标题： 白矮星-中子星或白矮星-黑洞合并过程中反复的部分扰动调制了长时标并合型伽马射线暴的瞬时辐射 显示英文标题

标题： Repeated partial disruptions in a WD-NS or WD-BH merger modulate the prompt emission of long-duration merger-type GRBs

摘要： 伽马射线暴（GRB）的起源一直是未解之谜。GRB 230307A 是一个非常明亮的事件，属于长时标GRB，但同时表现出类似于千倍新星的晚期辐射成分。与类似的事件 GRBs 060614 和 211211A 一起，它们构成了一个新的子类 GRB，具有有趣的起源系统。如果像最近文献中提出的那样，这类长时标合并型GRB起源于白矮星（WD）与中子星（NS）或黑洞（BH）的合并，那么由于白矮星较大的潮汐破坏半径以及不可忽略的残余轨道偏心率，重复的部分潮汐破坏将是不可避免的。这可能会调制中子星或黑洞的质量吸积和喷流发射过程，在轨道周期上导致伽马射线暴光变曲线上的准周期调制（QPM）。在这三个GRB的早期瞬时辐射阶段检测到潜在的QPM支持了这一场景，而相对较慢的QPM（$>$1 s）表明较轻的天体不可能是中子星。我们提出GRBs 230307A、060614和211211A的前身系统分别由质量为1.3$M_\odot$、0.9$M_\odot$和1.4$M_\odot$的白矮星和中子星（或黑洞）组成。经过几次调制循环后，白矮星被完全摧毁，剩余碎片的吸积主导了延长的辐射阶段。 显示英文摘要

摘要： The progenitors of gamma-ray bursts (GRBs) have long been an unresolved issue. GRB 230307A stands out as an exceptionally bright event, belonging to the long-duration GRBs but also exhibiting a late emission component reminiscent of a kilonova. Together with the similar events GRBs 060614 and 211211A, they make up a new sub-group of GRBs with intriguing progenitors. If such long-duration merger-type GRBs originated from the coalescence of a white dwarf (WD) with a neutron star (NS) or a black hole (BH), as proposed in the recent literature, then the larger tidal disruption radius of the WD, together with a non-negligible residual orbital eccentricity, would make repeated partial tidal disruptions inevitable. This may modulate the mass accretion and jet launching process at the NS or BH, resulting in a quasi-periodic modulation (QPM) in the light curve of the GRB, on the orbital period. The detection of potential QPMs during the early episode of prompt emission of these three GRBs supports this scenario, and the relatively slow QPM ($>$ 1 s) suggests that the lighter object can not be a NS. We propose that the progenitor system of GRBs 230307A, 060614, and 211211A consist of a WD of mass 1.3 $M_\odot$, 0.9 $M_\odot$ and 1.4 $M_\odot$, respectively, and a NS (or BH). After several cycles of modulations, the WD is completely destructed, and the accretion of the remaining debris dominates the extended emission episode.