Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric

By A. Arcones, Hans-Thomas Janka, L. Scheck. 2006

175 citations recorded by the source corpus.

We investigate the behavior and consequences of the reverse shock that terminates the supersonic expansion of the baryonic wind which is driven by neutrino heating off the surface of (non-magnetized) new-born neutron stars in supernova cores. To this end we perform long-time hydrodynamic simulations in spherical symmetry. In agreement with previous relativistic wind studies, we find that the neutrino-driven outflow accelerates to supersonic velocities and in case of a compact, ~1.4$\,M_\odot$ (gravitational mass) neutron star with a radius of about 10 km, the wind reaches entropies of about 100$\,k_{\mathrm B}$ per nucleon. The wind, however, is strongly influenced by the environment of the supernova core. It is decelerated and shock-heated abruptly by a termination shock that forms when the supersonic outflow collides with the slower preceding supernova ejecta. The radial position of this reverse shock varies with time and depends on the strength of the neutrino wind and the explosion conditions in progenitor stars with different masses and structure. Its basic properties and behavior can be understood by simple analytic considerations. We demonstrate that the entropy of the matter going through the reverse shock can increase to a multiple of the asymptotic wind value. Seconds after the onset of the explosion it therefore can exceed 400$\,k_{\mathrm B}$ per nucleon in low-mass progenitors around 10$\,M_\odot$, where the supernova shock and the reverse shock propagate outward quickly. The temperature of the shocked wind has typically dropped to about or less than 10 9 K, and density and temperature in the shock-decelerated matter continue to decrease only very slowly. For more massive progenitors with bigger and denser metal cores, the explosion expands more slowly so that the termination shock stays at smaller radii and affects the wind at higher temperatures and densities. In this case the termination shock might play a non-negligible, strongly time- and progenitor-dependent role in discussing supernova nucleosynthesis.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b7319cae2fbed60988a40562e15cf9cb46ed7794

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 Nuclear and High Energy Physics

Citations in the corpus

The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, background): “H E ] 1 7 Ja lenged in providing suitable conditions to produce heavy r-process elements (e.g. Arcones et al. 2007; Fischer et al. 2010; Hüdepohl et al. 2010; Roberts et al. 2010)1.”
MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, background): “…et al. 1997; Meyer & Brown 1997; Farouqi et al. 2010) (a) did not result in having sufficiently high entropies (Thompson et al. 2001; Wanajo 2006; Arcones et al. 2007), and (b) in addition, the innermost ejecta turned out to be proton-rich instead of neutron-rich (Pruet et al. 2006; Fröhlich et…”
CHARGED-PARTICLE AND NEUTRON-CAPTURE PROCESSES IN THE HIGH-ENTROPY WIND OF CORE-COLLAPSE SUPERNOVAE (2010, background): “A “cold” r-process, which proceeds at high temperatures and ends at even lower temperatures (T9 ≈ 0.35) with no chemical equilibrium until the A 195 peak is formed (see also Arcones et al. 2007; Wanajo 2007).”
Magnetized relativistic jets and long-duration GRBs from magnetar spin-down during core-collapse supernovae (2009, unknown): “5 of Arcones et al. 2007).”
SYSTEMATICS OF DYNAMICAL MASS EJECTION, NUCLEOSYNTHESIS, AND RADIOACTIVELY POWERED ELECTROMAGNETIC SIGNALS FROM NEUTRON-STAR MERGERS (2013, background): “…yet and core-collapse supernova simulations continue to be unable to yield the extreme conditions for forming the heaviest neutronrich nuclei (Arcones et al. 2007; Hoffman et al. 2008; Janka et al. 2008; Roberts et al. 2010; Hüdepohl et al. 2010; Fischer et al. 2010; Wanajo et al. 2011;…”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “However, after about 1.5 seconds post bounce the neutrino-driven wind appears as discussed in e.g. Arcones et al. (2007); Fischer et al. (2010b).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, background): “…number, page 3 of 26 luminosity adds to the neutrino fluxes imposed spherically symmetrically at the inner grid boundary so that the outgoing luminosities are considerably different from the values assumed at the inner grid boundary (see, e.g., Scheck et al. 2006; Arcones et al. 2007).”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “…of the reverse shock (e.g., Woosley et al. 1994; Wanajo et al. 2001; Farouqi et al. 2010) or after the fallback started (e.g., Fryer et al. 2006; Arcones et al. 2007); the polar jets from rotating magneto-hydrodynamical explosions of CCSN (Nishimura et al. 2006); the neutron-rich matter ejected…”
PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS (2012, methodology): “…is treated by the Consistent Multi-fluid Advection (CMA) scheme of Plewa & Müller (1999), and selfgravity of the stellar plasma includes corrections of the New- tonian gravitational potential for general relativistic effects as described in detail in Scheck et al. (2006) and Arcones et al. (2007).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “A contraction of the boundary radius is prescribed to mimic the shrinking neutron-star core (Scheck et al. 2006; Arcones et al. 2007), and neutrino luminosities of chosen magnitude and time dependence are imposed there to parametrize the neutrino losses from the interior core volume.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…progenitor mass coordinate (e.g. Woosley & Weaver 1995; Thielemann et al. 1996; Timmes et al. 1996) do not take into account the details of pushing the ejecta out on a timescale & 1 s by the neutrino-driven wind forming the double-shock structure (e.g. Arcones et al. 2007; Arcones & Janka 2011).”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “…favored production site, core-collapse supernovae, in contrast, seems to struggle to produce the conditions required for a successful r-process (Arcones et al. 2007; Hüdepohl et al. 2010; Roberts et al. 2010; Fischer et al. 2010; Arcones & Montes 2011; Arcones & Thielemann 2013), though some…”
Europium production: neutron star mergers versus core-collapse supernovae (2013, background): “Recently, hydrod - namical simulations with accurate neutrino transport haveshown that the neutrino winds are proton-rich (Arcones et al. 2007; Fischer et al. 2010; Hüdepohl et al. 2010) or slightly neutron-ich (Martı́nez-Pinedo et al. 2012; Roberts et al. 2012), but never very neutron-rich, as…”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “This hypothesis has attracted much attention recently, after attempts to robustly produce heavy r-process elements in core-collapse supernova simulations encountered significant difficulties (Arcones et al. 2007; Fischer et al. 2010; Roberts et al. 2010; Thielemann et al. 2011).”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, background): “Our results, obtained using general relativistic radiation hydrodynamics based on spectral three flavor Boltzmann neutrino transport, are in qualitative agreement with the detailed parametrized investigation by Arcones et al. (2007).”