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85:, which do not have a radiative core and only have a convective zone, demonstrate that they maintain large-scale, solar-strength magnetic fields and display solar-like activity despite the absence of tachoclines. This suggests that the convective zone alone may be responsible for the function of the solar dynamo.
23:
Internal rotation in the Sun, showing differential rotation in the outer convective region (as a function of latitude) and almost uniform rotation in the central radiative region. The transition between these regions is called the tachocline. To convert the y-axis to period, use 500 nanoHz = 23.15
65:
indicate that the tachocline is located at a radius of at most 0.70 times the solar radius (measured from the core, i.e., the surface is at 1 solar radius), with a thickness of 0.04 times the solar radius. This would mean the area has a very large shear profile that is one way that large scale
56:
as the rotation rate changes very rapidly. The convective exterior rotates as a normal fluid with differential rotation with the poles rotating slowly and the equator rotating quickly. The radiative interior exhibits solid-body rotation, possibly due to a
331:
Charbonneau, P.; Christensen-Dalsgaard, J.; Henning, R.; Larsen, R. M.; Schou, J.; Thompson, M. J.; Tomczyk, S. (December 1999). "Helioseismic
Constraints on the Structure of the Solar Tachocline".
61:. The rotation rate through the interior is roughly equal to the rotation rate at mid-latitudes, i.e. in-between the rate at the slow poles and the fast equator. Recent results from
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The geometry and width of the tachocline are thought to play an important role in models of the
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370:"Helioseismic measurement of the extent of overshoot below the solar convection zone"
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200:"The Discovery of Solar-like Activity Cycles Beyond the End of the Main Sequence?"
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Region of the Sun between the radiative interior and the convective zone
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Spiegel, E. A.; Zahn, J. -P. (November 1992). "The solar tachocline".
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290:"Large-Scale Dynamics of the Convection Zone and Tachocline"
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Basu, Sarbani; Antia, H. M.; Narasimha, D. (March 1994).
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Hughes, D. W.; Rosner, R.; Weiss, N. O. (2007-05-31).
81:
field. Recent radio observations of cooler stars and
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374:Monthly Notices of the Royal Astronomical Society
52:. This causes the region to have a very large
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417:. Cambridge University Press. p. 382.
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111:An illustration of the structure of the
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198:Route, Matthew (October 20, 2016).
978:. You can help Knowledge (XXG) by
100:in 1992 by analogy to the oceanic
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204:The Astrophysical Journal Letters
962:
942:
941:
77:field to create a much stronger
294:Living Reviews in Solar Physics
66:magnetic fields can be formed.
1:
924:List of heliophysics missions
970:This article related to the
929:Category:Missions to the Sun
32:is the transition region of
235:10.3847/2041-8205/830/2/L27
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957:
259:Astronomy and Astrophysics
937:
905:G-type main-sequence star
469:
333:The Astrophysical Journal
92:was coined in a paper by
73:by winding up the weaker
768:In mythology and culture
288:Miesch, Mark S. (2005).
395:10.1093/mnras/267.1.209
271:1992A&A...265..106S
46:differentially rotating
635:Supra-arcade downflows
181:
25:
615:Coronal mass ejection
282:Additional References
110:
22:
879:Standard solar model
849:Solar radio emission
667:List of solar cycles
414:The Solar Tachocline
315:10.12942/lrsp-2005-1
699:Magnetic switchback
386:1994MNRAS.267..209B
345:1999ApJ...527..445C
306:2005LRSP....2....1M
226:2016ApJ...830L..27R
889:Sunlight radiation
484:Internal structure
182:
42:radiative interior
26:
987:
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919:Solar observatory
834:Solar observation
732:Termination shock
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600:Transition region
424:978-1-139-46258-7
36:of more than 0.3
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839:Solar phenomena
814:Solar astronomy
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709:Helioseismology
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630:Helmet streamer
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63:helioseismology
50:convective zone
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94:Edward Spiegel
40:, between the
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980:expanding it
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854:Solar System
824:Solar energy
819:Solar dynamo
780:Heliophysics
610:Coronal loop
605:Coronal hole
582:Moreton wave
564:Chromosphere
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160:Solar corona
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135:Chromosphere
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83:brown dwarfs
68:
59:fossil field
38:solar masses
29:
27:
912:Exploration
790:Solar deity
737:Heliosheath
719:Heliosphere
689:Wolf number
662:Solar cycle
526:Photosphere
265:: 106–114.
130:Photosphere
102:thermocline
1019:Categories
864:Solar time
785:In culture
742:Heliopause
694:Solar wind
625:Prominence
517:Atmosphere
502:Tachocline
217:1609.07761
185:References
175:Solar wind
170:Prominence
155:Solar core
150:Tachocline
90:tachocline
30:tachocline
1030:Sun stubs
747:Bow shock
654:Variation
620:Nanoflare
404:0035-8711
361:0004-637X
324:1614-4961
244:119111063
210:(2): 27.
88:The term
947:Category
300:(1): 1.
120:Granules
79:toroidal
75:poloidal
44:and the
763:Eclipse
756:Related
577:Spicule
549:Sunspot
544:Faculae
539:Granule
463:The Sun
382:Bibcode
341:Bibcode
302:Bibcode
267:Bibcode
222:Bibcode
125:Sunspot
592:Corona
421:
402:
359:
322:
242:
48:outer
974:is a
704:Flare
572:Plage
240:S2CID
212:arXiv
165:Flare
54:shear
34:stars
24:days.
976:stub
884:Star
795:List
492:Core
474:List
419:ISBN
400:ISSN
357:ISSN
320:ISSN
96:and
28:The
1025:Sun
972:Sun
390:doi
378:267
349:doi
337:527
310:doi
263:265
230:doi
208:830
113:Sun
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