Differential Rotation and Dynamics of the Solar Interior

Thompson, M. J.; Toomre, J.; Anderson, E.; Antia, H. M.; Berthomieu, G.; Burtonclay, D.; Chitre, S. M.; Christensen‐Dalsgaard, J.; Corbard, T.; DeRosa, Marc L.; Genovese, Christopher R.; Gough, D. O.; Haber, D. A.; Harvey, J. W.; Hill, F.; Howe, R.; Korzennik, S. G.; Kosovichev, A. G.; Leibacher, J. W.; Pijpers, F. P.; Provost, J.; Rhodes, E. J.; Schou, J.; Sekii, T.; Stark, Philip B.; Wilson, P. R.

doi:10.1126/science.272.5266.1300

Cited by 373 publications

(237 citation statements)

References 71 publications

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“…Helioseismic results from Thompson et al (1996) and Schou et al (1998) showed that radial gradients in subsurface angular velocity are small in the convection zone down to around 0.7 solar radii, and that the large radial shears that occur around 0.7 solar radii are such that the rotation rate decreases with depth at low latitudes, contrary to the assumption of Leighton (1969). Unlike the model of Leighton (1969), the model behaved in a stable, oscillatory manner without a radial gradient in the interior angular velocity.…”

Section: The Influence Of Meridional Flows On the Babcock-leighton Modelmentioning

confidence: 49%

Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

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This review describes observations of the polar magnetic fields, models for the cyclical formation and decay of these fields, and evidence of their great influence in the solar atmosphere. The polar field distribution dominates the global structure of the corona over most of the solar cycle, supplies the bulk of the interplanetary magnetic field via the polar coronal holes, and is believed to provide the seed for the creation of the activity cycle that follows. A broad observational knowledge and theoretical understanding of the polar fields is therefore an essential step towards a global view of solar and heliospheric magnetic fields. Analyses of both high-resolution and long-term synoptic observations of the polar fields are summarized. Models of global flux transport are reviewed, from the initial phenomenological and kinematic models of Babcock and Leighton to present-day attempts to produce time-dependent maps of the surface magnetic field and to explain polar field variations, including the weakness of the cycle 23 polar fields. The relevance of the polar fields to solar physics extends far beyond the surface layers from which the magnetic field measurements usually derive. As well as discussing the polar fields' role in the interior as seed fields for new solar cycles, the review follows their influence outward to the corona and heliosphere. The global coronal magnetic structure is determined by the surface magnetic flux distribution, and is dominated on large scales by the polar fields. We discuss the observed effects of the polar fields on the coronal hole structure, and the solar wind and ejections that travel through the atmosphere. The review concludes by identifying gaps in our knowledge, and by pointing out possible future sources of improved observational information and theoretical understanding of these fields. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: The Influence Of Meridional Flows On the Babcock-leighton Modelmentioning

confidence: 49%

Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

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“…Surface differential rotation (SDR) can be easily observed in the Sun, with detailed observations going back to Carrington (1860); and subsurface rotation has been inferred from helioseismic data of the Sun's 5 minute p-mode oscillations (e.g., Thompson et al 1996). However, it is a challenge to observe SDR directly at the surfaces of other stars.…”

Section: Introductionmentioning

confidence: 99%

Differential Rotation of the Active G5 V Star κ¹Ceti: Photometry from theMOSTSatellite

