Long-term trends of magnetic bright points I. Number of magnetic bright points at disc centre

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00458154" target="_blank" >RIV/67985815:_____/16:00458154 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201525926" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201525926</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201525926" target="_blank" >10.1051/0004-6361/201525926</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Long-term trends of magnetic bright points I. Number of magnetic bright points at disc centre

Popis výsledku v původním jazyce

We study magnetic bright points (MBPs) as proxies for such small-scale, kG solar magnetic fields. This study is based on a homogeneous data set that covers a period of eight years. The number of detected MBPs versus time is analysed to find out if there is an activity cycle for these magnetic features too and, if so, how it is related to the sunspot cycle. After a careful preselection and monthly median filtering of the data, the investigation revealed that the number of MBPs close to the equator is coupled to the global solar cycle but shifted in time by about 2.5 yr. Furthermore, the instantaneous number of detected MBPs depends on the hemisphere, with one hemisphere being more prominent, i.e. showing a higher number of MBPs. After the end of Cycle 23 and at the starting point of Cycle 24, the more active hemisphere changed from south to north. Clear peaks in the detected number of MBPs are found at latitudes of about ±7°, in congruence with the positions of the sunspot belts at the end of the solar cycle.

Název v anglickém jazyce

Long-term trends of magnetic bright points I. Number of magnetic bright points at disc centre

Popis výsledku anglicky

We study magnetic bright points (MBPs) as proxies for such small-scale, kG solar magnetic fields. This study is based on a homogeneous data set that covers a period of eight years. The number of detected MBPs versus time is analysed to find out if there is an activity cycle for these magnetic features too and, if so, how it is related to the sunspot cycle. After a careful preselection and monthly median filtering of the data, the investigation revealed that the number of MBPs close to the equator is coupled to the global solar cycle but shifted in time by about 2.5 yr. Furthermore, the instantaneous number of detected MBPs depends on the hemisphere, with one hemisphere being more prominent, i.e. showing a higher number of MBPs. After the end of Cycle 23 and at the starting point of Cycle 24, the more active hemisphere changed from south to north. Clear peaks in the detected number of MBPs are found at latitudes of about ±7°, in congruence with the positions of the sunspot belts at the end of the solar cycle.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/7AMB14AT022" target="_blank" >7AMB14AT022: Úplný obraz sluneční aktivity na malých měřítkách a jeho důsledky</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

585

Číslo periodika v rámci svazku

January

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

"A39/1"-"A39/10"

Kód UT WoS článku

000369710300046

EID výsledku v databázi Scopus

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