• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>The Astrophysical journal >RESOLVING GAMMA-RAY BURST 00030lC WITH A GRAVITATIONAL MICROLENS
【24h】

RESOLVING GAMMA-RAY BURST 00030lC WITH A GRAVITATIONAL MICROLENS

机译：用引力微缩技术解决伽马射线暴00030lC

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

The afterglow of the gamma-ray burst (GRB) 00030lC exhibited achromatic, short-timescale variability that is difficult to reconcile with the standard relativistic shock model. We interpret the observed light curves as a microlensing event superposed on power-law flux decays typical of afterglows. In general, a relativistic GRB shock appears on the sky as a thin ring expanding at a superluminal speed. Initially the ring is small relative to its angular separation from the lens, and so its flux is magnified by a constant factor As the ring grows and sweeps across the lens, its magnification reaches a maximum. Subsequently, the flux gradually recovers its unlensed value. This behavior involves only three free parameters in its simplest formulation and was predicted theoretically by A. Loeb & R. Perna. Fitting the available R-band photometric data of GRB 00030lC to a simple model of the microlensing event and a broken power law for the afterglow, we find reasonable values for all the parameters and a reduced X'/degrees of freedom parameter of l .48 compared with 2.99 fOr the broken powerlaw fit alone. The peak magnification of ~2 occurred 3.8 days after the burst. The entire optical to IR data imply a width of the GRB ring of order l0% of its radius, similar to theoretical expectations. The angular resolution provided by microlensing is better than a microarcsecond. We infer a mass of approximately 0.5 Mo for a lens located halfway Lo the source at z. = 2.04. A galaxy 2" from GRB 000301C might be the host of the stellar lens, but current data provides only an upper limit on its surface brightness at the GRB position.
机译：伽玛射线爆发（GRB）00030lC的余辉显示出消色差，短时标变化性，很难与标准相对论冲击模型进行协调。我们将观察到的光曲线解释为叠加在余辉典型的幂律通量衰减上的微透镜事件。通常，相对论的GRB震荡以超光速扩张的细环出现在天空中。最初，该环相对于其与透镜的角度间隔较小，因此其通量会放大一个恒定因子。当环长大并扫过透镜时，其放大率达到最大值。随后，通量逐渐恢复其非透镜值。此行为最简单的公式仅涉及三个自由参数，并且由A. Loeb＆R. Perna从理论上进行了预测。将GRB 00030lC的可用R波段光度数据拟合到微透镜事件的简单模型和余辉的折光力定律，我们发现所有参数的合理值以及降低的X'/自由度参数为.48与2.99相比，单独的断电定律适合。爆裂后3.8天出现了最大放大倍数〜2。整个光学到IR数据意味着GRB环的宽度约为其半径的10％，与理论预期相似。通过微透镜提供的角分辨率比微秒更好。对于位于z处源Lo中途的透镜，我们推断出质量约为0.5Mo。 = 2.04。来自GRB 000301C的2英寸星系可能是恒星透镜的主体，但是当前数据仅提供了其在GRB位置的表面亮度的上限。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号