THE CIRCULATION DOMINATED SOLAR DYNAMO MODEL REVISITED Gustavo A. Guerrero E. (IAG/USP) Elisabete M. de Gouveia Dal Pino (IAG/USP) Jose D. Muñoz (UNAL)

Slides:

Advertisements

Similar presentations

The solar dynamo(s) Fausto Cattaneo Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas Chicago 2003.

Advertisements

Vu Pham A new dynamo pattern revealed by the tilt angle of bipolar sunspot groups Egor Illarionov Moscow State University Helicity Thinkshop on Solar Physics.

Historical Development of Solar Dynamo Theory Historical Development of Solar Dynamo Theory Arnab Rai Choudhuri Department of Physics Indian Institute.

The Origin of the Solar Magnetic Cycle Arnab Rai Choudhuri Department of Physics Indian Institute of Science.

2011/08/ ILWS Science Workshop1 Solar cycle prediction using dynamos and its implication for the solar cycle Jie Jiang National Astronomical Observatories,

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

Irregularities of solar cycle and their theoretical modeling Arnab Rai Choudhuri Department of Physics Indian Institute of Science.

Planetary tides and solar activity Katya Georgieva

1. 2 Apologies from Ed and Karl-Heinz

Scientific astrology: planetary effects on solar activity Katya Georgieva Solar-Terrestrial Influences Lab., Bulgarian Academy of Sciences In collaboration.

Effects of magnetic diffusion profiles on the evolution of solar surface poloidal fields. Night Song The Evergreen State College Olympia, WA with.

Physics 681: Solar Physics and Instrumentation – Lecture 20 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

Influence of depth-dependent diffusivity profiles in governing the evolution of weak, large-scale magnetic fields of the sun Night Song and E.J. Zita,

Solar dynamo and the effects of magnetic diffusivity E.J. Zita and Night Song, The Evergreen State College 1 Mausumi Dikpati and Eric McDonald, HAO/NCAR.

Effects of magnetic diffusion profiles on the evolution of solar surface poloidal fields. Night Song The Evergreen State College Olympia, WA with.

Influence of depth-dependent diffusivity profiles in governing the evolution of weak, large-scale magnetic fields of the Sun Night Song and E.J. Zita,

Influence of depth-dependent diffusivity profiles in governing the evolution of weak, large-scale magnetic fields of the Sun Night Song and E.J. Zita,

Prediction on Time-Scales of Years to Decades Discussion Group A.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

A topological view of 3D global magnetic field reversal in the solar corona Rhona Maclean Armagh Observatory 5 th December 2006.

Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetism Feb. 09, 2012.

Magnetic models of solar-like stars Laurène Jouve (Institut de Recherche en Astrophysique et Planétologie) B-Cool meeting December 2011.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

Sunspots: the interface between dynamos and the theory of stellar atmospheres Axel Brandenburg (Nordita/Stockholm) 70 yr Guenther.

From kinematics to dynamics: Meridional circulation and torsional oscillations From kinematics to dynamics: Meridional circulation and torsional oscillations.

The Flux Transport Dynamo, Flux Tubes and Helicity The Flux Transport Dynamo, Flux Tubes and Helicity Arnab Rai Choudhuri Department of Physics Indian.

Activity Cycles in Stars Dr. David H. Hathaway NASA Marshall Space Flight Center National Space Science and Technology Center.

Effects of the Observed Meridional Flow Variations since 1996 on the Sun’s Polar Fields David H. Hathaway 1 and Lisa Upton 2,3 1 NASA/Marshall Space Flight.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

The Solar Dynamo and Emerging Flux Presented by Angelo P. Verdoni Physics 681 Fall 05 George H. Fisher, Yuhong Fan, Dana W. Longcope, Mark G. Linton and.

The Solar Dynamo Saga: Chapter12 David Hathaway NASA Marshall Space Flight Center 2011 December 12 – NSO

R.D. Simitev School of Mathematics & Statistics F.H. Busse Institute of Physics Convection-driven spherical dynamos: bistability and attempts to model.

Solar activity as a surface phenomenon Axel Brandenburg (Nordita/Stockholm) Kemel+12 Ilonidis+11Brandenburg+11Warnecke+11 Käpylä+12.

Fifty Years Of Solar Events NOAO 50 th Anniversary Symposium.

The Rise of Solar Cycle 24: Magnetic Fields from the Dynamo through the Photosphere and Corona and Connecting to the Heliosphere Part 1: Interior and Photosphere.

