'Magnetic helicity' presentation slideshows

Cosmological signatures of primordial helical magnetic fields

Cosmological signatures of primordial helical magnetic fields. Tina Kahniashvili Carnegie Mellon University, USA Abastumani Astrophysical Observatory, Georgia Cosmological Magnetic Fields Monte Verita, Switzerland June 3 2009. Outline. General overview Space-time symmetry

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The Solar Corona

The Solar Corona. B. C. Low High Altitude Observatory National Center for Atmospheric Research. The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research

589 views • 39 slides

Chandrasekhar-Kendall functions in astrophysical magnetism

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I. ROGACHEVSKII, N. KLEEORIN, E. LIVERTS Ben-Gurion University of the Negev, Beer Sheva, ISRAEL

New Mechanism of Generation of Large-Scale Magnetic Field in Turbulence with Large-Scale Velocity Shear. I. ROGACHEVSKII, N. KLEEORIN, E. LIVERTS Ben-Gurion University of the Negev, Beer Sheva, ISRAEL. Outline. Introduction

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Making Magnetic Fields: Dynamos in the Nonlinear Regime

Making Magnetic Fields: Dynamos in the Nonlinear Regime. Collaborators: Alex Lazarian --- U. Wisconsin Jungyeon Cho --- Chungnam U. Dmitry Shapovalov --- JHU. Baltimore -September 2005. Outline:. Defining the problem Magnetic Helicity

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Mei Zhang ? National Astronomical Observatory, Chinese Academy of Sciences ?

Helicity Transport from the convection zone to interplanetary space. Mei Zhang ? National Astronomical Observatory, Chinese Academy of Sciences ?. Collaborators : Boon Chye Low, Natasha Flyer, Mark Miesch (NCAR, Boulder, USA) Yin Zhang, Chuanyu Wang, Juan Hao (NAOC, Beijing, China).

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Kinetic and Magnetic Helicities of Solar Active Regions

Kinetic and Magnetic Helicities of Solar Active Regions. Ram Ajor Maurya, Ashok Ambastha And Vema Reddy. Udaipur Solar Observatory Physical Research Laboratory, India. Outline. Objectives Introduction and background The Data and Sample of Active Regions

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Numerical simulations of astrophysical dynamos

Numerical simulations of astrophysical dynamos. Dynamos: numerical issues Alpha dynamos do exist: linear and nonlinear Constrained by magnetic helicity: need fluxes How high do we need to go with Rm? MRI and low PrM issue. Axel Brandenburg ( Nordita, Stockholm ). Struggle for the dynamo.

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Helicity and Helicity flux during the solar cycle

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Magnetic Helicity Transport in Active Region NOAA 10930

Magnetic Helicity Transport in Active Region NOAA 10930. Zhang, Y., Tan, B. L., Yan, Y. H Solar radio research group National Astronomical Observatories Chinese Academy of Sciences. Magnetic Helicity. Rotational motion of sunspot around its center.

447 views • 20 slides

Magnetic helicity: why is it so important and how to get rid of it

Magnetic helicity: why is it so important and how to get rid of it. Axel Brandenburg (Nordita, Copenhagen) Kandaswamy Subramanian (Pune). Brandenburg (2001, ApJ 550, 824; 2005, ApJ 625, 539) Brandenburg & Subramanian (2005, Phys. Rep., astro-ph/0405052). Magnetic helicity.

358 views • 20 slides

Diagnostics of flare activity level from turbulence parameters of photospheric plasma

RHESSI/SOHO/TRACE Workshop. Pre-event Physics. December 8-11, 2004,Sonoma, California. Diagnostics of flare activity level from turbulence parameters of photospheric plasma. Abramenko, Valentyna Big Bear Solar Observatory of NJIT avi@bbso.njit.edu www.bbso.njit.edu/~avi. Introduction.

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Active Region Evolution and the Removal of Magnetic Helicity by CMEs

Active Region Evolution and the Removal of Magnetic Helicity by CMEs. Len Culhane Mullard Space Science Laboratory University College London. SUMMARY. Long-term Evolution of Sigmoidal Structures and Related CME Activity (Glover, Harra, Matthews, Hori, Culhane, 2001, In Press, A&A)

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Shell Model Approaches to the Problem of Galactic MHD

Shell Model Approaches to the Problem of Galactic MHD. Rodion Stepanov , Peter Frick, ICMM, Perm, Russia Dmitry Sokoloff , MSU, Russia Franck Plunian, LGIT, Grenoble, France. Why and what is a shell model? MHD turbulence with rotation and applied magnetic field

280 views • 19 slides

Mei Zhang ? National Astronomical Observatory, Chinese Academy of Sciences ?

Solar cycle variation of kinetic helicity. Mei Zhang ? National Astronomical Observatory, Chinese Academy of Sciences ?. Collaborators : Junwei Zhao (Stanford, USA) Mark Miesch (HAO/NCAR, USA). Plan of the Talk. Motivation: Solar-cycle variation of current helicity

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Effects of Primordial Magnetic Helicity and Detection Possibilities

Effects of Primordial Magnetic Helicity and Detection Possibilities. Tina Kahniashvili Kansas State University New Views of the Universe. Papers: C. Caprini, R.Durrer, T.K., 2004, PRD, 69, 063006 A. Kosowsky, T.K., G. Lavrelashvili, B.Ratra, 2005, PRD, 71, 043006

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Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions

Spatio-Temporal Dynamics of Magnetic Fields and Flaring Productivity of Active Regions. Valentina I. Abramenko Big Bear Solar Observatory of NJIT Email: avi@bbso.njit.edu http://www.bbso.njit.edu/~avi/. Introduction.

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Yongliang Song & Mei Zhang (National Astronomical Observatory of China)

The effect of non-radial magnetic field on measuring helicity transfer rate. Yongliang Song & Mei Zhang (National Astronomical Observatory of China). Motivation. Our previous studies (Zhang & Low 2005; Zhang et al. 2006; Zhang & Flyer 2008; Zhang et al. 2012) have suggested that:

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2. Method outline Equation of relative helicity (Berger 1985):

a. b. c. Determination of Coronal Magnetic Helicity of Solar Active Regions Using the Linear Force-Free Field Model. Eun-Kyung Lim, Hyewon Jeong, Jongchul Chae Seoul National University, Korea. 2. Method outline Equation of relative helicity (Berger 1985):

184 views • 8 slides