Current Helicity of in Solar Active Regions as a Tracer of Solar Dynamo

Sokoloff Dmitry, d_sokoloff@hotmail.com, Moscow State University, Russia, Russian Fed
Znang Hongqi, hzhang@bao.ac.cn, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Moss David, moss@maths.man.ac.uk, School of Mathematics, University of Manchester, Manchester M13 9PL, UK
Kleeorin Nathan, nat@menix.bgu.ac.il, Department of Mechanical Engineering, Ben-Gurion University of Negev, POB 653, 84105 Beer-Sheva, Israel
Kuzanyan Kirill, kuzanyan@izmiran.ru, IZMIRAN, Troitsk, Moscow Region 142190, Russia
Rogachevskii Igor, gary@bgu.ac.il, Department of Mechanical Engineering, Ben-Gurion University of Negev, POB 653, 84105 Beer-Sheva, Israel
Yu Gao, gy@bao.ac.cn, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Haiqing Xu, xu@bao.ac.cn, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China

Abstract
The current helicity in solar active regions traces the magnetic helicity of large-scale dynamo generated field. We consider a dynamo model with dynamo suppression based on the magnetic helicity evolution and algebraic quenching, obtain butterfly diagrams for the small-scale current helicity and for the large-scale magnetic helicity and compare them with obtained from observations the butterfly diagram for the current helicity in active regions. This comparison shows that the large-scale magnetic helicity resembles the observational data much better then the small-scale current helicity. Theoretical interpretation of these results is given.