Migration and Extension of Solar Active Longitudinal Zones

Gyenge, N.; Baranyi, T.; Ludmány, A.

doi:10.1007/s11207-013-0424-3

Cited by 20 publications

(17 citation statements)

References 29 publications

(46 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The shape of migration clearly follows parabolicshaped path as found in several earlier studies ( 2011a; Usoskin et al 2007Usoskin et al , 2005Gyenge et al 2014).…”

Section: Solar Non-axisymmetric Activitysupporting

confidence: 84%

See 1 more Smart Citation

Active Longitude and Coronal Mass Ejection Occurrences

Gyenge

Singh

Kiss

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

The spatial inhomogeneity of the distribution of coronal mass ejection (CME) occurrences in the solar atmosphere could provide a tool to estimate the longitudinal position of the most probable CME-capable active regions in the Sun. The anomaly in the longitudinal distribution of active regions themselves is often referred to as active longitude (AL). In order to reveal the connection between the AL and CME spatial occurrences, here we investigate the morphological properties of active regions. The first morphological property studied is the separateness parameter, which is able to characterise the probability of the occurrence of an energetic event, such as solar flare or CME. The second morphological property is the sunspot tilt angle. The tilt angle of sunspot groups allows us to estimate the helicity of active regions. The increased helicity leads to a more complex built-up of the magnetic structure and also can cause CME eruption. We found that the most complex active regions appear near to the AL and the AL itself is associated with the most tilted active regions. Therefore, the number of CME occurrences is higher within the AL. The origin of the fast CMEs is also found to be associated with this region. We concluded that the source of the most probably CME-capable active regions is at the AL. By applying this method we can potentially forecast a flare and/or CME source several Carrington rotations in advance. This finding also provides new information for solar dynamo modelling.

show abstract

“…The shape of migration clearly follows parabolicshaped path as found in several earlier studies ( 2011a; Usoskin et al 2007Usoskin et al , 2005Gyenge et al 2014).…”

Section: Solar Non-axisymmetric Activitysupporting

confidence: 84%

“…The role of differential rotation is also controversy. Various studies concluded that the differential rotation is not the reason of the migration of the AL (Balthasar 2007;Juckett 2006Juckett , 2007Gyenge et al 2014).…”

Section: Solar Non-axisymmetric Activitymentioning

confidence: 99%

Active Longitude and Coronal Mass Ejection Occurrences

Gyenge

Singh

Kiss

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Follow-up studies concerning the preferred locations (longitudes) of sunspot formation delivered inconsistent and partly contradictory results. Even today, the possible number, migration, life times, longterm behavior and the particular method to track them remain a subject of debate (see Berdyugina and Usoskin 2003;Usoskin et al 2005;Pelt et al 2006;Usoskin et al 2007;Weber et al 2013;Gyenge et al 2014). …”

Section: Cyclic Changes Of the Coronal Magnetic Fieldmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

176

125

View full text Add to dashboard Cite

This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

show abstract

“…The long homogeneous series of sunspot data is indispensable for studies of long-term processes. This has been exploited by Gyenge, Baranyi, and Ludmány (2014) in tracking the migration of solar active longitudes. After comparing the positions of flares and active longitudes, Gyenge, Ludmány, and Baranyi (2016) showed that the most flare-productive active regions tend to be located in or close to the active longitudinal belt.…”

Section: Examples For the Exploitation Of The Databasesmentioning

confidence: 99%

On-line Tools for Solar Data Compiled at the Debrecen Observatory and Their Extensions with the Greenwich Sunspot Data

2016

Self Cite

View full text Add to dashboard Cite

The primary task of the Debrecen Heliophysical Observatory (DHO) has been the most detailed, reliable, and precise documentation of the solar photospheric activity since 1958. This long-term effort resulted in various solar catalogs based on ground-based and space-borne observations. A series of sunspot databases and on-line tools were compiled at DHO: the Debrecen Photoheliographic Data (DPD, 1974-), the dataset based on the Michelson Doppler Imager (MDI) of the Solar and Heliospheric Observatory (SOHO) called SOHO/MDI-Debrecen Data (SDD, 1996(SDD, -2010, and the dataset based on the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory (SDO) called SDO/HMI-Debrecen Data (HMIDD, 2010-). User-friendly web-presentations and on-line tools were developed to visualize and search data. As a last step of compilation, the revised version of Greenwich Photoheliographic Results (GPR, 1874(GPR, -1976 catalog was converted to DPD format, and a homogeneous sunspot database covering more than 140 years was created. The database of images for the GPR era was completed with the full-disc drawings of the Hungarian historical observatoriesÓgyalla and Kalocsa and with the polarity drawings of Mount Wilson Observatory. We describe the main characteristics of the available data and on-line tools.

show abstract

Migration and Extension of Solar Active Longitudinal Zones

Cited by 20 publications

References 29 publications

Active Longitude and Coronal Mass Ejection Occurrences

Active Longitude and Coronal Mass Ejection Occurrences

The magnetic field in the solar atmosphere

On-line Tools for Solar Data Compiled at the Debrecen Observatory and Their Extensions with the Greenwich Sunspot Data

Contact Info

Product

Resources

About