Rotating radio transients (RRATs), loosely defined as objects that are discovered through only their single pulses, are sporadic pulsars that have a wide range of emission properties. For many of them, we must measure their periods and determine timing solutions relying on the timing of their individual pulses, while some of the less sporadic RRATs can be timed by using folding techniques as we do for other pulsars. Here, based on Parkes and Green Bank Telescope (GBT) observations, we introduce our results on eight RRATs including their timing-derived rotation parameters, positions, and dispersion measures (DMs), along with a comparison of the spin-down properties of RRATs and normal pulsars. Using data for 24 RRATs, we find that their period derivatives are generally larger than those of normal pulsars, independent of any intrinsic correlation with period, indicating that RRATs' highly sporadic emission may be associated with intrinsically larger magnetic fields. We carry out Lomb$-$Scargle tests to search for periodicities in RRATs' pulse detection times with long timescales. Periodicities are detected for all targets, with significant candidates of roughly 3.4 hr for PSR J1623$-$0841 and 0.7 hr for PSR J1839$-$0141. We also analyze their single-pulse amplitude distributions, finding that log-normal distributions provide the best fits, as is the case for most pulsars. However, several RRATs exhibit power-law tails, as seen for pulsars emitting giant pulses. This, along with consideration of the selection effects against the detection of weak pulses, imply that RRAT pulses generally represent the tail of a normal intensity distribution.
Spectral and Timing Nature of the Symbiotic X-ray Binary 4U 1954+319: The Slowest Rotating Neutron Star in an X-ray Binary System
共生的X射线双星4U 1954+319是一个罕见的系统，拥有一颗奇特的中子星（NS）和一颗M-型光学伴星。它的NS旋转周期约为5.4小时，是所有已知的吸积动力恒星中最长的，并且在8年内表现出很大的波动（约7%）。2012年，Swift/BAT在X射线增亮附近检测到自旋趋势转变。根据2011年和2012年的60 ks朱雀观测，在这次爆发之前和之后，源处于静止和明亮状态。观察到的连续体是很好地描述了一个康普顿模型，除了一个狭窄的6.4 keV的Fe K α线在爆发。高质量X射线双星的光谱与缓慢旋转的双星相似，它的高脉冲分数（~60-80%），以及在Corbet图中的位置有利于高B场（>~ 1 e +12 G），而不是像低质量X射线双星那样的弱场。观测到的低X射线光度（1 e +33- 1 e +35 erg/s），可能的宽轨道，和缓慢的恒星风的SyXB准球形吸积在亚音速沉降制度一个合理的模型。假设~ 1 e +13 G NS，该方案可以解释~5.4 h的平衡转动，而不需要使用吸积盘情形中所需的类磁场（~ 1 e +16 G）。多个不规则耀斑的时间尺度（~50 s）也可以归因于从阿尔芬壳层的自由落体时间（~ 1 e +13 G场）。超越规范的二元分类的SyXB的物理解释进行了讨论。
Discovery of 27 new Rotating Radio Transients by MeerTRAP
The University of Manchester（曼彻斯特大学）；Sydney Institute for Astronomy, School of Physics, The University of Sydney（悉尼大学物理学院天体物理研究所）；ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav)（引力波发现卓越研究中心）；The University of Oxford（牛津大学）；INAF - Osservatorio Astronomico di Roma（罗马天文台）；SKA Observatory（平方公里阵列射电望远镜观测站）；South African Radio Astronomy Observatory（南非射电天文观测台）
Multi-Method Timing of Transient Radio Pulsars with the GBT350 and GBNCC Surveys
West Virginia University（西弗吉尼亚大学）；Lafayette College（拉斐特学院）；Western Kentucky University（西肯塔基大学）；University of Amsterdam（阿姆斯特丹大学）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所 ASTRON）；Hillsdale College（山岭学院）；McGill University（麦吉尔大学）；University of Wisconsin-Milwaukee（威斯康星大学密尔沃基分校）；University of Manchester（曼彻斯特大学）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所 (ICE, CSIC)）；University of British Columbia（不列颠哥伦比亚大学）
Timing and statistical analysis of single-pulse search pulsar discoveries from the PALFA survey
West Virginia University（西弗吉尼亚大学）；Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；University of Wisconsin - Milwaukee（威斯康星大学密尔沃基分校）；Cornell Center for Astrophysics and Planetary Science（康奈尔天体物理学与行星科学中心）；South African Radio Astronomy Observatory（南非射电天文观测站）；Franklin and Marshall College（富兰克林和马歇尔学院）
Timing, Polarization, and Single-Pulse Properties of Long-Period FAST Pulsars
McGill University（麦吉尔大学）；Guizhou Normal University（贵州师范大学）；Tsinghua University（清华大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）
