An Optimization Principle for Computing Stationary MHD Equilibria with Solar Wind Flow

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00538198" target="_blank" >RIV/67985815:_____/20:00538198 - isvavai.cz</a>

Výsledek na webu

<a href="http://hdl.handle.net/11104/0316020" target="_blank" >http://hdl.handle.net/11104/0316020</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1007/s11207-020-01719-8" target="_blank" >10.1007/s11207-020-01719-8</a>

Jazyk výsledku

angličtina

Název v původním jazyce

An Optimization Principle for Computing Stationary MHD Equilibria with Solar Wind Flow

Popis výsledku v původním jazyce

In this work we describe a numerical optimization method for computing stationary MHD equilibria. The newly developed code is based on a nonlinear force-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasma beta and Alfven Mach number M-A are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where beta and M-A are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows for the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magnetostatic models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe.

Název v anglickém jazyce

An Optimization Principle for Computing Stationary MHD Equilibria with Solar Wind Flow

Popis výsledku anglicky

In this work we describe a numerical optimization method for computing stationary MHD equilibria. The newly developed code is based on a nonlinear force-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasma beta and Alfven Mach number M-A are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where beta and M-A are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows for the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magnetostatic models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

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 periodika

Solar Physics

ISSN

1573-093X

e-ISSN

—

Svazek periodika

295

Číslo periodika v rámci svazku

10

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

14

Strana od-do

145

Kód UT WoS článku

000589557800001

EID výsledku v databázi Scopus

2-s2.0-85094652525