The Sun as a whole: activity as seen by helioseismology

Hinode 7, Takayama, Japan, th November, 2013 Solar Cycle Predictions Recent Advances in Modeling and Observations Dibyendu Nandy Center for Excellence.

3D Spherical Shell Simulations of Rising Flux Tubes in the Solar Convective Envelope Yuhong Fan (HAO/NCAR) High Altitude Observatory (HAO) – National Center.

Recent Progress in Understanding The Sun’s Magnetic Dynamo David H. Hathaway NASA/MSFC National Space Science and Technology Center 2004 April 28 University.

Flows in the Solar Convection Zone David Hathaway NASA/MSFC National Space Science and Technology Center 2004 July 21 David Hathaway NASA/MSFC National.

Modeling the Sun’s global magnetic field Karel Schrijver SHINE 2006 "[The] most important attitude is to find which forgotten physical processes are responsible.

Team Report on integration of FSAM to SWMF and on FSAM simulations of convective dynamo and emerging flux in the solar convective envelope Yuhong Fan and.

The Solar Dynamo NSO Solar Physics Summer School Tamara Rogers, HAO June 15, 2007.

The Solar Dynamo Saga: Chapter 11 Dr. David Hathaway NASA Marshall Space Flight Center 2009 August 15 Huntsville Hamfest.

Meridional Circulation Variability from Large-Aperture Ring Diagrams Irene González Hernández Rudi Komm Thierry Corbard Frank Hill Rachel Howe Deborah.

The Sun as whole: activity as seen by helioseismology A.C. Birch (Max Planck Institute for Solar System Research)

Andrés Muñoz-Jaramillo Harvard-Smithsonian Center for Astrophysics

1 Mei Zhang （ National Astronomical Observatory, Chinese Academy of Sciences ） Solar cycle variation of kinetic helicity Collaborators: Junwei Zhao (Stanford,

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

Self-assembly of shallow magnetic spots through strongly stratified turbulence Axel Brandenburg (Nordita/Stockholm) Kemel+12 Brandenburg+13 Warnecke+11.

Dynamo Model for Magnetic Activity Saturation in Rapidly Rotating Solar-Type Stars Stellar magnetic activity: dependence on rotation rate (observations)

Solar Magnetic Field Reversal V J Pizzo SHINE Workshop August 18, 2002.

Sunspot activity and reversal of polar fields in the current cycle 24 A.V. Mordvinov 1, A.A. Pevtsov 2 1 Institute of Solar-Terrestrial Physics of SB RAS,

Prograde patterns in rotating convection and implications for the dynamo Axel Brandenburg (Nordita, Copenhagen  Stockholm) Taylor-Proudman problem Near-surface.

What the Long-Term Sunspot Record Tells Us About Space Climate David H. Hathaway NASA/MSFC National Space Science and Technology Center Huntsville, AL,

Solar Magnetism: Solar Cycle Solar Dynamo Coronal Magnetic Field CSI 662 / ASTR 769 Lect. 03, February 6 Spring 2007 References: NASA/MSFC Solar Physics.

CSI /PHYS Solar Atmosphere Fall 2004 Lecture 04 Sep. 22, 2004 Solar Magnetic Field, Solar Cycle, and Solar Dynamo.

H. Isobe Plasma seminar 2004/06/16 1. Explaining the latitudinal distribution of sunspots with deep meridional flow D. Nandy and A.R. Choudhhuri 2002,

CSI 769/ASTR 769 Topics in Space Weather Fall 2005 Lecture 03 Sep. 20, 2005 Surface Magnetic Field Aschwanden, “Physics of the Solar Corona” Chap. 5, P.

SOHO/ESA/NASA Solar cycle - modeling and predicting Petri Käpylä NORDITA AlbaNova University Center Stockholm, Sweden Stockholm, 2nd Feb 2007 SST NASA.

Solar Magnetic Field Reversal and the Role of Dynamo Families

An update on convection zone modeling with the ASH code

Is solar activity a surface phenomenon?

