New Insights on Penumbra Magneto-Convection

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F19%3A00552737" target="_blank" >RIV/67985815:_____/19:00552737 - isvavai.cz</a>

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

New Insights on Penumbra Magneto-Convection

Popis výsledku v původním jazyce

In July 2009, we observed the early stages of the NOAA 11024 AR leading sunspot while developing its penumbra. The spectro-polarimetric dataset lead us to new observational findings. In this contribution, we put into context our and other authors' results to draw the overall picture of sunspot formation. Most important, the comparison on the properties of different types of penumbrae lead us to the conclusion that the formation of penumbrae is not just one mechanism. While the sole cause necessary for penumbral magneto-convection is a stably inclined magnetic field, observations show that inclined fields can be caused by flux emergence, to form orphan penumbrae, or by field lines transported down from upper photospheric layers, to form sunspot penumbra. This conclusion, together with the recent findings by Jurčák and collaborators on a canonical value of the vertical component of the magnetic field blocking the action of penumbral magneto-convection in umbral areas, is a crucial step forward towards the understanding of the coupling of solar plasmas and magnetic fields in penumbral atmospheres.

Název v anglickém jazyce

New Insights on Penumbra Magneto-Convection

Popis výsledku anglicky

In July 2009, we observed the early stages of the NOAA 11024 AR leading sunspot while developing its penumbra. The spectro-polarimetric dataset lead us to new observational findings. In this contribution, we put into context our and other authors' results to draw the overall picture of sunspot formation. Most important, the comparison on the properties of different types of penumbrae lead us to the conclusion that the formation of penumbrae is not just one mechanism. While the sole cause necessary for penumbral magneto-convection is a stably inclined magnetic field, observations show that inclined fields can be caused by flux emergence, to form orphan penumbrae, or by field lines transported down from upper photospheric layers, to form sunspot penumbra. This conclusion, together with the recent findings by Jurčák and collaborators on a canonical value of the vertical component of the magnetic field blocking the action of penumbral magneto-convection in umbral areas, is a crucial step forward towards the understanding of the coupling of solar plasmas and magnetic fields in penumbral atmospheres.

Druh

D - Stať ve sborníku

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA14-04338S" target="_blank" >GA14-04338S: Fyzikální podstata slunečních skvrn</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2019

Kód důvěrnosti údajů

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

Název statě ve sborníku

Solar Polarization Workshop 8

ISBN

978-1-58381-939-5

ISSN

1050-3390

e-ISSN

1050-3390

Počet stran výsledku

9

Strana od-do

261-269

Název nakladatele

Astronomical Society of the Pacific

Místo vydání

San Francisco

Místo konání akce

Florence

Datum konání akce

12. 9. 2016

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

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