PSR~J1910$-$5959A: A rare gravitational laboratory for testing white dwarf models
A. Corongiu, V. Venkatraman Krishnan, P. C. C. Freire, M. Kramer, A. Possenti, M. Geyer, A. Ridolfi, F. Abbate, M. Bailes, E. D. Barr, V. Balakrishnan, S. Buchn… 展开作者
A. Corongiu, V. Venkatraman Krishnan, P. C. C. Freire, M. Kramer, A. Possenti, M. Geyer, A. Ridolfi, F. Abbate, M. Bailes, E. D. Barr, V. Balakrishnan, S. Buchner, D. J. Champion, W. Chen, B. V. Hugo, A. Karastergiou, A. G. Lyne, R. N. Manchester, P. V. Padmanabh, A. Parthasarathy, S. M. Ransom, J. M. Sarkissian, M. Serylak, W. van Straten
备注：
18 pages, 12 figures. Abstract shortened and rephrased because of arXiv characters limits. Accepted for publication on A&A on January 9th 2023 Updated version after linguistic revision
PSRJ1910-5959A (J1910A) is a binary millisecond pulsar in a 0.837 day circular orbit around a helium white dwarf (HeWD) companion. This pulsar is located 6.3 arcmin away from the centre of the globular cluster NGC6752. Given the large offset, the association of the pulsar to NGC6752 has been debated. We have made use of two decades of archival Parkes 64-m "Murriyang" telescope data and recently carried out observations with the MeerKAT telescope. We obtained Pulse times of arrival using standard data reduction techniques and analysed using Bayesian pulsar timing techniques. We analysed the pulsar's total intensity and polarisation profile, to study the interstellar scattering along the line of sight, and the pulsar's geometry by applying the rotating vector model. We obtain precise measurements of several post-Keplerian parameters: the range $r=0.202(6)T_\odot$ and shape s=0.999823(4) of the Shapiro delay, from which we infer the orbital inclination to be $88.9^{+0.15}_{-0.14}°$ and the masses of both the pulsar and the companion to be $1.55(7)M_{\odot}$ and $0.202(6)M_{\odot}$ respectively; a secular change in the orbital period $\dot{P}_{\rm b}=-53^{+7.4}_{-6.0}\times 10^{-15}$\,s\,s$^{-1}$ that proves the association to NGGC6752 and a secular change in the projected semi-major axis of the pulsar $\dot{x}= -40.7^{+7.3}_{-8.2}\times10^{-16}$\,s\,s$^{-1}$ that is likely caused by the spin-orbit interaction from a misaligned HeWD spin, at odds with the likely isolated binary evolution of the system. We also discuss some theoretical models for the structure and evolution of WDs in NS-WD binaries by using J1910A's companion as a test bed. J1910A is a rare system for which several parameters of both the pulsar and the HeWD companion can be accurately measured. As such, it is a test bed to discriminate between alternative models for HeWD structure and cooling.
PSR J2032+4127, the counterpart of TeV J2032+4130? Multiwavelength Monitoring of the Approach to Periastron
PSR J2032+4127最近被发现是一个长周期（45-50年）双星，与Be星MT 91 213在一个高偏心轨道上。近日星将于2017年11月发生，这一罕见的事件促使多波长监测活动，以确定该系统是否是伽马射线双星，如果是的话，研究什么将是已知紧凑物体的第二个伽马射线双星。在与TeV J2032+4130相同的方向上，来自这个双星系统的伽马射线发射可能与来自该区域的扩展的非常高能量的伽马射线发射有关。作为监测的一部分，Swift、Fermi-LAT和VERITAS正在进行观测。我们介绍了这些观测的现状、初步结果和通过近星点继续监测的计划。
A Unified Multi-Band Secular Framework for the Hierarchical Triple PSR J0435+3233 System
Tata Institute of Fundamental Research（塔塔基础研究所）；Indian Institute of Science Education and Research Thiruvananthapuram（特鲁凡得琅印度科学教育与研究学院）；University of Turku（图尔库大学）；Tsinghua University（清华大学）；Chinese Academy of Sciences（中国科学院）
Radio eclipse of the slowest spinning Galactic-field spider pulsar PSR J1932+2121 and its X-ray emission prospect
Central China Normal University（华中师范大学）；Institute of Astrophysics, Central China Normal University（华中师范大学天体物理研究所）；Laboratory for Compact Object Astrophysics and Astronomical Technology, Central China Normal University（华中师范大学致密天体天文学与技术实验室）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）
PSR J2222--0137. I. Improved physical parameters for the system
PSR J2222-0137双星系统是一个独特的重力理论实验室。为了充分利用其潜在的测试，我们的目标是改善其物理参数的测量：自旋，轨道方向，和后开普勒参数量化观察到的相对论效应。我们提出了改进的分析档案VLBI数据，使用坐标公约，在时间上使用的完全一致。我们还获得了更好的旋光与FAST。我们提供了一个显着延长的时间与Effelsberg，Nancay，Lovell和绿银行望远镜的数据进行分析。通过VLBI分析，我们得到了升交点位置角的新估计，ω =189（19）度，以及具有更保守不确定度的脉冲星的新位置。FAST旋光测量，特别是检测脉冲间，产生更好的估计的自旋几何形状的脉冲星，特别是84度的自旋轴的倾角。由Shapiro延迟与近星点推进率的一致性，得到了一个新的广义相对论（GR）的1%检验。在自洽分析中假设GR，我们得到脉冲星和伴星的质量分别为1.831（10）M_sun和1.319（4）M_sun，总质量为3.150（14）M_sun，证实它是银河系中已知质量最大的双简并双星。这个分析也产生了轨道方向：轨道倾角为85.27（4）度，表明脉冲星的自旋和轨道角动量之间的紧密对齐;欧米茄= 188（6）度，与我们的VLBI结果相匹配。我们还得到了轨道周期导数的精确值0.251（8）e-12 s^-1，这与GR预测的多普勒因子加上引力波（GW）发射引起的轨道衰减的预期变化一致。
Improved proper motion and gravity tests with PSR J1913+1102
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Aalborg University（奥尔堡大学）；Henan Academy of Sciences（河南省科学院）；Beijing Normal University（北京师范大学）；University of East Anglia（东英吉利大学）；University of Manchester（曼彻斯特大学）
