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arXiv 0810.1118astro-ph
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脉冲星PSR B0809 +74和B0950 +08的星际等离子体Turbulence谱

Interstellar Plasma Turbulence Spectrum Toward the Pulsars PSR B0809+74 and B0950+08

T. V. Smirnova, V. I. Shishov

备注：
13 pages, 11 figures
发表信息：
Astron.Rep.52:736,2008
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摘要：

利用低频（41、62、89和112 MHz）观测研究了双星PSR B 0809 +74和B 0950 +08的星际振动。在这些频率的衍射衍射的特征时间和频率尺度已被确定。综合分析的频率和时间结构函数减少到相同的频率表明，星际等离子体的频谱不均匀性向两个恒星的幂律描述。朝向PSR B 0950 +08（n = 3.00 +-0.05）的星际等离子体不均匀性的波动谱的指数与柯尔莫哥洛夫指数明显不同。对于PSR B 0809 +74，频谱为幂律，指数n = 3.7 +- 0.1。已检测到朝向PSR B 0950 +08的强烈角折射。沿视线的不均匀性的分布进行了分析，它已被证明，PSR B 0950 +08发生的湍流层与增强的电子密度，这是本地化在约10 pc的观察者。对于PSR B 0809 +74，不均匀性的分布是准均匀的。我们估计了四个非均匀体上电子密度的均方涨落，其特征尺度为rho_0 = 10^7 m。在这个尺度上，10-pc层中的局部湍流水平比导致PSR B 0809 +74湍流的扩展区域高20倍。

英文摘要：

Interstellar scintillations of pulsars PSR B0809+74 and B0950+08 have been studied using observations at low frequencies (41, 62, 89, and 112 MHz). Characteristic temporal and frequency scales of diffractive scintillations at these frequencies have been determined. The comprehensive analysis of the frequency and temporal structure functions reduced to the same frequency has shown that the spectrum of interstellar plasma inhomogeneities toward both pulsars is described by a power law. The exponent of the spectrum of fluctuations of interstellar plasma inhomogeneities toward PSR B0950+08 (n = 3.00 +- 0.05) appreciably differs from the Kolmogorov exponent. Toward PSR B0809+74 the spectrum is a power law with an exponent n = 3.7 +- 0.1. A strong angular refraction has been detected toward PSR B0950+08. The distribution of inhomogeneities along the line of sight has been analyzed; it has been shown that the scintillations of PSR B0950+08 take place on a turbulent layer with enhanced electron density, which is localized at approximately 10 pc from the observer. For PSR B0809+74 the distribution of inhomogeneities is quasi-uniform. Mean-square fluctuations of electron density on inhomogeneities with a characteristic scale rho_0 = 10^7 m toward four pulsars have been estimated. On this scale the local turbulence level in the 10-pc layer is 20 times higher than in an extended region responsible for the scintillations of PSR B0809+74.

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