The Vela Pulsar’s Proper Motion and Parallax Derived from VLBI Observations
The Vela Pulsar’s Proper Motion and Parallax Derived from VLBI Observations
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DOI：
10.1086/378089
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发表时间：
2003-02
期刊：
影响因子：
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通讯作者：
Richard Dodson;D. Legge;John E. Reynolds;P. McCulloch
中科院分区：
文献类型：
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作者：
Richard Dodson;D. Legge;John E. Reynolds;P. McCulloch
船帆座脉冲星是射电波段最亮的脉冲星。正是这个物体（通过它的小故障）告诉我们，恒星是固体旋转体，而不是振荡体。沿着蟹状星云脉冲星，它是许多脉冲星行为模型的来源。因此，了解它的距离和起源至关重要。Vela脉冲星的自行和视差是由2.3和8.4 GHz甚长基线干涉测量（VLBI）观测得到的。数据跨度为6.8年，包括11个时期。我们得到一个自行μα cos δ = -49.68 ± 0.06，μδ = 29.9 ± 0.1 mas yr-1，视差3.5 ± 0.2 mas，相当于287 pc的距离。当我们减去银河系自转和太阳特有速度时，我们得到μ* = 45 ± 1.3 mas yr-1，位置角为301° ± 1.8 °，这意味着自行相对于X射线星云的对称轴有一个很小但很大的偏移。
The Vela pulsar is the brightest pulsar at radio wavelengths. It was the object that told us (via its glitching) that pulsars were solid rotating bodies not oscillating ones. Along with the Crab pulsar, is it the source of many of the models of pulsar behavior. Therefore it is of vital importance to know how far away it is and its origin. The proper motion and parallax for the Vela pulsar have been derived from 2.3 and 8.4 GHz very long baseline interferometry (VLBI) observations. The data span 6.8 years and consist of 11 epochs. We find a proper motion of μα cos δ = -49.68 ± 0.06, μδ = 29.9 ± 0.1 mas yr-1 and a parallax of 3.5 ± 0.2 mas, which is equivalent to a distance of 287 pc. When we subtract out the Galactic rotation and solar peculiar velocity, we find μ* = 45 ± 1.3 mas yr-1 with a position angle of 301° ± 1.°8 which implies that the proper motion has a small but significant offset from the X-ray nebula's symmetry axis.