论文标题
搜索使用GMRT的较晚无线电观察从较晚的无线电观察开始的合并弹射器排放
Search for merger ejecta emission from late time radio observations of short GRBs using GMRT
论文作者
论文摘要
短伽马射线爆发(GRB)是涉及中子星的紧凑型二进制合并的后果。如果合并残留物是毫秒的磁铁而不是黑洞,则沉积在新兴喷射中的旋转能量中很大一部分可以通过与环境介质的相互作用来产生延迟的无线电。从短GRB中检测这种延迟时间的无线电发射可能对理解祖细胞的物理学具有深远的影响。我们报告了五个短GRB的无线电观察结果-050709、061210、100625A,140903A和160821B,使用巨大的Metrewave Radio望远镜(GMRT)在1250、610和325 MHz频率下$ \ sim $ \ sim $ 2-11 $ 2-11美元以后,从1250、610和325 MHz频率开始。在低频下的GMRT观测对于检测峰值合并弹射发射的特征尤为重要。这些观察结果是与这些GRB有关的最延迟的搜索,对于任何延迟的低频排放。我们没有发现这种排放的证据。我们发现,这些GRB都不与最大旋转的磁力一致,旋转能量为$ \ sim 10^{53} \,{\ rm ergs} $。但是,不能完全排除具有较低旋转能的磁铁。尽管没有发现,但我们的研究强调了无线电观测的力量,在寻找与短GRB相关的磁性特征中。但是,只有将来的无线电观测值才能具有检测这些签名或对模型更加严格的约束的功能。
Short gamma-ray bursts (GRBs) are the aftermath of compact binary mergers involving neutron stars. If the merger remnant is a millisecond magnetar instead of a black hole, a significant proportion of the rotational energy deposited to the emerging ejecta can produce a late-time radio brightening from its interaction with the ambient medium. Detection of this late-time radio emission from short GRBs can have profound implications for understanding the physics of the progenitor. We report the radio observations of five short GRBs - 050709, 061210, 100625A, 140903A, and 160821B using the Giant Metrewave Radio Telescope (GMRT) at 1250, 610, and 325 MHz frequencies after $\sim$ $2 - 11$ years from the time of the burst. The GMRT observations at low frequencies are particularly important to detect the signature of merger ejecta emission at the peak. These observations are the most delayed searches associated with some of these GRBs for any late-time low-frequency emission. We find no evidence for such an emission. We find that none of these GRBs are consistent with maximally rotating magnetar with a rotational energy of $\sim 10^{53}\, {\rm ergs}$. However, magnetars with lower rotational energies cannot be completely ruled out. Despite the non detection, our study underscores the power of radio observations in the search for magnetar signatures associated with short GRBs. However, only future radio observatories may have the capabilities to either detect these signatures or put more stringent constraints on the model.