Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes
Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes
复制标题
用MAGIC望远镜观测黑寡妇B1957 20毫秒脉冲星双星系统
DOI：
10.1093/mnras/stx1405
复制
发表时间：
2017
影响因子：
4.8
通讯作者：
Sitarek J. et al.
中科院分区：
文献类型：
--
作者：
Ahnen M. L.; Saito T.;Sitarek J. et al.
B1957+20是一颗毫秒脉冲星，位于黑寡妇型紧凑型双星系统中，有一颗低质量恒星伴星。脉冲星风与伴星风和/或星际等离子体的相互作用有望为电子加速到TeV能量和随后在逆康普顿过程中产生高能γ射线创造合理的条件。我们利用B1957+20的主要大气伽马成像切伦科夫望远镜（MAGIC）望远镜进行了广泛的观测。我们在几个不同模型的框架下解释结果，即毫秒脉冲星附近的发射，脉冲星与恒星伴星风区或弓形激波星云的相互作用。没有发现明显的稳定的高能γ射线发射。我们推导出200 GeV以上双星系统γ射线平均发射的95%置信上限为3.0 × 10−12cm−2s−1。MAGIC得到的上限首次约束了B1957+20高能辐射的不同模型。特别是，在单能量电子注入的内部混合风星云模型中，电子的加速效率被限制在脉冲星自旋下降功率的~ 2 - 10%以下。对于脉冲星发射，所获得的每个发射峰值的上限都远高于指数截止拟合的费米- lat数据，外推到50 GeV以上的能量。MAGIC上限可以排除在无线电频率主峰的亚tev能量范围内的简单幂律尾延伸。
B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12cm−2s−1on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to theFermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies.