymmetric explosions are likely to take place in lower mass and lower metallicity stars (see Hirschi et al. 2005; Yoon & Langer 2005; Woosley & Heger 2006).”
• The Progenitor Stars of Gamma-Ray Bursts (2005, background): “…time that if the magnetic torques are negligible, which is to say much weaker than estimated by Spruit (2002), it is easy to give GRB progenitors the necessary angular momentum (Heger et al. 2000; Hirschi et al. 2004, 2005), but then one must invoke another mechanism to slow down typical pulsars.”
• GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “These data supported a strong dependence of GRB formation with metallicity (e.g., Hirschi et al. 2005; Yoon et al. 2006) as would be theoretically expected in the collapsar model (Woosley 1993; MacFadyen & Woosley 1999).”
• A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION (2013, background): “Given the large variation in average metallicity between different galaxies, these effects could produce large deviations between the SFR and GRB rate in different galaxies (Hirschi et al. 2005).”
• Most Black Holes Are Born Very Slowly Rotating (2019, background): “Previous works on massive stars (e.g., Hirschi et al. 2005; Heger et al. 2005; Woosley & Heger 2006) are based on physics that over-predict core rotation rates for low-mass stars, hence their predictions of compact object rotation rates are unreliable.”
• Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, methodology): “This underlines, as already emphasised in previous works (seee.g. Hirschi et al. 2004, 2005; Woosley & Heger 2006), how important it is to properly account for angular momentum transfer during the MS phase.”
• ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “In general, the cores of massive stars are expected to rotate rapidly and thus may lead to rapid BH spin at formation, unless there is efficient angular momentum coupling between the core and the (expanding) envelope (e.g., Hirschi et al. 2005).”
• CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, background): “The lower opacity and mass loss rates of low-metallicity stars eases this requirement and provides a credible rationale for preferring lowmetallicity GRB hosts (Hirschi et al. 2005; Yoon & Langer 2005; Woosley & Heger 2006).”