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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 &lt;delta n(e)&gt;/n(e) in the solar wind are 0.06-0.07 over wide range of heliospheric distances.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • 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

  • 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

  • UT code for WoS article

    000430336500005

  • EID of the result in the Scopus database

    2-s2.0-85046377082