2014MNRAS.443.3134P -
Mon. Not. R. Astron. Soc., 443, 3134-3156 (2014/October-1)
Neutrino-driven winds from neutron star merger remnants.
PEREGO A., ROSSWOG S., CABEZON R.M., KOROBKIN O., KAPPELI R., ARCONES A. and LIEBENDORFER M.
Abstract (from CDS):
We present a detailed, three-dimensional hydrodynamic study of the neutrino-driven winds emerging 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 neutrino absorption. Consistent with earlier two-dimensional studies, a strong baryonic wind is blown out along the original binary rotation axis within ~100 ms. From this model, we compute a lower limit on the expelled mass of 3.5x10–3 M☉, relevant for heavy element nucleosynthesis. Because of stronger neutrino irradiation, the polar regions show substantially larger electron fractions than those at lower latitudes. The polar ejecta produce interesting r-process contributions from A ~ 80 to about 130, while the more neutron-rich, lower latitude parts produce elements up to the third r-process peak near A ~ 195. We calculate the properties of electromagnetic transients powered by the radioactivity in the wind, in addition to the `macronova' transient stemming from the dynamic ejecta. The polar regions produce ultraviolet/optical transients reaching luminosities up to 1041erg/s, which peak around 1 d in optical and 0.3 d 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 d in optical and infrared.
Abstract Copyright:
© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)
Journal keyword(s):
accretion, accretion discs - dense matter - hydrodynamics - neutrinos - stars: neutron
Simbad objects:
1
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