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首页> 外文期刊>The Astrophysical journal >PSR J1833-1034: DISCOVERY OF THE CENTRAL YOUNG PULSAR IN THE SUPERNOVA REMNANT G21.5-0.9
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PSR J1833-1034: DISCOVERY OF THE CENTRAL YOUNG PULSAR IN THE SUPERNOVA REMNANT G21.5-0.9

机译：PSR J1833-1034：超新星遗迹G21.5-0.9中的中央年轻脉冲的发现

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摘要

We have discovered the pulsar associated with the supernova remnant G21.5-0.9. PSR J1833-1034, with spin period P = 61.8 ms and dispersion measure 169 cm~(-3) pc, is very faint, with pulse-averaged flux density of ≈70 μJy at a frequency of 1.4 GHz, and was first detected in a deep search with the Parkes telescope. Subsequent observations with Parkes and the Green Bank Telescope have confirmed this detection and yield a period derivative P = 2.02 x 10~(-13). These spin parameters imply a characteristic age τ_c = 4.8 kyr and a spin-down luminosity E = 3.3 x 10~(37) ergs s~(-1), the latter value exceeded only by the Crab pulsar among the rotation-powered pulsars known in our Galaxy. The pulsar has an unusually steep radio spectrum in the 0.8-2.0 GHz range, with power-law index ≈3.0, and a narrow single-peaked pulse profile with FWHM of 0.04P. We have analyzed 350 ks of archival Chandra X-Ray Observatory HRC data and find a pointlike source of luminosity ≈3 x 10~(-5)E, offset from the center of an elliptical region of size ≈7″ x 5″ and luminosity ≈10~(-3)E within which likely lies the pulsar wind termination shock. We have searched for X-ray pulsations in a 30 ks HRC observation without success, deriving a pulsed fraction upper limit for a sinusoidal pulse shape of about 70% of the pulsar flux. We revisit the distance to G21.5-0.9 based on H I and CO observations, arguing that it is 4.7 ± 0.4 kpc. We use existing X-ray and radio observations of the pulsar wind nebula, along with the measured properties of its engine and a recent detection of the supernova remnant shell, to argue that G21.5-0.9 and PSR J1833-1034 are much younger than τ_c and likely their true age is approx < 1000 yr. In that case, the initial spin period of the pulsar was approx > 55 ms.
机译：我们发现了与超新星残余G21.5-0.9相关的脉冲星。 PSR J1833-1034的自旋周期P = 61.8 ms，色散测量为169 cm〜（-3）pc，非常微弱，在1.4 GHz频率下的脉冲平均磁通密度为≈70μJy，首先在使用派克斯望远镜进行深入搜索。随后用Parkes和Green Bank望远镜进行的观测证实了这一发现，并得出了周期导数P = 2.02 x 10〜（-13）。这些自旋参数暗示着特征年龄τ_c= 4.8 kyr，自旋下降的光度E = 3.3 x 10〜（37）ergs s〜（-1），后者值仅在已知的旋转脉冲星中被蟹状脉冲星超过在我们的银河系中。脉冲星在0.8-2.0 GHz范围内具有异常陡峭的无线电频谱，幂律指数≈3.0，FWHM为0.04P时具有狭窄的单峰脉冲轮廓。我们分析了350 ks钱德拉X射线观测天文台HRC数据，发现了点状光源的发光度≈3x 10〜（-5）E，偏离了尺寸约为≈7“ x 5”的椭圆形区域的中心和发光度≈10〜（-3）E，其中可能存在脉冲星风终止冲击。我们已经在30 ks HRC观测中搜索了X射线脉动，但没有成功，得出了约70％脉冲星通量的正弦脉冲形状的脉冲分数上限。我们基于H I和CO观测值重新考虑到G21.5-0.9的距离，认为它是4.7±0.4 kpc。我们利用脉冲星云的现有X射线和无线电观测，以及其发动机的测量特性以及对超新星残留壳的最新探测，认为G21.5-0.9和PSR J1833-1034比τ_c，并且他们的真实年龄可能约为<1000年。在这种情况下，脉冲星的初始自旋周期约为> 55 ms。

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