Three-dimensional structure of a sunspot light bridge

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00470619" target="_blank" >RIV/67985815:_____/16:00470619 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/16:00488879

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201629586" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201629586</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201629586" target="_blank" >10.1051/0004-6361/201629586</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Three-dimensional structure of a sunspot light bridge

Popis výsledku v původním jazyce

Active regions are the most prominent manifestations of solar magnetic fields their generation and dissipation are fundamental problems in solar physics. Light bridges are commonly present during sunspot decay, but a comprehensive picture of their role in the removal of the photospheric magnetic field is still lacking. We study the three-dimensional configuration of a sunspot, and in particular, its light bridge, during one of the last stages of its decay.The sunspot shows a light bridge with penumbral continuum intensity that separates the central umbra from a smaller umbra. We find that in this region the magnetic field lines form a canopy with lower magnetic field strength in the inner part. The photospheric light bridge is dominated by gas pressure (high-beta), as opposed to the surrounding umbra, where the magnetic pressure is higher. A convective flow is observed in the light bridge. This flow is able to bend the magnetic field lines and to produce field reversals. The field lines merge above the light bridge and become as vertical and strong as in the surrounding umbra. We conclude that this occurs because two highly magnetized regions approach each other during the sunspot evolution.

Název v anglickém jazyce

Three-dimensional structure of a sunspot light bridge

Popis výsledku anglicky

Active regions are the most prominent manifestations of solar magnetic fields their generation and dissipation are fundamental problems in solar physics. Light bridges are commonly present during sunspot decay, but a comprehensive picture of their role in the removal of the photospheric magnetic field is still lacking. We study the three-dimensional configuration of a sunspot, and in particular, its light bridge, during one of the last stages of its decay.The sunspot shows a light bridge with penumbral continuum intensity that separates the central umbra from a smaller umbra. We find that in this region the magnetic field lines form a canopy with lower magnetic field strength in the inner part. The photospheric light bridge is dominated by gas pressure (high-beta), as opposed to the surrounding umbra, where the magnetic pressure is higher. A convective flow is observed in the light bridge. This flow is able to bend the magnetic field lines and to produce field reversals. The field lines merge above the light bridge and become as vertical and strong as in the surrounding umbra. We conclude that this occurs because two highly magnetized regions approach each other during the sunspot 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/7E13003" target="_blank" >7E13003: High-Resolution Solar Physics Network</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

596

Číslo periodika v rámci svazku

December

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

13

Strana od-do

"A59/1"-"A59/13"

Kód UT WoS článku

000390797900111

EID výsledku v databázi Scopus

2-s2.0-85002658883