Dynamic Variations at the Base of the Solar Convection Zone

Howe, R.; Christensen‐Dalsgaard, J.; Hill, F.; Komm, R.; Larsen, Ryan Godsk; Schou, J.; Thompson, M. J.; Toomre, J.

doi:10.1126/science.287.5462.2456

Cited by 438 publications

(337 citation statements)

References 27 publications

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“…32). The torsional oscillations were first discovered on the Sun's surface [129], and then were found in the upper convection zone by helioseismology [130,131]. The depth of these evolving zonal flows is not yet established.…”

Section: Results For Solar Rotationmentioning

confidence: 99%

Advances in Global and Local Helioseismology: An Introductory Review

Kosovichev

2011

The Pulsations of the Sun and the Stars

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Abstract. Helioseismology studies the structure and dynamics of the Sun's interior by observing oscillations on the surface. These studies provide information about the physical processes that control the evolution and magnetic activity of the Sun. In recent years, helioseismology has made substantial progress towards the understanding of the physics of solar oscillations and the physical processes inside the Sun, thanks to observational, theoretical and modeling efforts. In addition to the global seismology of the Sun based on measurements of global oscillation modes, a new field of local helioseismology, which studies oscillation travel times and local frequency shifts, has been developed. It is capable of providing 3D images of the subsurface structures and flows. The basic principles, recent advances and perspectives of global and local helioseismology are reviewed in this article.

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Section: Results For Solar Rotationmentioning

confidence: 99%

Advances in Global and Local Helioseismology: An Introductory Review

Kosovichev

2011

The Pulsations of the Sun and the Stars

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“…The presence of the ∼1.3-year period within the active belt allows the conjecture that the ALs may be connected to a source region close to the tachocline zone. This implication is based on the results by Howe et al (2000), who found the same period of the radial torsional oscillation at the tachocline zone during the period between 1995 and 2000 and by Bigazzi & Ruzmaikin (2004), who argued that the non-axisymmetry of the solar dynamo could only remain at the bottom of the convective zone.…”

Section: Temporal Properties Of Solar Flares Near Almentioning

confidence: 91%

“…The half width of this AL was about 30°, a flip-flop event was identified, but the most interesting result was that the flux emergence exhibited a 1.3-year periodicity within the active longitudinal domain while this period was absent from of this domain. This raised the possible interpretation that the active regions emerging within the AL are anchored at the bottom of the convective zone where this period was also detected by Howe et al (2000) and the rest of the active regions emerge from higher layers.…”

Section: Introductionmentioning

confidence: 99%

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Active Longitude and Solar Flare Occurrences

Gyenge

Ludmány

Baranyi

2016

ApJ

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The aim of the present work is to specify the spatio-temporal characteristics of flare activity observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Geostationary Operational Environmental Satellite (GOES) in connection with the behavior of the longitudinal domain of enhanced sunspot activity known as active longitude (AL). By using our method developed for this purpose, we identified the AL in every Carrington Rotation provided by the Debrecen Photoheliographic Data. The spatial probability of flare occurrence has been estimated depending on the longitudinal distance from AL in the northern and southern hemispheres separately. We have found that more than 60% of the RHESSI and GOES flares is located within 36   from the AL. Hence, the most flare-productive active regions tend to be located in or close to the active longitudinal belt. This observed feature may allow for the prediction of the geo-effective position of the domain of enhanced flaring probability. Furthermore, we studied the temporal properties of flare occurrence near the AL and several significant fluctuations were found. More precisely, the results of the method are the following fluctuations: 0.8, 1.3, and 1.8 years. These temporal and spatial properties of the solar flare occurrence within the active longitudinal belts could provide us with an enhanced solar flare forecasting opportunity.

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“…Komm et al (2002Komm et al ( , 2003Komm et al ( , 2004 and Howe et al (2000) found out that the 1.3-year periodicity at the base of the convection zone is most pronounced in the solar rotation rate at the equator of the tachocline. The 1.3-year variation of the solar rotation rate in the vicinity of the tachocline was also revealed by Schou (2003).…”

Section: Variation Of Solar Indices With a Period Of 13 Yearsmentioning

confidence: 99%

Large-scale patterns and ‘active longitudes’

Обридко¹

2009

Proc. IAU

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Abstract. The following aspects of the physics of large-scale solar magnetic fields are discussed: structure of large-scale fields (LSF) and connection with local fields; dynamo and origin of LSF; LSF cycle variation; meridional circulation and LSF; rotation of LSF; fine structure of the field in quiet regions and the concept of the pebble-shaped field; active longitudes, their manifestation in various solar indices, and dependence on the power of solar activity.

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Dynamic Variations at the Base of the Solar Convection Zone

Cited by 438 publications

References 27 publications

Advances in Global and Local Helioseismology: An Introductory Review

Advances in Global and Local Helioseismology: An Introductory Review

Active Longitude and Solar Flare Occurrences

Large-scale patterns and ‘active longitudes’

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