Orphan penumbrae: Submerging horizontal fields
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F14%3A00429420" target="_blank" >RIV/67985815:_____/14:00429420 - isvavai.cz</a>
Výsledek na webu
<a href="http://dx.doi.org/10.1051/0004-6361/201322340" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201322340</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/201322340" target="_blank" >10.1051/0004-6361/201322340</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
Orphan penumbrae: Submerging horizontal fields
Popis výsledku v původním jazyce
We investigate the properties of orphan penumbrae, which are photospheric filamentary structures observed in active regions near polarity inversion lines that resemble the penumbra of regular sunspots but are not connected to any umbra. Orphan penumbraeform between regions of opposite polarity in places with horizontal magnetic fields. Their magnetic configuration is that of Omega-shaped flux ropes. In the two cases studied here, the opposite-polarity regions approach each other with time and the wholestructure submerges as the penumbral filaments disappear. Orphan penumbrae are very similar to regular penumbrae, including the existence of strong gas flows. Therefore, they could have a similar origin. The main difference between them is the absence of a "background" magnetic field in orphan penumbrae. This could explain most of the observed differences. The fast flows we detect in orphan penumbrae may be caused by the siphon flow mechanism. Based on the similarities between orphan an
Název v anglickém jazyce
Orphan penumbrae: Submerging horizontal fields
Popis výsledku anglicky
We investigate the properties of orphan penumbrae, which are photospheric filamentary structures observed in active regions near polarity inversion lines that resemble the penumbra of regular sunspots but are not connected to any umbra. Orphan penumbraeform between regions of opposite polarity in places with horizontal magnetic fields. Their magnetic configuration is that of Omega-shaped flux ropes. In the two cases studied here, the opposite-polarity regions approach each other with time and the wholestructure submerges as the penumbral filaments disappear. Orphan penumbrae are very similar to regular penumbrae, including the existence of strong gas flows. Therefore, they could have a similar origin. The main difference between them is the absence of a "background" magnetic field in orphan penumbrae. This could explain most of the observed differences. The fast flows we detect in orphan penumbrae may be caused by the siphon flow mechanism. Based on the similarities between orphan an
Klasifikace
Druh
J<sub>x</sub> - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)
CEP obor
BN - Astronomie a nebeská mechanika, astrofyzika
OECD FORD obor
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Návaznosti výsledku
Projekt
<a href="/cs/project/GAP209%2F12%2F0287" target="_blank" >GAP209/12/0287: Spektropolarimetrická analýza sluneční fotosféry</a><br>
Návaznosti
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Ostatní
Rok uplatnění
2014
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Astronomy & Astrophysics
ISSN
0004-6361
e-ISSN
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Svazek periodika
564
Číslo periodika v rámci svazku
April
Stát vydavatele periodika
FR - Francouzská republika
Počet stran výsledku
15
Strana od-do
"A91/1"-"A91/15"
Kód UT WoS článku
000334671000091
EID výsledku v databázi Scopus
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