脉冲星驱动超新星中新生风泡的爆破
Blowouts of Nascent Wind Bubbles in Pulsar-Driven Supernovae
AI总结：
研究脉冲星驱动超新星中新生风泡爆破的条件及影响，提出半解析框架并计算多波段光变曲线，揭示不同磁场强度下超新星发光特征和X射线前兆。
摘要：
快速旋转、强磁场的中子星（NS）可能在多种核心坍缩事件中形成。如果NS在超新星爆发物变得透明之前注入的能量与超新星爆发能量相当，那么新生NS风泡可以追上外层爆发物并因流体不稳定性驱动爆破。基于多维数值研究，我们构建了一个最小半解析框架，以跟踪爆破后的动力学和辐射演化，通过扫描爆发物和NS参数来映射爆破条件，并计算适用于调查的多波段光变曲线。对于剥离包层超新星，其爆发物质量为$M_\mathrm{ej} \sim 10\,M_\odot$，爆炸能量为$E_\mathrm{sn} \sim 10^{51}\,\mathrm{erg}$，当NS的磁场强度$B_{\mathrm{dip}} \gtrsim 10^{13}\,\mathrm{G}$且自转周期$P_\mathrm{NS} \lesssim \mathrm{a\ few}\,\mathrm{ms}$时，会发生爆破。相对弱磁场情况下的$B_\mathrm{dip} \lesssim 10^{14}\,\mathrm{G}$会产生明亮的双峰紫外/光学光变曲线，如超亮超新星LSQ14bdq所观测到的。更强磁场情况下的$B_\mathrm{dip} \gtrsim 10^{14}\,\mathrm{G}$则导致超新星前有X射线爆破前兆。我们还研究了较弱和低质量超新星爆炸，代表超剥离超新星和吸积或并合引发的坍缩事件，在这些情况下，爆破更容易在更广的NS参数范围内实现，产生持续时间$10^{2\mbox{--}4}\,\mathrm{s}$、峰值亮度$10^{42\mbox{--}48}\,\mathrm{erg\,s^{-1}}$的快速X射线暂现源。我们的结果鼓励协调紫外、光学和X射线观测以约束宇宙中最高能NS的形成。
英文摘要：
Formation of a rapidly spinning, strongly magnetized neutron star (NS) may occur in various classes of core-collapse events. If the NS injects an amount of energy comparable to the explosion energy of the accompanying supernova (SN) before the SN ejecta becomes transparent, the nascent NS wind bubble can overtake the outer ejecta and undergo a blowout driven by hydrodynamic instabilities. Based on multidimensional numerical studies, we construct a minimal semi-analytic framework to follow the post-blowout dynamics and radiative evolution, map the blowout conditions by scanning the ejecta and NS parameters, and compute survey-ready multi-band light curves. For stripped-envelope SNe with an ejecta mass of $M_\mathrm{ej} \sim 10\,M_\odot$ and an explosion energy of $E_\mathrm{sn} \sim 10^{51}\,\mathrm{erg}$, blowout occurs for NSs with magnetic field strengths of $B_{\mathrm{dip}} \gtrsim 10^{13}\,\mathrm{G}$ and spin periods of $P_\mathrm{NS} \lesssim \mathrm{a\ few}\,\mathrm{ms}$. Relatively weak-field cases with $B_\mathrm{dip} \lesssim 10^{14}\,\mathrm{G}$ produce luminous double-peaked UV/optical light curves, as observed in the superluminous SN LSQ14bdq, while stronger-field cases with $B_\mathrm{dip} \gtrsim 10^{14}\,\mathrm{G}$ result in hypernovae preceded by X-ray blowout precursors. We also examine weaker and lower-mass SN explosions representing ultra-stripped SNe and accretion- or merger-induced collapse events, in which blowout is more readily achieved over a broader range of NS parameters, producing fast X-ray transients with durations of $ 10^{2\mbox{--}4}\,\mathrm{s}$ and peak luminosities of $10^{42\mbox{--}48}\,\mathrm{erg\,s^{-1}}$. Our results encourage coordinated UV, optical, and X-ray observations which constrain the formation of the most energetic NSs in the universe.
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