Observation and Modeling of Small Spatial Structures of Solar Radio Noise Storms Using the uGMRT

IF 2.4 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Surajit Mondal, Peijin Zhang, Devojyoti Kansabanik, Divya Oberoi, Gillian Pearce
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Abstract

One of the most commonly observed solar radio sources in the metric and decametric wavelengths is the solar noise storm. These are generally associated with active regions and are believed to be powered by the plasma emission mechanism. Since plasma emission is emitted primarily at the fundamental and harmonic of the local plasma frequency, it is significantly affected by density inhomogeneities in the solar corona. The source can become significantly scatter-broadened due to the multi-path propagation caused by refraction from the density inhomogeneities. Past observational and theoretical estimates suggest some minimum observable source size in the solar corona. The details of this limit, however, depend on the modeling approach and details of the coronal turbulence model chosen. Hence pushing the minimum observable source size to smaller values can help constrain the plasma environment of the observed sources. In this work, we for the first time, use data from the upgraded Giant Metrewave Radio Telescope in the 250 – 500 MHz band, to determine multiple instances of very small-scale structures in the noise storms. We also find that these structures are stable over timescales of 15 – 30 minutes. By comparing the past observations of type III radio bursts and noise storms, we hypothesize that the primary reason behind the detection of these small sources in noise storm is due to the local environment of the noise storm. We also build an illustrative model and propose some conditions under which the minimum observable source size predicted by theoretical models, can be lowered significantly.

利用uGMRT观测和模拟太阳射电噪声风暴的小空间结构
在公制和十米制波长中最常观测到的太阳射电源之一是太阳噪声风暴。这些通常与活跃区域有关,并被认为是由等离子体发射机制提供动力的。由于等离子体发射主要是在局部等离子体频率的基频和谐波上发射的,因此它受到日冕密度不均匀性的显著影响。由于密度不均匀性引起的折射引起的多径传播会使光源的散射明显展宽。过去的观测和理论估计表明,在日冕中存在可观测到的最小辐射源大小。然而,这个极限的细节取决于所选择的建模方法和日冕湍流模型的细节。因此,将最小可观测源尺寸推到更小的值可以帮助约束被观测源的等离子体环境。在这项工作中,我们首次使用升级后的巨型米波射电望远镜在250 - 500兆赫波段的数据,来确定噪声风暴中非常小尺度结构的多个实例。我们还发现这些结构在15 - 30分钟的时间尺度上是稳定的。通过对比以往对III型射电暴和噪声风暴的观测,我们假设在噪声风暴中探测到这些小辐射源的主要原因是由于噪声风暴的局部环境。我们还建立了一个说明性模型,并提出了理论模型预测的最小可观测源尺寸可以显著降低的一些条件。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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来源期刊
Solar Physics
Solar Physics 地学天文-天文与天体物理
CiteScore
5.10
自引率
17.90%
发文量
146
审稿时长
1 months
期刊介绍: Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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