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Large-scale flows in the Sun: Characteristics and time variations

Published online by Cambridge University Press:  27 November 2018

Sarbani Basu
Sarbani Basu*
Affiliation:
Department of Astronomy, Yale University PO Box 208101, New Haven, CT 06520-8101, USA email: [email protected]
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Abstract

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The study of solar rotation has a 150-year history. Early studies were restricted to looking at the movement of sunspots; much later came studies using other tracers such as supergranules, and spectroscopic measurements using Doppler shifts of spectral lines. These studies also found evidence of other large-scale flows, such as the meridional flows in the north-south direction and the zonal flows, or torsional oscillations, parallel to the equator. However, until the 1980s, the study of solar rotation and large-scale flows was restricted to what could be observed on the solar surface. The advent of good helioseismic data changed that and gave us the means to study flows in the solar interior. Instruments like GONG, MDI and HMI have now collected helioseismic data for two solar cycles and these also allow us to study the large scale flows and their variations with time and solar activity. We review what the long data sets tell us about the these flows and discuss some of the differences between solar cycles 23 and 24.

Keywords

Sun:generalSun:rotationSun:activitySun:oscillationsSun:interior
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 3 - 8
Copyright
Copyright © International Astronomical Union 2018 

References

Antia, H. M. & Basu, S., 2000, ApJ, 541, 442Google Scholar
Antia, H. M. & Basu, S., 2001, ApJL, 559, L67Google Scholar
Antia, H. M. & Basu, S., 2010, Astrophys. J., 720, 494Google Scholar
Antia, H. M. & Basu, S., 2011, Astrophys. J. Letters, 735, L45Google Scholar
Antia, H. M. & Basu, S. 2013, in Journal of Physics Conference Series, Vol. 440, Journal of Physics Conference Series, 012018Google Scholar
Antia, H. M., Basu, S., & Chitre, S. M., 2008, Astrophys. J., 681, 680Google Scholar
Barekat, A., Schou, J., & Gizon, L., 2016, Astron. Astrophys., 595, A8Google Scholar
Basu, S. & Antia, H. M., 2001, MNRAS, 324, 498Google Scholar
Basu, S. & Antia, H. M., 2003, ApJ, 585, 553Google Scholar
Basu, S. & Antia, H. M., 2010, Astrophys. J., 717, 488Google Scholar
Basu, S., Antia, H. M., & Tripathy, S. C., 1999, Astrophys. J., 512, 458Google Scholar
Beck, J. G., 2000, Solar Phys., 191, 47Google Scholar
Bogart, R. S., Baldner, C. S., & Basu, S., 2015, Astrophys. J., 807, 125Google Scholar
Brown, T. M., 1985, Nature, 317, 591Google Scholar
Chakraborty, S., Choudhuri, A. R., & Chatterjee, P., 2009, Physical Review Letters, 102, 041102Google Scholar
Chen, R. & Zhao, J., 2017, Astrophys. J., 849, 144Google Scholar
Corbard, T., Jiménez-Reyes, S. J., Tomczyk, S., Dikpati, M., & Gilman, P. 2001, in ESA Special Publication, Vol. 464, SOHO 10/GONG 2000 Workshop: Helio- and Asteroseismology at the Dawn of the Millennium, ed. Wilson, A. & Pallé, P. L., 265–272Google Scholar
Duvall, Jr, T. L., Dziembowski, W. A., Goode, P. R., et al. 1984, Nature, 310, 22Google Scholar
Giles, P. M., Duvall, T. L., Scherrer, P. H., & Bogart, R. S., 1997, Nature, 390, 52Google Scholar
Gizon, L. & Birch, A. C., 2005, Living Reviews in Solar Physics, 2, 6Google Scholar
Glatzmaier, G. A., 1985, Astrophys. J., 291, 300Google Scholar
Haber, D. A., Hindman, B. W., Toomre, J., et al. 2002, Astrophys. J., 570, 855Google Scholar
Hathaway, D. H. & Rightmire, L., 2010, Science, 327, 1350Google Scholar
Hazra, G., Karak, B. B., & Choudhuri, A. R., 2014, Astrophys. J., 782, 93Google Scholar
Hill, F., Stark, P. B., Stebbins, R. T., et al. 1996, Science, 272, 1292Google Scholar
Howard, R. & Labonte, B. J., 1980, ApJL, 239, L33Google Scholar
Howe, R., Christensen-Dalsgaard, J., Hill, F., et al. 2005, ApJ, 634, 1405Google Scholar
Howe, R., Christensen-Dalsgaard, J., Hill, F., et al. 2007, Advances in Space Research, 40, 915Google Scholar
Howe, R., Christensen-Dalsgaard, J., Hill, F., et al.. 2000a, Science, 287, 2456Google Scholar
Howe, R., Christensen-Dalsgaard, J., Hill, F., et al. 2000b, ApJL, 533, L163Google Scholar
Jackiewicz, J., Serebryanskiy, A., & Kholikov, S., 2015, Astrophys. J., 805, 133Google Scholar
Komm, R. W., Howard, R. F., & Harvey, J. W., 1993, Sol Phys, 147, 207Google Scholar
Müller, D., Marsden, R. G., Cyr, O. C. St., & Gilbert, H. R., 2013, Solar Phys., 285, 25Google Scholar
Rajaguru, S. P. & Antia, H. M., 2015, Astrophys. J., 813, 114Google Scholar
Scheiner, C. 1630, Rosa Ursina, doi:10.3931/e-rara-556Google Scholar
Scherrer, P. H., Bogart, R. S., Bush, R. I., et al. 1995, Solar Phys., 162, 129Google Scholar
Scherrer, P. H., Schou, J., Bush, R. I., et al. 2012, Solar Phys., 275, 207Google Scholar
Schou, J., Antia, H. M., Basu, S., et al. 1998, Astrophys. J., 505, 390Google Scholar
Thompson, M. J., Toomre, J., Anderson, E. R., et al. 1996, Science, 272, 1300Google Scholar
Vorontsov, S. V., Christensen-Dalsgaard, J., Schou, J., Strakhov, V. N., & Thompson, M. J., 2002, Science, 296, 101Google Scholar