Radial evolution of nonthermal electron populations in the low-latitude solar wind: Helios, Cluster, and Ulysses Observations

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F09%3A00331561" target="_blank" >RIV/67985815:_____/09:00331561 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378289:_____/09:00331561

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

Radial evolution of nonthermal electron populations in the low-latitude solar wind: Helios, Cluster, and Ulysses Observations

Popis výsledku v původním jazyce

We provide a statistical study of solar wind electron velocity distribution functions (eVDFs) acquired on several spacecraft in low ecliptic latitudes within heliocentric range from 0.3 up to 4 AU. We focus on the non-thermal properties of eVDFs in the slow and fast solar wind regimes. The aim of the present work is to provide an analytical model to fit separately all three components of observed solar wind eVDFs (i.e., the core, the halo, and the strahl) and to study their fractional densities and alsothe non-Maxwellian character of high-energy eVDF tails. Our results indicates that halo and strahl relative densities vary in an opposite way. The relative number of strahl electrons is decreasing with radial distance while the relative number of halo electrons is increasing. The fractional density of the core population remains roughly constant. These findings confirm that there are mechanisms in the solar wind that scatter strahl electrons into the halo.

Název v anglickém jazyce

Radial evolution of nonthermal electron populations in the low-latitude solar wind: Helios, Cluster, and Ulysses Observations

Popis výsledku anglicky

We provide a statistical study of solar wind electron velocity distribution functions (eVDFs) acquired on several spacecraft in low ecliptic latitudes within heliocentric range from 0.3 up to 4 AU. We focus on the non-thermal properties of eVDFs in the slow and fast solar wind regimes. The aim of the present work is to provide an analytical model to fit separately all three components of observed solar wind eVDFs (i.e., the core, the halo, and the strahl) and to study their fractional densities and alsothe non-Maxwellian character of high-energy eVDF tails. Our results indicates that halo and strahl relative densities vary in an opposite way. The relative number of strahl electrons is decreasing with radial distance while the relative number of halo electrons is increasing. The fractional density of the core population remains roughly constant. These findings confirm that there are mechanisms in the solar wind that scatter strahl electrons into the halo.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BL - Fyzika plasmatu a výboje v plynech

OECD FORD obor

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Projekt

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Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2009

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Journal of Geophysical Research

ISSN

0148-0227

e-ISSN

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Svazek periodika

114

Číslo periodika v rámci svazku

-

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

15

Strana od-do

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Kód UT WoS článku

000265932600001

EID výsledku v databázi Scopus

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