We present the results of an XMM-Newton observation of the slowly rotating ($P = 3.4$ s), highly magnetized ($B \approx 3 \times 10^{13}$ G) radio pulsar PSR J0726-2612. A previous X-ray observation with the Chandra satellite showed that some of the properties of PSR J0726-2612 are similar to those of the X-ray Dim Isolated Neutron Stars (XDINSs), a small class of nearby slow pulsars characterized by purely thermal X-ray spectra and undetected in the radio band. We confirm the thermal nature of the X-ray emission of PSR J0726-2612, which can be fit by the sum of two blackbodies with temperatures $kT_1 = 0.074_{-0.011}^{+0.006}$ keV and $kT_2 = 0.14_{-0.02}^{+0.04}$ keV and emitting radii $R_1 = 10.4_{-2.8}^{+10.8}$ km and $R_2 = 0.5_{-0.3}^{+0.9}$ km, respectively (assuming a distance of 1 kpc). A broad absorption line modeled with a Gaussian profile centred at $0.39_{-0.03}^{+0.02}$ keV is required in the fit. The pulse profile of PSR J0726-2612 is characterized by two peaks with similar intensity separated by two unequal minima, a shape and pulsed fraction that cannot be reproduced without invoking magnetic beaming of the X-ray emission. The presence of a single radio pulse suggests that in PSR J0726-2612 the angles that the dipole axis and the line of sight make with the rotation axis, $ξ$ and $χ$ respectively, are similar. This geometry differs from that of the two radio-silent XDINSs with a double peaked pulse profile similar to that of PSR J0726-2612, for which $ξ\sim 90^\circ$ and $χ\sim 45^\circ$ have been recently estimated. These results strengthen the similarity between PSR J0726-2612 and the XDINSs and support the possibility that the lack of radio emission from the latter might simply be due to an unfavourable viewing geometry.
Low Frequency Radio Imaging Study of PSR J1818-1607
IISER Bhopal（印度科学教育研究所博帕尔分校）；National Centre for Radio Astrophysics, SP Pune University Campus（国家射电天体物理中心，浦那大学校区）；Indian Institute of Technology Roorkee（印度理工学院罗尔基分校）；The Institute of Mathematical Sciences（数学科学研究院）；Homi Bhabha National Institute（霍米·巴巴国立研究所）
High-Energy emissions from the Pulsar/Be binary system PSR J2032+4127/MT91 213
PSR J2032+4127是一颗射电强伽玛射线脉冲星，它围绕一颗高质量Be型恒星运行，轨道周期长达25- 50年，并将在2017年底/2018年初接近近星点。该系统由一颗年轻的脉冲星和一颗Be型星组成，这颗Be型星类似于所谓的γ射线双星PSR~B1259-63/LS 2883。因此，预计PSR J2032+4127显示出由脉冲星风和Be风/近星盘之间的相互作用引起的高能发射增强。Ho等人最近报道了来自该系统的X射线通量的快速增加。在本文中，我们还证实了快速增加的X射线通量沿轨道，而GeV通量没有显着的变化。我们讨论了脉冲星风和星风相互作用引起的激波的高能辐射，并研究了脉冲星风在这一双星系统中的性质。我们认为，Swift观测到的X射线通量的增加率表明：（1）两风相互作用区域的动量比沿轨道的变化，或者（2）脉冲星风的磁化参数随离脉冲星径向距离的变化。我们还讨论了脉冲星风/Be盘在近星通道的相互作用，并提出了在脉冲星周围形成吸积盘的可能性。我们通过逆康普顿散射过程的冷相对论性脉冲星风小康软光子从吸积盘的高能量的排放。
Revealing the Unseen: The Discovery of Long-Awaited Radiation from the Intermittent Pulsar PSR B1931+24
Kashi University（喀什大学）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；Central China Normal University（华中师范大学）；University of Manchester（曼彻斯特大学）；Max-Planck Institut für Radioastronomie（马克斯·普朗克射电天文研究所）
Quasi-Simultaneous Radio/X-ray Observations of the Candidate Transitional Millisecond Pulsar 3FGL J1544.6-1125 During its Low-Luminosity Accretion-Disc State
Discovery of two millisecond pulsars in Fermi sources with the Nancay Radio Telescope
我们报告发现两个毫秒脉冲星在寻找无线电脉动的位置\emph{Fermi Large Area Telescope}源与以前没有已知的同行，使用Nançay射电望远镜。这两颗毫秒双星，PSR J2017+0603和J2302+4442的自转周期分别为2.896和5.192毫秒，并且都是低偏心率轨道的双星系统，轨道周期分别为2.2和125.9天，这表明它们有很长的再循环过程。这两个天体随后都探测到了伽马射线脉动，表明它们为发现它们的相关\emph{Fermi}源提供了动力。伽马射线光变曲线和光谱特性与之前探测到的伽马射线毫秒双星相似。对观测到的射电和伽马射线光变曲线的详细建模表明，伽马射线发射似乎起源于磁层的高海拔地区。此外，X射线观测揭示了PSR J2302+4442位置存在X射线源，与中子星的热辐射一致。这些发现以及在伽马射线中大量探测到射电巨响的毫秒双星表明，许多没有已知对应物的\emph{Fermi}源可能是未知的毫秒双星。
