Skip to main content Accessibility help
×
Home
Hostname: page-component-747cfc64b6-ngm8v Total loading time: 0.337 Render date: 2021-06-14T19:13:10.223Z Has data issue: true Feature Flags: { "shouldUseShareProductTool": true, "shouldUseHypothesis": true, "isUnsiloEnabled": true, "metricsAbstractViews": false, "figures": true, "newCiteModal": false, "newCitedByModal": true, "newEcommerce": true }

Current helicity constraints in solar dynamo models

Published online by Cambridge University Press:  18 July 2013

D. Sokoloff
Affiliation:
Department of Physics, Moscow State University, Moscow 119992, Russia email: sokoloff.dd@gmail.com
H. Zhang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: hzhang@bao.ac.cn
D. Moss
Affiliation:
School of Mathematics, University of Manchester, Manchester M13 9PL, UK email: moss@maths.man.ac.uk
N. Kleeorin
Affiliation:
Department of Mechanical Engineering, Ben-Gurion University of Negev, POB 653, 84105 Beer-Sheva, Israel email: nat@menix.bgu.ac.il
K. Kuzanyan
Affiliation:
IZMIRAN, Troitsk, Moscow Region 142190, Russia email: kuzanyan@izmiran.ru
I. Rogachevski
Affiliation:
Department of Mechanical Engineering, Ben-Gurion University of Negev, POB 653, 84105 Beer-Sheva, Israel email: gary@bgu.ac.il
Yu Gao
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: hzhang@bao.ac.cn
H. Xu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: hzhang@bao.ac.cn
Rights & Permissions[Opens in a new window]

Abstract

We investigate to what extent the current helicity distribution observed in solar active regions is compatible with solar dynamo models. We use an advanced 2D mean-field dynamo model with dynamo action largely concentrated near the bottom of the convective zone, and dynamo saturation based on the evolution of the magnetic helicity and algebraic quenching. For comparison, we also studied a more basic 2D mean-field dynamo model with simple algebraic alpha quenching only. Using these numerical models we obtain butterfly diagrams for both the small-scale current helicity and the large-scale magnetic helicity, and compare them with the butterfly diagram for the current helicity in active regions obtained from observations. This comparison shows that the current helicity of active regions, as estimated by −A·B evaluated at the depth from which the active region arises, resembles the observational data much better than the small-scale current helicity calculated directly from the helicity evolution equation. Here B and A are respectively the dynamo generated mean magnetic field and its vector potential.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

References

Baliunas, S., Frick, P., Moss, D., Popova, E., Sokoloff, D., & Soon, W. 2006, MNRAS, 365, 181 CrossRefGoogle Scholar
Bao, S. D. & Zhang, H. Q. 1998, ApJ, 496, L43 CrossRefGoogle Scholar
Brandenburg, A. 2007, Highlights of Astronomy, 14, 291 Google Scholar
Choudhuri, A. R., Chatterjee, P., & Nandy, D. 2004, ApJ, 615, L57 CrossRefGoogle Scholar
Dikpati, M. & Gilman, P. A. 2001, ApJ, 559, 420 CrossRefGoogle Scholar
Hagino, M. & Sakurai, T. 2004, Publ. Astron. Soc. Japan., 56, 831 CrossRefGoogle Scholar
Kleeorin, N., Kuzanyan, K., Moss, D., Rogachevskii, I., Sokoloff, D., & Zhang, H. 2003, A&A, 409, 1097 Google Scholar
Kleeorin, N., Rogachevskii, I., & Ruzmaikin, A. 1995, A&A, 297, 159 Google Scholar
Mitra, D., Moss, D., Tavakol, R., & Brandenburg, A. 2011, A&A, 526, A138 Google Scholar
Parker, E. 1955, ApJ, 122, 293 CrossRefGoogle Scholar
Pevtsov, A. A., Canfield, R. C., & Metcalf, T. R. 1994, ApJ, 425, L117 CrossRefGoogle Scholar
Pouquet, A., Frisch, U., & Leorat, J. 1976, J. Fluid Mech., 77, 321 CrossRefGoogle Scholar
Seehafer, N. 1990, Solar Phys., 125, 219 CrossRefGoogle Scholar
Xu, H., Gao, Y, Popova, H. P., Nefedov, S. N., Zhang, H., & Sokoloff, D. D. 2009, Astron. Rep., 53, 160 CrossRefGoogle Scholar
Zhang, H., Sokoloff, D., Rogachevskii, I., Moss, D., Lamburt, V., Kuzanyan, K., & Kleeorin, N. 2006, MNRAS, 365, 276 CrossRefGoogle Scholar
Zhang, H., Moss, D., Kleeorin, N., Kuzanyan, K., Rogachevskii, I., Sokoloff, D., & Gao, Y., Xu, H. 2012, ApJ, 751, 47 CrossRefGoogle Scholar
You have Access

Send article to Kindle

To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

Current helicity constraints in solar dynamo models
Available formats
×

Send article to Dropbox

To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

Current helicity constraints in solar dynamo models
Available formats
×

Send article to Google Drive

To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

Current helicity constraints in solar dynamo models
Available formats
×
×

Reply to: Submit a response

Please enter your response.

Your details

Please enter a valid email address.

Conflicting interests

Do you have any conflicting interests? *