Nucleosynthesis in the Outflow from Gamma-Ray Burst Accretion Disks

By Ruth Surman, Gail McLaughlin, W. Hix. 2005

151 citations recorded by the source corpus.

We examine the nucleosynthesis products that are produced in the outflow from rapidly accreting disks. We find that the type of element synthesis varies dramatically with the degree of neutrino trapping in the disk and therefore the accretion rate of the disk. Disks with relatively high accretion rates such as Ṁ = 10 M☉ s-1 can produce very neutron-rich nuclei that are found in the r-process. Disks with more moderate accretion rates can produce copious amounts of nickel, as well as the light elements such as lithium and boron. Disks with lower accretion rates such as Ṁ = 1 M☉ s-1 produce large amounts of nickel, as well as some unusual nuclei such as 49Ti, 45Sc, 64Zn, and 92Mo. This wide array of potential nucleosynthesis products is due to the varying influence of electron neutrinos and antineutrinos emitted from the disk on the neutron-to-proton ratio in the outflow. We use a parameterization for the outflow and discuss our results in terms of entropy and outflow acceleration.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b7e373efd1c28935b8d68ad2c209db0835114096

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atmospheric Science

In Instrumentation

Citations in the corpus

Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “Disk winds are one example, yet the actual amount of material and angular momentum that is removed by such winds can vary significantly (Vlahakis & Königl 2001; Surman et al. 2006; Janiuk 2017).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, methodology): “A series of long- 1 The “disk wind” of collapsar models has been also investigated (e.g., Surman et al. 2006, 2008; Perego et al. 2014; Surman et al. 2014) as sites of heavy element nucleosynthesis term explosion simulations, based on the special relativistic MHD (Takiwaki et al. 2009; Takiwaki &…”
r-Process Nucleosynthesis in Hot Accretion Disk Flows from Black Hole-Neutron Star Mergers (2008, methodology): “We calculate the element synthesis using a nuclear statistical equilibrium code, a charged particle reaction code, and finally an r-process network code as described in Surman et al. (2006).”
OPACITIES AND SPECTRA OF THE r-PROCESS EJECTA FROM NEUTRON STAR MERGERS (2013, background): “2) Following the merger, material which has accumulated in a centrifugally supported disk may be blown off in a neutrino or nuclear driven wind (Levinson 2006; Surman et al. 2006; Metzger et al. 2008, 2009).”
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, background): “Also, as previously noted, we ignore nucleosynthesis in the neutrino-powered wind (Pruet et al. 2005), gamma-ray burst accretion disks (Surman et al. 2006) here, and any other r-process site.”
Time-dependent models of accretion discs formed from compact object mergers (2008, background): “Nonrelativistic outflows are sufficiently dense to synthesize heavy isotopes (Pruet et al. 2004; Surman et al. 2006), which may power transient emission via radioactive decay.”
EFFECT OF A HIGH OPACITY ON THE LIGHT CURVES OF RADIOACTIVELY POWERED TRANSIENTS FROM COMPACT OBJECT MERGERS (2013, background): “Though the physical properties of the disk winds remain uncertain, neutrino irradiation may drive the electron fraction to Ye & 0.4, in which case the nucleosynthesis may not extend past Z ∼ 50 (Surman et al. 2006, 2008; Metzger et al. 2008; Darbha et al. 2010).”
The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, background): “Other potential astrophysical sites that have been explored include hot accretion disk outflows from neutron star or neutron star-black hole mergers [35, 36, 30, 31], supernova neutronrich jets [37], gamma-ray burst collapsar outflows [38, 39, 40], shocked surface layers of O-Ne-Mg cores [41, 42], a”
Origin of the Chemical Elements (2010, background): “Among the Origin of the Chemical Elements suggested alternative scenarios are wind outflows from the accretion disks around black holes formed by core collapse of very massive stars (Surman et al. 2006).”