Ruciński

Walker

Matthews

et al. 2004

PUBL ASTRON SOC PAC

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ABSTRACT. About 30.5 days of nearly uninterrupted broadband photometry of the solar-type star k 1 Ceti, obtained with the MOST (Microvariability and Oscillations of Stars) satellite, shows evidence for two large starspots with different rotation periods of 8.9 and ∼9.3 days ( ). Ground-based measurements of Ca ii H and K emission DQ/Q Ӎ 4% in 2002 and 2003 reveal variations in chromospheric activity with a period of about 9.3 days. The data were obtained during the MOST commissioning phase. When the data are combined with historical observations, they indicate that the 9.3 day spot has been stable in its period for over 30 yr. The photometry, with a sampling rate of approximately once per minute, was also used to search for acoustic (p-mode) oscillations in the star. We detect no clear evidence for p-modes in the k 1 Ceti photometry, with a noise level around 7-9 mmag at frequencies in the range of 0.5-4 mHz (3 j detection limit of 21-27 mmag). There were no flares or planetary transits during 30.5 days of MOST monitoring with light amplitudes greater than 2 mmag (durations 1200 minutes) and 3 mmag (2-200 minute durations). While this rules out any close-in planets with Jupiter diameters ≥0.5 and orbital inclinations close to 90Њ, the scatter in differential radial velocities permit a close giant planet in a more highly inclined orbit.On-line material: machine-readable table

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“…The flow structures of both scales can deepen our understanding of the generation of solar magnetism, and of the birth and evolution of solar active regions. Solar rotation rates have been widely studied by use of direct Doppler velocity measurements (e.g., Howard & LaBonte 1980), by tracking photospheric magnetic or supergranular features (e.g., Meunier 1999), and by both global and local helioseismology (e.g., Thompson et al 1996;Giles 1999). The solar-cycle variations of solar rotation known as torsional oscillations were first observed by Howard & LaBonte (1980), and then studied by many researchers using different approaches (e.g., Snodgrass 1985;Howe et al 2000;Ulrich 2001).…”

Section: Introductionmentioning

confidence: 99%

Torsional Oscillation, Meridional Flows, and Vorticity Inferred in the Upper Convection Zone of the Sun by Time‐Distance Helioseismology

Zhao

Kosovichev

2004

ApJ

314

241

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By applying time-distance helioseismology measurements and inversions to Solar and Heliospheric Observatory (SOHO) Michelson Doppler Imager (MDI) dynamics campaign data, we obtain synoptic maps of subsurface plasma-flow fields at a depth of 0-12 Mm for seven solar Carrington rotations, covering the years 1996-2002, from solar-activity minimum to maximum. Vorticity distribution and both zonal and meridional flows are derived from such synoptic flow maps, which contain an enormous amount of information about solar dynamics. The results for the zonal flows agree well with previous results. The meridional flows of an order of 20 m s À1 are found to remain poleward during the whole period of observations. In addition to the poleward meridional flows observed at the solar minimum, extra meridional circulation cells of flow converging toward the activity belts are found in both hemispheres, which may imply plasma downdrafts in the activity belts. These converging flow cells migrate toward the solar equator together with the activity belts as the solar cycle evolves. The vorticity distributions are largely linear with latitude, and the deviations from the vorticity caused by the mean differential rotation are presented. Patterns of large-scale flows are investigated for a large active region at different depths. Converging flows toward the center of the active region are found near the solar surface, and divergent flows in this large active region are found to be rooted much deeper than similar flows observed in individual sunspots. We conclude that the extremely rich and complicated dynamics of the upper convection zone reveal remarkable organization on the large scale, which can be correlated with the magnetic activity zones.

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Differential Rotation and Dynamics of the Solar Interior

Cited by 373 publications

References 71 publications

Solar Magnetism in the Polar Regions

Solar Magnetism in the Polar Regions

Differential Rotation of the Active G5 V Star κ¹Ceti: Photometry from theMOSTSatellite

Torsional Oscillation, Meridional Flows, and Vorticity Inferred in the Upper Convection Zone of the Sun by Time‐Distance Helioseismology

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Differential Rotation and Dynamics of the Solar Interior

Cited by 373 publications

References 71 publications

Solar Magnetism in the Polar Regions

Solar Magnetism in the Polar Regions

Differential Rotation of the Active G5 V Star κ1Ceti: Photometry from theMOSTSatellite

Torsional Oscillation, Meridional Flows, and Vorticity Inferred in the Upper Convection Zone of the Sun by Time‐Distance Helioseismology

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Product

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Differential Rotation of the Active G5 V Star κ¹Ceti: Photometry from theMOSTSatellite