P-mode induced convective collapse in vertical expanding magnetic flux tubes?

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00485019" target="_blank" >RIV/67985815:_____/17:00485019 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1017/S174392131700401X" target="_blank" >http://dx.doi.org/10.1017/S174392131700401X</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/S174392131700401X" target="_blank" >10.1017/S174392131700401X</a>

Jazyk výsledku

angličtina

Název v původním jazyce

P-mode induced convective collapse in vertical expanding magnetic flux tubes?

Popis výsledku v původním jazyce

Small-scale kG strong magnetic field elements in the solar photosphere are often identified as so-called magnetic bright points (MBPs). In principle these MBPs represent the cross-section of a vertical, strong, magnetic flux tube which is expanding with height in thensolar atmosphere. As these magnetic elements re present possible MHD wave guides, a significant interest has been already paid to them from the viewpoint of observations and simulations. In this work we would like to shed more light on a possible scenario for the creation of such strong magnetic field concentrations. The accepted standard scenario involves the convective collapse process. In this ongoing work we will show indications that this convective collapse process maybecome triggered by sufficiently strong pressure disturbances. However, it is highly unlikely that p-mode waves can be of such a strength.

Název v anglickém jazyce

P-mode induced convective collapse in vertical expanding magnetic flux tubes?

Popis výsledku anglicky

Small-scale kG strong magnetic field elements in the solar photosphere are often identified as so-called magnetic bright points (MBPs). In principle these MBPs represent the cross-section of a vertical, strong, magnetic flux tube which is expanding with height in thensolar atmosphere. As these magnetic elements re present possible MHD wave guides, a significant interest has been already paid to them from the viewpoint of observations and simulations. In this work we would like to shed more light on a possible scenario for the creation of such strong magnetic field concentrations. The accepted standard scenario involves the convective collapse process. In this ongoing work we will show indications that this convective collapse process maybecome triggered by sufficiently strong pressure disturbances. However, it is highly unlikely that p-mode waves can be of such a strength.

Druh

D - Stať ve sborníku

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název statě ve sborníku

Fine Structure and Dynamics of the Solar Atmosphere

ISBN

9781107170049

ISSN

1743-9213

e-ISSN

—

Počet stran výsledku

8

Strana od-do

86-93

Název nakladatele

Cambridge University Press

Místo vydání

Cambridge

Místo konání akce

Cartagena de Indias

Datum konání akce

9. 10. 2016

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

000455235900014