Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10389417" target="_blank" >RIV/00216208:11320/18:10389417 - isvavai.cz</a>
Alternative codes found
RIV/68378289:_____/18:00489280
Result on the web
<a href="https://doi.org/10.3847/1538-4357/aab60f" target="_blank" >https://doi.org/10.3847/1538-4357/aab60f</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/aab60f" target="_blank" >10.3847/1538-4357/aab60f</a>
Alternative languages
Result language
angličtina
Original language name
Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind
Original language description
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 <delta n(e)>/n(e) in the solar wind are 0.06-0.07 over wide range of heliospheric distances.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10305 - Fluids and plasma physics (including surface physics)
Result continuities
Project
Result was created during the realization of more than one project. More information in the Projects tab.
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2018
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
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Volume of the periodical
857
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
7
Pages from-to
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UT code for WoS article
000430336500005
EID of the result in the Scopus database
2-s2.0-85046377082