Neutrino-driven winds from neutron star merger remnants

By Albino Perego, Stephan Rosswog, Rubén M. Cabezon, Oleg Korobkin, R. Kaeppeli, A. Arcones, M. Liebendoerfer. 2014

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We present a detailed, three-dimensional hydrodynamic study of the neutrino-driven winds that emerge from the remnant of a neutron star merger. Our simulations are performed with the Newtonian, Eulerian code FISH, augmented by a detailed, spectral neutrino leakage scheme that accounts for heating due to neutrino absorption in optically thin conditions. Consistent with the earlier, two-dimensional study of Dessart et al. (2009), we nd that a strong baryonic wind is blown out along the original binary rotation axis within 100 milliseconds after the merger. We compute a lower limit on the expelled mass of 3:5 10 3 M , large enough to be relevant for heavy element nucleosynthesis. The physical properties vary signicantly between dierent wind regions. For example, due to stronger neutrino irradiation, the polar regions show substantially larger electron fractions than those at lower latitudes. This has its bearings on the nucleosynthesis: the polar ejecta produce interesting r-process contributions from A 80 to about 130, while the more neutron-rich, lower-latitude parts produce in addition also elements up to the third r-process peak near A 195. We also calculate the properties of electromagnetic transients that are powered by the radioactivity in the wind, in addition to the \macronova" transient that stems from the dynamic ejecta. The high-latitude (polar) regions produce UV/optical transients reaching luminosities up to 10 41 erg s 1 , which peak around 1 day in optical and 0.3 days in bolometric luminosity. The lower-latitude regions, due to their contamination with high-opacity heavy elements, produce dimmer and more red signals, peaking after 2 days in optical and infrared. Our numerical experiments indicate that it will be dicult to infer the collapse time-scale of the hypermassive neutron star to a black hole based on the wind electromagnetic transient, at least for collapse time-scales larger than the wind production time-scale.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a192e72d4543f434b934db26e05ba27f4b1a2a11

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Citations in the corpus

Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, background): “Neutrino heating is much more important if the merger produces a long-lived HMNS (Dessart et al. 2009; Metzger & Fernández 2014; Perego et al. 2014; Martin et al. 2015), resulting in a larger ejecta mass with higher electron fraction, depending on the uncertain lifetime of such a remnant.”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta (2017, background): “While winds from the accretion disk around the post-merger remnant can eject the requisite amount of mass (e.g. Fernández & Metzger 2013; Metzger & Fernández 2014; Perego et al. 2014; Siegel & Metzger 2017), the predicted wind velocities are too low (< 0.1c).”
Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “…of light) during the merger and post-merger phases(e.g., Dessart et al. 2009; Bauswein et al. 2013; Fernández & Metzger 2013; Hotokezaka et al. 2013b; Rosswog 2013; Metzger & Fernández 2014; Perego et al. 2014; Foucart et al. 2015, 2016; Just et al. 2015; Sekiguchi et al. 2015; Radice et al. 2016).”
Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations (2018, background): “Alternatively, as with the red ejecta, the blue ejecta could originate from an accretion disc outflow (e.g. Metzger & Fernandez 2014; Perego et al. 2014); however, the high velocity is incompatible with both hydrodynamical and MHD simulations (e.g. Fan, Messenger & Heng 2014; Siegel & Metzger 2017).”
Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, methodology): “This has been used as an argument for a non-zero lifetime of the HMNS in GW170817, which would irradiate the ejecta with neutrinos and increase the electron fraction (Metzger & Fernández 2014; Perego et al. 2014; Fujibayashi et al. 2018), resulting in a larger ejecta mass with Ye > 0.25.”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “In these cases, neutrino driven winds and viscous and magnetic processes in the disk are expected to unbind sufficient material to explain the optical and infrared observations for AT2017gfo (Perego et al. 2014; Wu et al. 2016; Siegel & Metzger 2017).”
The cocoon emission - an electromagnetic counterpart to gravitational waves from neutron star mergers (2017, background): “The latter is particularly relevant in neutrino driven winds that may dominate at high latitudes (Perego et al. 2014a).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, methodology): “Beside the dynamical ejecta, winds from the accretion disk of central BH driven by strong neutrino flux are expected to fill this underproduction of lighter r-process elements (Wanajo & Janka 2012; Perego et al. 2014; Rosswog et al. 2014; Just et al. 2014).”
AT 2017gfo: An Anisotropic and Three-component Kilonova Counterpart of GW170817 (2017, background): “If the merger does not lead to the prompt collapse of the central massive neutron star (MNS), neutrino-matter interactions and magnetic processes produce wind outflows (Perego et al. 2014).”
The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, background): “-process material in these objects. One arises from the disintegration of the disk at late times [144] and the other comes from wind like out ows from the disk [151, 152] or hypermassive neutron star [36]. Particularly the latter environment would be more similar to that of a neutrino driven wind in”
Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “We therefore do not investigate here the potentially relevant outflow component which may arise during the lifetime of such a massive NS (Dessart et al. 2009; Metzger & Fernández 2014; Perego et al. 2014).”
r-PROCESS LANTHANIDE PRODUCTION AND HEATING RATES IN KILONOVAE (2015, background): “…tidally (Lattimer et al. 1977; Freiburghaus et al. 1999), dynamically from the region where the two neutron stars collide (Bauswein et al. 2013; Hotokezaka et al. 2013a), or from the accretion disk that forms after the merger (Fernández & Metzger 2013; Perego et al. 2014; Just et al. 2015).”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, methodology): “…viscous and magnetic stresses, and energy which is released in the post-merger accretion disk due to nuclear recombination (Dessart et al. 2009; Perego et al. 2014; Martin et al. 2015; Chen & Beloborodov 2007; Siegel et al. 2014; Ciolfi & Siegel 2015; Metzger et al. 2008; Fernández & Metzger…”