English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We perform general relativistic, magnetohydrodynamic (GRMHD) simulations ofmerging binary neutron stars incorporating neutrino transport and magneticfields. Our new radiative transport module for neutrinos adopts a generalrelativistic, truncated-moment (M1) formalism. The binaries consist of twoidentical, irrotational stars modeled by the SLy nuclear equation of state(EOS). They are initially in quasicircular orbit and threaded with a poloidalmagnetic field that extends from the stellar interior into the exterior, as intypical pulsars. We insert neutrino processes shortly after the merger andfocus on the role of neutrinos in launching a jet following the collapse of thehypermassive neutron star (HMNS) remnant to a spinning black hole (BH). Wetreat two microphysical versions: one (a "warm-up") evolving a single neutrinospecies and considering only charged-current processes, and the other evolvingthree species $(\nu_e, \bar{\nu}_e, \nu_{\rm x})$ and related processes. Wetrace the evolution until the system reaches a quasiequilibrium state after BHformation. We find that the BH + disk remnant eventually launches an incipientjet. The electromagnetic Poynting luminosity is $\sim 10^{53} \rm \, erg\,s^{-1}$, consistent with that of typical short gamma-ray bursts (sGRBs). Theeffect of neutrino cooling shortens the lifetime of the HMNS, and lowers theamplitude of the major peak of the gravitational wave (GW) power spectrumsomewhat. After BH formation, neutrinos help clear out the matter near the BHpoles, resulting in lower baryon-loaded surrounding debris. The neutrinoluminosity resides in the range $\sim 10^{52-53} \rm \,erg\,s^{-1}$ oncequasiequilibrium is achieved. Comparing with the neutrino-free models, weobserve that the inclusion of neutrinos yields similar ejecta masses and isinefficient in carrying off additional angular momentum.

Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields