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Detecting the oscillation and propagation of the nascent dynamic solar wind structure at 2.6 solar radii using VLBI radio telescopes

Citation

Ma, M and Molera Calves, G and Cimo, G and Xiong, M and Li, P and Kong, J and Zhang, P and He, J and Liu, L and Kummamuru, P and Hou, C and Edwards, J and Liu, Q and Chen, Z and Chu, Z and Wu, D and Zhao, X and Wang, Z and Han, S and Zhi, Q and Liu, Y and Quick, J and Gonzalez, J and Miro, CG and Kharinov, M and Mikhailov, A and Neidhardt, A and Venturi, T and Morsiani, M and Maccaferri, G and Xia, B and Zhang, H and Hao, L, Detecting the oscillation and propagation of the nascent dynamic solar wind structure at 2.6 solar radii using VLBI radio telescopes, The Astrophysical Journal Letters, 940, (2) Article 32. ISSN 2041-8213 (2022) [Refereed Article]


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Copyright Statement

P{ublished with a cc logo cc pd CC0 1.0 Universal (CC0 1.0) Public Domain Dedication. (https://creativecommons.org/publicdomain/zero/1.0/)

Official URL: https://iopscience.iop.org/journal/2041-8205

DOI: doi:10.3847/2041-8213/ac96e7

Abstract

Probing the solar corona is crucial to study the coronal heating and solar wind acceleration. However, the transient and inhomogeneous solar wind flows carry large-amplitude inherent Alfven waves and turbulence, which make detection more difficult. We report the oscillation and propagation of the solar wind at 2.6 solar radii (Rs) by observation of China Tianwen and ESA Mars Express with radio telescopes. The observations were carried out on Oct.9 2021, when one coronal mass ejection (CME) passed across the ray paths of the telescope beams. We obtain the frequency fluctuations (FF) of the spacecraft signals from each individual telescope. Firstly, we visually identify the drift of the frequency spikes at a high spatial resolution of thousands of kilometers along the projected baselines. They are used as traces to estimate the solar wind velocity. Then we perform the cross-correlation analysis on the time series of FF from different telescopes. The velocity variations of solar wind structure along radial and tangential directions during the CME passage are obtained. The oscillation of tangential velocity confirms the detection of streamer wave. Moreover, at the tail of the CME, we detect the propagation of an accelerating fast field-aligned density structure indicating the presence of magnetohydrodynamic waves. This study confirm that the ground station-pairs are able to form particular spatial projection baselines with high resolution and sensitivity to study the detailed propagation of the nascent dynamic solar wind structure.

Item Details

Item Type:Refereed Article
Keywords:VLBI, space craft, radio telescopes, Mars Express, solar wind
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Solar physics
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Molera Calves, G (Dr Guifre Molera Calves)
UTAS Author:Kummamuru, P (Mr Pradyumna Kummamuru)
UTAS Author:Edwards, J (Mr Jasper Edwards)
ID Code:154106
Year Published:2022
Deposited By:Physics
Deposited On:2022-10-28
Last Modified:2023-01-13
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