Electron beam propagation and radio-wave scattering in the inner heliosphere using five spacecraft

IF 5.4 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
L. A. Cañizares, S. T. Badman, N. Chrysaphi, S. Bhunia, B. Sánchez-Cano, S. A. Maloney, P. T. Gallagher
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Abstract

Context. Solar energetic particles such as electrons can be accelerated to mildly relativistic velocities in the solar corona. These electrons travel through the turbulent corona, generating radio waves, which are then severely affected by scattering.Aims. The physical interpretation of the discrepancies between the actual and observed radio sources is still subject to debate. We used radio emission observed by an unprecedented total of five spacecraft to track the path of radio sources from the low corona to the inner heliosphere (15–75 R or 0.07–0.35 au generated during a solar event on 4 December 2021.Methods. We used the Bayesian multilateration technique known as BELLA to track the apparent path of radio sources observed by Parker Solar Probe, STEREO A, Wind, Solar Orbiter, and Mars Express. To validate the accuracy of the tracked path, we used Nançay Radioheliograph interferometric imaging at 150 MHz, which was found to agree with the estimated footpoints predicted by BELLA. We further validated our results using ACE in situ measurements.Results. We find that the apparent radio sources followed the path of an Archimedean Parker spiral, with an associated solar wind velocity of approximately 493 km s−1 (consistent with the corresponding speed observed at 1 au at the relevant longitude), and connected to the solar surface at 75° longitude east. Finally, we made quantitative estimates of the scattering of radio waves, which we found to be in good agreement with contemporary models of scattering in which the radio waves primarily propagate along the local Parker spiral.Conclusions. This work shows conclusive evidence that the cause of the widely observed ‘higher-than-expected’ electron densities at interplanetary distances is due to radio-wave scattering, and provides a more detailed understanding of the propagation of radio waves emitted near the local plasma frequency in turbulent astrophysical plasmas.
利用五个航天器在日光层内部进行电子束传播和无线电波散射
背景。电子等太阳高能粒子可在日冕中加速到轻度相对论速度。这些电子在湍流日冕中传播,产生无线电波,然后受到散射的严重影响。关于实际射电源与观测到的射电源之间差异的物理解释仍存在争议。我们利用史无前例的五艘航天器观测到的射电辐射来追踪 2021 年 12 月 4 日太阳活动期间射电源从低日冕到内日光层(15-75 R⊙ 或 0.07-0.35 au)的路径。我们使用被称为 BELLA 的贝叶斯多射影技术来跟踪帕克太阳探测器、STEREO A、Wind、太阳轨道器和火星快车观测到的射电源的视路径。为了验证跟踪路径的准确性,我们使用了 150 MHz 的 Nançay 射电日像仪干涉成像,结果发现与 BELLA 预测的估计脚点一致。我们还利用 ACE 实地测量进一步验证了我们的结果。我们发现,视射电源沿着阿基米德帕克螺旋的路径移动,相关太阳风速度约为 493 km s-1(与在相关经度 1 au 处观测到的相应速度一致),并在东经 75° 处与太阳表面相连。最后,我们对无线电波的散射进行了定量估算,发现其与当代的散射模型十分吻合,在当代模型中,无线电波主要沿当地帕克螺旋线传播。这项工作提供了确凿的证据,证明在行星际距离上被广泛观测到的 "高于预期 "的电子密度是由无线电波散射引起的,并提供了对湍流天体物理等离子体中靠近本地等离子体频率发射的无线电波传播的更详细的了解。
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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