Understanding the Sub-surface Dynamics of Sunspots Post Emergence

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F19%3A10407007" target="_blank" >RIV/00216208:11320/19:10407007 - isvavai.cz</a>

Výsledek na webu

<a href="https://www.mff.cuni.cz/veda/konference/wds/proc/pdf19/WDS19_24_f1_Pillai.pdf" target="_blank" >https://www.mff.cuni.cz/veda/konference/wds/proc/pdf19/WDS19_24_f1_Pillai.pdf</a>

DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

Understanding the Sub-surface Dynamics of Sunspots Post Emergence

Popis výsledku v původním jazyce

This paper presents the preliminary results for the dynamical disconnection of sunspot phenomenon. We obtain our results by doing actual calculation of parameters like the tilt angle of sunspot and the longitudinal drift when compared to the results based on predictions. These predictions are obtained from models supporting the disconnection phenomenon. We aim to provide evidence to support the dynamical disconnection process of sunspot. The previous model-based results were obtained using low resolution data from the Michelson Doppler Imager instrument in Solar and Heliospheric Observatory (SOHO/MDI). Due to the low resolution of the data, there was an inconsistency in corelating the strong magnetic field of the sunspot with the dynamical disconnection process. Thus a new approach to revisit the entire dynamical disconnection phenomenon using the Heliographic Magnetic Imager instrument in Solar Dynamic Observatory (HMI/SDO) data is needed. The source will yield to high resolution data cubes which becomes easy to distinguish between the magnetic field structures of various active regions (AR), sunspot and its flux tube. Our work is an extension of the work done by Svanda v et al. using SOHO/MDI data.

Název v anglickém jazyce

Understanding the Sub-surface Dynamics of Sunspots Post Emergence

Popis výsledku anglicky

This paper presents the preliminary results for the dynamical disconnection of sunspot phenomenon. We obtain our results by doing actual calculation of parameters like the tilt angle of sunspot and the longitudinal drift when compared to the results based on predictions. These predictions are obtained from models supporting the disconnection phenomenon. We aim to provide evidence to support the dynamical disconnection process of sunspot. The previous model-based results were obtained using low resolution data from the Michelson Doppler Imager instrument in Solar and Heliospheric Observatory (SOHO/MDI). Due to the low resolution of the data, there was an inconsistency in corelating the strong magnetic field of the sunspot with the dynamical disconnection process. Thus a new approach to revisit the entire dynamical disconnection phenomenon using the Heliographic Magnetic Imager instrument in Solar Dynamic Observatory (HMI/SDO) data is needed. The source will yield to high resolution data cubes which becomes easy to distinguish between the magnetic field structures of various active regions (AR), sunspot and its flux tube. Our work is an extension of the work done by Svanda v et al. using SOHO/MDI data.

Druh

D - Stať ve sborníku

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

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Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2019

Kód důvěrnosti údajů

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

Název statě ve sborníku

WDS&apos;19 Proceedings of Contributed Papers — Physics

ISBN

978-80-7378-409-6

ISSN

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e-ISSN

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Počet stran výsledku

7

Strana od-do

138-144

Název nakladatele

Matfyzpress

Místo vydání

Praha

Místo konání akce

Praha

Datum konání akce

4. 6. 2019

Typ akce podle státní příslušnosti

EUR - Evropská akce

Kód UT WoS článku

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