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arXiv 1509.08754astro-ph.SR
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2009年IBEX-Lo测量的星际氢通量：数值模拟和数据比较

Interstellar hydrogen fluxes measured by IBEX-Lo in 2009: numerical modeling and comparison with the data

O. A. Katushkina, V. V. Izmodenov, D. B. Alexashov, N. A. Schwadron, D. J. McComas

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摘要：

在本文中，我们使用日光层中星际中性氢分布的最新动力学模型，对IBEX-Lo在23号轨道（2009年春季）期间测量的星际氢通量进行了数值建模。该模型考虑了太阳参数的时间和日纬度变化以及由于日光层界面电荷交换引起的氢分布的非麦克斯韦动力学性质。我们发现，有一个定性的差异之间的IBEX-Lo数据和三维，时间依赖性模型的建模结果。也就是说，该模型预测能量仓~2（20-41 eV）中的计数率比能量仓~1（11-21 eV）中的计数率大，而数据显示相反的情况。研究了模型参数对IBEX-Lo通量和两个能量通道通量比的影响。我们发现，最重要的参数，这有一个主要的影响，在两个能量箱的通量的比例，是太阳辐射压力。参数拟合结果表明，当太阳辐射压与太阳引力之比$μ_0$为1.26 $^{+0.06}_{-0.076}$，1 AU处氢的总电离率为$β_{E,0}=3.7^{+0.39}_{-0.35}\times 10^{-7}$ ~s $^{-1}$时，模型结果与实验数据吻合最好。我们发现，$μ_0$的值远大于$μ_0=0.89$，这是从综合太阳莱曼α通量数据的研究期间的值。我们讨论了这些差异的可能原因。

英文摘要：

In this paper, we perform numerical modeling of the interstellar hydrogen fluxes measured by IBEX-Lo during orbit 23 (spring 2009) using a state-of-the-art kinetic model of the interstellar neutral hydrogen distribution in the heliosphere. This model takes into account the temporal and heliolatitudinal variations of the solar parameters as well as non-Maxwellian kinetic properties of the hydrogen distribution due to charge exchange in the heliospheric interface. We found that there is a qualitative difference between the IBEX-Lo data and the modeling results obtained with the three-dimensional, time-dependent model. Namely, the model predicts a larger count rate in energy bin~2 (20-41 eV) than in energy bin~1 (11-21 eV), while the data shows the opposite case. We perform study of the model parameter effects on the IBEX-Lo fluxes and the ratio of fluxes in two energy channels. We shown that the most important parameter, which has a major influence on the ratio of the fluxes in the two energy bins, is the solar radiation pressure. The parameter fitting procedure shows that the best agreement between the model result and the data occurs in the case when the ratio of the solar radiation pressure to the solar gravitation, $μ_0$, is 1.26$^{+0.06}_{-0.076}$, and the total ionization rate of hydrogen at 1 AU is $β_{E,0}=3.7^{+0.39}_{-0.35}\times 10^{-7}$~s$^{-1}$. We have found that the value of $μ_0$ is much larger than $μ_0=0.89$, which is the value derived from the integrated solar Lyman-alpha flux data for the period of time studied. We discuss possible reasons for the differences.

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