Unraveling the Eclipse Mechanism of a Binary Millisecond Pulsar Using Broadband Radio Spectra
Unraveling the Eclipse Mechanism of a Binary Millisecond Pulsar Using Broadband Radio Spectra
复制标题
使用宽带射电频谱揭示二元毫秒脉冲星的日食机制
DOI：
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发表时间：
2021
影响因子：
4.9
通讯作者：
B. Stappers
中科院分区：
文献类型：
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作者：
Devojyoti Kansabanik;B. Bhattacharyya;J. Roy;B. Stappers
致密双星系统中毫秒双星射电辐射的频率相关食提供了一个了解食机制和确定食介质性质的机会。我们结合联合收割机多频观测升级的巨型米波射电望远镜和模型的宽带无线电频谱的光学厚到薄的过渡制度，以约束日食机制。日食相位谱的最佳拟合模型有利于相对论电子的同步辐射吸收。我们能够将日食开始的频率严格限制在345 ± 5 MHz，这比以前的估计精确了一个数量级。同步加速器吸收对磁场强度的依赖性使我们能够估计日食介质的磁场强度为13G，这与考虑入射脉冲星风和伴星风之间的压力平衡所获得的值非常相似。将这种方法应用于其他毫秒双星，将使我们能够确定是否日食机制都是相同的，也估计的风和磁场的伴星的属性。该方法也可以应用于其他系统中的双星与伴风相互作用的双星系统，在所有情况下，它将导致更好地了解演变过程。
The frequency dependent eclipses of the radio emission from millisecond pulsars in compact binary systems provide an opportunity to understand the eclipse mechanism and to determine the nature of the eclipsing medium. We combine multifrequency observations from the upgraded Giant Metrewave Radio Telescope and model the broadband radio spectrum in the optically thick to thin transition regime to constrain the eclipse mechanism. The best-fit model to the eclipse phase spectra favors synchrotron absorption by relativistic electrons. We are able to strongly constrain the frequency of onset of the eclipse to 345 ± 5 MHz, which is an order of magnitude more precise than previous estimates. The dependence on the magnetic field strength of synchrotron absorption allowed us to estimate the magnetic field strength of the eclipse medium to be ∼13 G, which is very similar to the values obtained by considering a pressure balance between the incident pulsar wind and the stellar wind of the companion. Applying this method to other millisecond binary pulsars will enable us to determine if the eclipse mechanisms are all the same and also estimate the wind and magnetic field properties of the companion stars. The method could also be applied to other systems where pulsars interact with companion winds in binary systems and in all cases it will lead to a better understanding of the evolutionary processes.
影响因子：
4.8
作者：
E. J. Polzin;R. Breton;A. O. Clarke;V. Kondratiev;B. Stappers;J. Hessels;C. Bassa;J. Broderick;J. Grießmeier;C. Sobey;S. Veen;J. V. Leeuwen;P. Weltevrede
通讯作者：
E. J. Polzin;R. Breton;A. O. Clarke;V. Kondratiev;B. Stappers;J. Hessels;C. Bassa;J. Broderick;J. Grießmeier;C. Sobey;S. Veen;J. V. Leeuwen;P. Weltevrede