Connection Between Proton Beam and Alpha Core in the Solar Wind

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10423321" target="_blank" >RIV/00216208:11320/20:10423321 - isvavai.cz</a>

Výsledek na webu

<a href="https://www.mff.cuni.cz/veda/konference/wds/proc/pdf20/WDS20_01_f2_Durovcova.pdf" target="_blank" >https://www.mff.cuni.cz/veda/konference/wds/proc/pdf20/WDS20_01_f2_Durovcova.pdf</a>

DOI - Digital Object Identifier

—

Jazyk výsledku

angličtina

Název v původním jazyce

Connection Between Proton Beam and Alpha Core in the Solar Wind

Popis výsledku v původním jazyce

Using the plasma data measured in-situ in the inner heliosphere (Helios 1 and 2), we focus on the proton beam development with an increasing radial distance from the Sun as well as on the connection between the proton beam parameters and the α core properties. We found that the relative content of α core is correlated with the relative proton beam abundance, and this effect is more pronounced in the fast solar wind streams during solar maximum. Since the fast wind is expected to come from distinct source regions, coronal holes, the connection between the α core and proton beam could indicate that the coronal holes are able to produce different types of the fast solar wind streams. On the other hand, in the collisionally old slow solar wind, merging of the proton beam with core is observed. In the parameter space of the α-proton core relative drift and the relative proton beam abundance, we distinguished two regimes and observed transition between them for the intermediate streams. We proposed two different scenarios of how the proton beam could be reduced. First, the protons in the intermediate streams could be heated via the alpha/proton magnetosonic instability and initiate the proton core and beam merging. Second, the proton beam could be reduced in order to balance the total ion momentum in the solar wind frame.

Název v anglickém jazyce

Connection Between Proton Beam and Alpha Core in the Solar Wind

Popis výsledku anglicky

Using the plasma data measured in-situ in the inner heliosphere (Helios 1 and 2), we focus on the proton beam development with an increasing radial distance from the Sun as well as on the connection between the proton beam parameters and the α core properties. We found that the relative content of α core is correlated with the relative proton beam abundance, and this effect is more pronounced in the fast solar wind streams during solar maximum. Since the fast wind is expected to come from distinct source regions, coronal holes, the connection between the α core and proton beam could indicate that the coronal holes are able to produce different types of the fast solar wind streams. On the other hand, in the collisionally old slow solar wind, merging of the proton beam with core is observed. In the parameter space of the α-proton core relative drift and the relative proton beam abundance, we distinguished two regimes and observed transition between them for the intermediate streams. We proposed two different scenarios of how the proton beam could be reduced. First, the protons in the intermediate streams could be heated via the alpha/proton magnetosonic instability and initiate the proton core and beam merging. Second, the proton beam could be reduced in order to balance the total ion momentum in the solar wind frame.

Druh

D - Stať ve sborníku

CEP obor

—

OECD FORD obor

10305 - Fluids and plasma physics (including surface physics)

Projekt

—

Návaznosti

S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název statě ve sborníku

WDS&apos;20 Proceedings of Contributed Papers — Physics

ISBN

978-80-7378-435-5

ISSN

—

e-ISSN

—

Počet stran výsledku

7

Strana od-do

7-13

Název nakladatele

Matfyzpress

Místo vydání

Praha

Místo konání akce

Praha/ZOOM

Datum konání akce

22. 9. 2020

Typ akce podle státní příslušnosti

EUR - Evropská akce

Kód UT WoS článku

—