PSRs B1757-24和B1951 +32的自主运动：年龄和关联的意义
Proper Motions of PSRs B1757-24 and B1951+32: Implications for Ages and Associations
摘要：
在过去的十年中，人们付出了相当大的努力来测量双星B1757-24和B1951+32的自行，以建立或反驳与附近超新星遗迹的关联，并更好地了解其周围星云的复杂几何形状。我们提出了自行测量的两个恒星与甚大阵列，增加测量的时间基线从3.9年到6.5年和从12.0年到14.5年，分别与以前的观测相比。我们确认PSR B1757-24的自行未被检测到，并且我们的测量（mu_a，mu_d）=（-11 +/- 9，-1 +/- 15）mas yr^{-1}证实PSR B1757-24与SNR G5.4-1.2的关联对于15.5 kyr的脉冲星特征年龄是不可能的，尽管对于明显更大的年龄不能排除关联。对于PSR B1951+32，我们测量到自行（mu_a，mu_d）=（-28.8 +/- 0.9，-14.7 +/- 0.9）mas yr^{-1}，与以前的结果相比，自行的不确定性降低了两倍。在修正到当地的静止标准后，自行表明脉冲星的动力学年龄约为51 kyr，假设它出生在超新星遗迹的几何中心附近。沿着脉冲星自行矢量的射电亮弧显示出时变结构，但与脉冲星以约2.5”的恒定间隔移动，这为将其解释为脉冲星驱动的激波结构提供了依据。
英文摘要：
Over the last decade, considerable effort has been made to measure the proper motions of the pulsars B1757-24 and B1951+32 in order to establish or refute associations with nearby supernova remnants and to understand better the complicated geometries of their surrounding nebulae. We present proper motion measurements of both pulsars with the Very Large Array, increasing the time baselines of the measurements from 3.9 yr to 6.5 yr and from 12.0 yr to 14.5 yr, respectively, compared to previous observations. We confirm the non-detection of proper motion of PSR B1757-24, and our measurement of (mu_a, mu_d) = (-11 +/- 9, -1 +/- 15) mas yr^{-1} confirms that the association of PSR B1757-24 with SNR G5.4-1.2 is unlikely for the pulsar characteristic age of 15.5 kyr, although an association can not be excluded for a significantly larger age. For PSR B1951+32, we measure a proper motion of (mu_a, mu_d) = (-28.8 +/- 0.9, -14.7 +/- 0.9) mas yr^{-1}, reducing the uncertainty in the proper motion by a factor of two compared to previous results. After correcting to the local standard of rest, the proper motion indicates a kinetic age of ~51 kyr for the pulsar, assuming it was born near the geometric center of the supernova remnant. The radio-bright arc of emission along the pulsar proper motion vector shows time-variable structure, but moves with the pulsar at an approximately constant separation ~2.5", lending weight to its interpretation as a shock structure driven by the pulsar.
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