论文标题
使用闪烁弧对PSR〜J1909-3744的离子星际介质和轨道动力学进行分析
Analysis of the ionized interstellar medium and orbital dynamics of PSR~J1909-3744 using scintillation arcs
论文作者
论文摘要
二元毫秒脉冲星（MSP）的长期研究提供了强场重力的精确测试，可用于测量中子星质量。 PSR〜J1909 $ - $ 3744，二进制MSP已成为多个PULSAR计时分析的主题。边缘轨道可以使用Shapiro延迟来测量其质量；但是，从倾斜角度，$ i $的意义上存在退化，以及用于上升节点的经度的多个解决方案，$ω$。由于离子化星际培养基（IISM）中的不均匀性引起的无线电脉冲星。这可能会导致动态光谱的功率光谱中的闪烁电弧，这些弧线可以使用它们来研究星际培养基并限制二元脉冲星轨道。在这里，我们使用64米Parkes射程望远镜（Murriyang）的观测值研究了PSR〜J1909-3744的闪烁，以$ \ $ \ $ \ $ 13 \，使用该技术在较低的信号到噪声方面研究闪烁。通过监测弧曲率测量的年度和轨道变化，我们能够表征Iism的速度。我们发现，这段时间内IISM的统计数据保持静止，并且首选略有各向异性模型（轴向比率$ \ gtrsim1.2 $）。我们在$ s = 0.49 \ pm0.04 $或$ d_s = 590 \ pm50 $ \，PC的相对距离与单个显性薄散射屏幕的相对距离，具有各向异性$ζ= 85 \ pm6^\ circ $（北部），并且在Anisotropy $ v _ _ _ \ _ _ \ _ \ _ \ velmit方向上ζ} = 14 \ pm10 $ \，km \，s $^{ - 1} $。通过结合IISM的物理模型和当前的PULSAR正时结果，我们还限制了$ω= 225 \ pm3^\ circ $和$ i = 86.46 \ pm0.05^\ circ $。
Long-term studies of binary millisecond pulsars (MSPs) provide precise tests of strong-field gravity and can be used to measure neutron-star masses. PSR~J1909$-$3744, a binary MSP has been the subject of several pulsar timing analyses. The edge-on orbit enables measurement of its mass using the Shapiro delay; however, there is degeneracy in the sense of the inclination angle, $i$, and multiple solutions for the longitude of ascending node, $Ω$. Radio pulsars scintillate due to inhomogeneities in the ionized interstellar medium (IISM). This can result in scintillation arcs in the power spectrum of the dynamic spectrum that can use these to study the interstellar medium and constrain binary pulsar orbits. Here, we study the scintillation of PSR~J1909-3744 using observations from the 64-m Parkes Radio Telescope (Murriyang) over $\approx$13\, years, using techniques to study scintillation in a lower signal-to-noise regime. By monitoring annual and orbital variations of the arc-curvature measurements we are able to characterise the velocity of the IISM. We find that the statistics of the IISM remained stationary over this time and a slightly anisotropic model (axial ratio $\gtrsim1.2$) is preferred. We measure the relative distance to a single dominant thin scattering screen at $s=0.49\pm0.04$, or $D_s=590\pm50$\,pc, with an angle of anisotropy $ζ=85\pm6^\circ$ (East of North) and velocity in the direction of anisotropy $V_{\textrm{IISM}, ζ}=14\pm10$\,km\,s$^{-1}$. By combining a physical model of the IISM and current pulsar timing results, we also constrain $Ω=225\pm3^\circ$ and $i=86.46\pm0.05^\circ$.
