论文标题
从中子二进制合并弹射器中的3D磁化喷射突破：射流和弹射器的余辉发射
3D magnetised jet break-out from neutron-star binary merger ejecta: afterglow emission from the jet and the ejecta
论文作者
论文摘要
我们执行三维（3D）一般性磁流失动力模拟，以对预期在二进制中子星级合并中产生的喷射射流进行模拟。来自3D模拟的相对主义流出的结构证实了我们先前从2D模拟中获得的结果，即，从合并弹出器中爆发的相对论磁化流出表现出$θ_{\ rm core} \ rm core} \ yout4^{\ of4^{\ oft4^{\ circ} $的空心核心。 JET} \ gtrsim10^{\ Circ} $，并伴随着弹出物质的风，将有助于Kilonova排放。我们还计算了相对论流出的非热余血发射，并将其贴合GRB170817A的全天余星，以及从VLBI观察结果报告的超光运动。这样，我们推断出$θ_ {\ rm obs} = 35.7^{\ circ的观察者角度 \，\，+1.8} _ {\ phantom {\ circ \，\，} -2.2} $。我们进一步计算出弹出物质的余辉发射，并在某种情况下约束参数空间，在这种情况下，负责热基洛诺瓦发射的物质也将导致尚未观察到非热发射。
We perform three-dimensional (3D) general-relativistic magnetohydrodynamic simulations to model the jet break-out from the ejecta expected to be produced in a binary neutron-star merger. The structure of the relativistic outflow from the 3D simulation confirms our previous results from 2D simulations, namely, that a relativistic magnetized outflow breaking out from the merger ejecta exhibits a hollow core of $θ_{\rm core}\approx4^{\circ}$, an opening angle of $θ_{\rm jet}\gtrsim10^{\circ}$, and is accompanied by a wind of ejected matter that will contribute to the kilonova emission. We also compute the non-thermal afterglow emission of the relativistic outflow and fit it to the panchromatic afterglow from GRB170817A, together with the superluminal motion reported from VLBI observations. In this way, we deduce an observer angle of $θ_{\rm obs}= 35.7^{\circ \,\,+1.8}_{\phantom{\circ \,\,}-2.2}$. We further compute the afterglow emission from the ejected matter and constrain the parameter space for a scenario in which the matter responsible for the thermal kilonova emission will also lead to a non-thermal emission yet to be observed.
