当前位置: X-MOL 学术Mon. Not. R. Astron. Soc. › 论文详情
Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)
Measuring Interstellar Delays of PSR J0613−0200 over 7 years, using the Large European Array for Pulsars
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-09-28 , DOI: 10.1093/mnras/staa2955
R A Main 1 , S A Sanidas 2, 3 , J Antoniadis 1, 4, 5 , C Bassa 6 , S Chen 7, 8, 9 , I Cognard 7, 9 , M Gaikwad 1 , H Hu 1 , G H Janssen 6, 10 , R Karuppusamy 1 , M Kramer 1, 2 , K J Lee 11 , K Liu 1 , G Mall 1 , J W McKee 12 , M B Mickaliger 2 , D Perrodin 13 , B W Stappers 2 , C Tiburzi 6 , O Wucknitz 1 , L Wang 2, 14 , W W Zhu 14
Affiliation  

Using data from the Large European Array for Pulsars (LEAP), and the Effelsberg telescope, we study the scintillation parameters of the millisecond pulsar J0613-0200 over a 7 year timespan. The "secondary spectrum" -- the 2D power spectrum of scintillation -- presents the scattered power as a function of time delay, and contains the relative velocities of the pulsar, observer, and scattering material. We detect a persistent parabolic scintillation arc, suggesting scattering is dominated by a thin, anisotropic region. The scattering is poorly described by a simple exponential tail, with excess power at high delays; we measure significant, detectable scattered power at times out to $\sim 5 \mu s$, and measure the bulk scattering delay to be between 50 to 200\,ns with particularly strong scattering throughout 2013. These delays are too small to detect a change of the pulse profile shape, yet they would change the times-of-arrival as measured through pulsar timing. The arc curvature varies annually, and is well fit by a one-dimensional scattering screen $\sim 40\%$ of the way towards the pulsar, with a changing orientation during the increased scattering in 2013. Effects of uncorrected scattering will introduce time delays correlated over time in individual pulsars, and may need to be considered in gravitational wave analyses. Pulsar timing programs would benefit from simultaneously recording in a way that scintillation can be resolved, in order to monitor the variable time delays caused by multipath propagation.

中文翻译:

使用大型欧洲脉冲星阵列测量 PSR J0613−0200 超过 7 年的星际延迟

使用来自欧洲大型脉冲星阵列 (LEAP) 和埃菲尔斯堡望远镜的数据,我们研究了毫秒脉冲星 J0613-0200 在 7 年时间跨度内的闪烁参数。“二次光谱”——闪烁的二维功率谱——将散射功率呈现为时间延迟的函数,并包含脉冲星、观测器和散射材料的相对速度。我们检测到持续的抛物线闪烁弧,表明散射由薄的各向异性区域主导。简单的指数尾部很难描述散射,在高延迟时功率过剩;我们测量了显着的、可检测的散射功率,超时时间为 $\sim 5 \mu s$,并测量了 50 到 200\,ns 之间的体散射延迟,整个 2013 年散射特别强。这些延迟太小而无法检测到脉冲轮廓形状的变化,但它们会改变通过脉冲星计时测量的到达时间。弧曲率每年都在变化,并且非常适合一维散射屏幕 $\sim 40\%$ 朝向脉冲星的方式,在 2013 年散射增加期间改变方向。未校正散射的影响将引入时间延迟在单个脉冲星中随时间相关,可能需要在引力波分析中加以考虑。脉冲星定时程序将受益于以一种可以解决闪烁的方式同时记录,以便监测由多径传播引起的可变时间延迟。弧曲率每年都在变化,并且非常适合一维散射屏幕 $\sim 40\%$ 朝向脉冲星的方式,在 2013 年散射增加期间改变方向。未校正散射的影响将引入时间延迟在单个脉冲星中随时间相关,可能需要在引力波分析中加以考虑。脉冲星定时程序将受益于以一种可以解决闪烁的方式同时记录,以便监测由多径传播引起的可变时间延迟。弧曲率每年都在变化,并且非常适合一维散射屏幕 $\sim 40\%$ 朝向脉冲星的路径,在 2013 年散射增加期间改变方向。未校正散射的影响将引入时间延迟在单个脉冲星中随时间相关,可能需要在引力波分析中加以考虑。脉冲星定时程序将受益于以一种可以解决闪烁的方式同时记录,以便监测由多径传播引起的可变时间延迟。并且可能需要在引力波分析中加以考虑。脉冲星定时程序将受益于以一种可以解决闪烁的方式同时记录,以便监测由多径传播引起的可变时间延迟。并且可能需要在引力波分析中加以考虑。脉冲星定时程序将受益于以一种可以解决闪烁的方式同时记录,以便监测由多径传播引起的可变时间延迟。
更新日期:2020-09-28
down
wechat
bug