THEORY OF MERIDIONAL FLOW AND DIFFERENTIAL ROTATION

Introduction to Space Weather

CP Hung, L Jouve, AS Brun, A Fournier, O Talagrand

Introduction to Space Weather

A low order dynamo model and possible applications

Solar and Heliospheric Physics

Presentation transcript:

THE CIRCULATION DOMINATED SOLAR DYNAMO MODEL REVISITED Gustavo A. Guerrero E. (IAG/USP) Elisabete M. de Gouveia Dal Pino (IAG/USP) Jose D. Muñoz (UNAL) IV WORKSHOP NOVA FISICA NO ESPACIO, CAMPOS DO JORDAO, FEVEREIRO 20-25

Contents Sunspot cycle The Solar dynamo Mathematical Formalism (MHD) Results Conclusions

SUNSPOT CYCLE FIGURES Pairs of sunspots appearance, tilt of inclination (Joy’s law). Latitude of appearance (Spörer`s Law) Inversion of polarities, 11 years cycle (Hale`s Law) Equatorward migration of sunspots Intensity of the Magnetic Fields ~10 3 G for the sunspots Tens of G. for the diffuse poloidal field Sunspots pair Observational butterfly diagram (NASA) Solar cycle

THE SOLAR DYNAMO 1. Dipolar initial magnetic field 2. Differential rotation -> belt of toroidal field arround the solar equator. 3. Magnetic Flux tubes (ρi Magnetic bouyancy. 4. Tilt bipolar active magnetic regions (BMR) 5. Decay of BMR`s. (Fan et al. 2003)

MATHEMATICAL FORMALISM The MHD induction equation is: By assuming spherical symmetry: Differential Rotation (1) (2) (3) Replacing (2) and (3) in (1) and separating the poloidal and toroidal components, we obtain: (4) (5) Meridional Circulation

Differential rotation Helioseismologic observations: dΩ/dr(r=0.7 Rסּ) (6) (Schou et al., 1998)

MATHEMATICAL FORMALISM The MHD induction equation is: By assuming spherical symmetry: Differential Rotation (1) (2) (3) Replacing (2) and (3) in (1) and separating the poloidal and toroidal components, we obtain: (4) (5) Meridional Circulation

A superficial flow about 20m/s is observed in all latitudes, but the way how the counter flow happens is until now unknown. We assume a simple convection cell by meridional quadrant thus: (Haber et al., 1998) (7) (8)

MATHEMATICAL FORMALISM The MHD induction equation is: By assuming spherical symmetry: Differential Rotation (1) (2) (3) Replacing (2) and (3) in (1) and separating the poloidal and toroidal components, we obtain: (4) (5) Meridional Circulation

Magnetic Bouyancy Diffusivity Magnetic diffusivity for the toroidal field Magnetic diffusivity for the poloidal field (9) (10) (11)

MATHEMATICAL FORMALISM The MHD induction equation is: By assuming spherical symmetry: Differential Rotation (1) (2) (3) Replacing (2) and (3) in (1) and separating the poloidal and toroidal components, we obtain: (4) (5) Meridional Circulation

TWO IMPORTANT MODELS Dikpati & Charbonneau, 1999, ApJ, 518, 508. –Solar like differential rotation. –Non local source formulation. Nandy & Choudhuri, 2002, Science,296, –Deep Meridional Flow. –Numerical formulation of the source term.

RESULTS ParameterValue Uo2000 cm/s So25 cm/s ηCηC 2.4x10 11 Rb (deep)0.675 R סּ We solved the equations (4) and (5) inequations (4) and (5) a two dimensional mesh of 128x128 spatial divisions, with 0.55<r<1 Rסּ, and 0<θ<π/2 and the next boundary conditions: At θ=0A=0 B=0 At θ=π/2 dA/dt=0B=0 At r=0.55A=0B=0 At r= Rסּ (free space cond)B=0 Toroidal field Radial field

Deep meridional Flow (Rb=0.61 ) Deep meridional Flow (Rb=0.61 R סּ ) t=T/8 t=T/2 t=T/4 t=3T/8 Toroidal Poloidal Toroidal field Radial field

Exploring a prolate differential rotation Based on early helioseismic results of Charbonneau et al., 1999, we modified the r C term in eq. (6) to get a prolate shape differentail rotationr C term in eq. (6) Toroidal field Radial field

Differential rotation Helioseismologic observations: dΩ/dr(r=0.7 Rסּ) (6) (Schou et al., 1998)

Exploring a prolate differential rotation Based on early helioseismic results of Charbonneau et al., 1999, we modified the r C term in eq. (6) to get a prolate shape differentail rotationr C term in eq. (6) Toroidal field Radial field

CONCLUSIONS 1.If the meridional flow is confined to the convective zone, the sunspots are mainly concentrated near the poles. 2.If the flow is allowed to penetrate deeper down 0.61R, the model gives a better result since a branch of maximum toroidal field is produced at low latitudes in agreement with the observations. However, in this case another branch also appears near the poles which is inconsistent with the observed butterfly diagrams. 3.If we consider a prolate differential rotation there is a lager concentration of the toroidal field towards the equator in better agreement with the observations. 4.Both the global behavior of the circulation and the physical mechanism behind it need further revisions.