Imperial College London
Portrait Picture

Professor Jonathan P. Eastwood

Faculty of Natural Sciences, Department of Physics

Professor of Space Physics
 
 
 
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Contact

 

jonathan.eastwood Website

 
 
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Assistant

 

Mr Luke Kratzmann +44 (0)20 7594 7770

 
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Location

 

Huxley BuildingSouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Krupar:2018:1538-4357/aab60f,
author = {Krupar, V and Maksimovic, M and Kontar, EP and Zaslavsky, A and Santolik, O and Soucek, J and Kruparova, O and Eastwood, JP and Szabo, A},
doi = {1538-4357/aab60f},
journal = {ASTROPHYSICAL JOURNAL},
title = {Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind},
url = {http://dx.doi.org/10.3847/1538-4357/aab60f},
volume = {857},
year = {2018}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - Type III bursts are generated by fast electron beams originated from magnetic reconnection sites of solar flares. As propagation of radio waves in the interplanetary medium is strongly affected by random electron density fluctuations, type III bursts provide us with a unique diagnostic tool for solar wind remote plasma measurements. Here, we performed a statistical survey of 152 simple and isolated type III bursts observed by the twin-spacecraft Solar TErrestrial RElations Observatory mission. We investigated their time–frequency profiles in order to retrieve decay times as a function of frequency. Next, we performed Monte Carlo simulations to study the role of scattering due to random electron density fluctuations on time–frequency profiles of radio emissions generated in the interplanetary medium. For simplification, we assumed the presence of isotropic electron density fluctuations described by a power law with the Kolmogorov spectral index. Decay times obtained from observations and simulations were compared. We found that the characteristic exponential decay profile of type III bursts can be explained by the scattering of the fundamental component between the source and the observer despite restrictive assumptions included in the Monte Carlo simulation algorithm. Our results suggest that relative electron density fluctuations $\langle \delta {n}_{{\rm{e}}}\rangle /{n}_{{\rm{e}}}$ in the solar wind are 0.06–0.07 over wide range of heliospheric distances.
AU  - Krupar,V
AU  - Maksimovic,M
AU  - Kontar,EP
AU  - Zaslavsky,A
AU  - Santolik,O
AU  - Soucek,J
AU  - Kruparova,O
AU  - Eastwood,JP
AU  - Szabo,A
DO  - 1538-4357/aab60f
PY  - 2018///
SN  - 0004-637X
TI  - Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind
T2  - ASTROPHYSICAL JOURNAL
UR  - http://dx.doi.org/10.3847/1538-4357/aab60f
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000430336500005&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/59702
VL  - 857
ER  -
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