A Review of Alfvenic Turbulence in High-Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F18%3A00496115" target="_blank" >RIV/67985815:_____/18:00496115 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1002/2017JA024203" target="_blank" >http://dx.doi.org/10.1002/2017JA024203</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1002/2017JA024203" target="_blank" >10.1002/2017JA024203</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A Review of Alfvenic Turbulence in High-Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

Popis výsledku v původním jazyce

Solar wind turbulence within high-speed streams is reviewed from the point of view of embedded single nonlinear Alfven wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase-steepen, with a right-hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of wave breaking and the latter that of “period doubling.” Interplanetary nonlinear Alfven waves, which are arc polarized, have a similar to 180 degrees foreshortened front and with an elongated trailing edge. Alfven waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable feature of plasma turbulence. Interplanetary Alfven waves are noted to be spherical waves, suggesting the possibility of additional local generation. They kinetically dissipate, forming MDs, indicating that the solar wind is partially “compressive” and static. The similar to 2 MeV protons can nonresonantly interact with MDs leading to rapid cross-field (similar to 5.5% Bohm) diffusion. The possibility of local (similar to 1 AU) generation of Alfven waves may make it difficult to forecast High-Intensity, Long-Duration AE Activity and relativistic magnetospheric electrons with great accuracy. The future Solar Orbiter and Solar Probe Plus missions should be able to not only test these ideas but to also extend our knowledge of plasma turbulence evolution.

Název v anglickém jazyce

A Review of Alfvenic Turbulence in High-Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

Popis výsledku anglicky

Solar wind turbulence within high-speed streams is reviewed from the point of view of embedded single nonlinear Alfven wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase-steepen, with a right-hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of wave breaking and the latter that of “period doubling.” Interplanetary nonlinear Alfven waves, which are arc polarized, have a similar to 180 degrees foreshortened front and with an elongated trailing edge. Alfven waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable feature of plasma turbulence. Interplanetary Alfven waves are noted to be spherical waves, suggesting the possibility of additional local generation. They kinetically dissipate, forming MDs, indicating that the solar wind is partially “compressive” and static. The similar to 2 MeV protons can nonresonantly interact with MDs leading to rapid cross-field (similar to 5.5% Bohm) diffusion. The possibility of local (similar to 1 AU) generation of Alfven waves may make it difficult to forecast High-Intensity, Long-Duration AE Activity and relativistic magnetospheric electrons with great accuracy. The future Solar Orbiter and Solar Probe Plus missions should be able to not only test these ideas but to also extend our knowledge of plasma turbulence evolution.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA15-10057S" target="_blank" >GA15-10057S: Ionty ve slunečním větru: korelace, omezení a kausalita</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

Journal of Geophysical Research: Space Physics

ISSN

2169-9402

e-ISSN

—

Svazek periodika

123

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

35

Strana od-do

2458-2492

Kód UT WoS článku

000433498400001

EID výsledku v databázi Scopus

2-s2.0-85041405230