Simulation of Flux Emergence from the Convection Zone Fang Fang 1, Ward Manchester IV 1, William Abbett 2 and Bart van der Holst 1 1 Department of Atmospheric,

Slides:



Advertisements
Similar presentations
Solar Theory (MT 4510) Clare E Parnell School of Mathematics and Statistics.
Advertisements

Numerical Simulations of Supergranulation and Solar Oscillations Åke Nordlund Niels Bohr Institute, Univ. of Copenhagen with Bob Stein (MSU) David Benson,
IHY General Assembly, Paris, January 2006 Photospheric flows around sunspots and pores Michal Sobotka Astronomical Institute, Academy of Sciences.
A complete study of magnetic flux emergence, interaction, and diffusion should take into account some “anomalies” In the photosphere we can observe flux.
A complete study of magnetic flux emergence, interaction, and diffusion should take into account some “anomalies” In the photosphere we can observe flux.
1. 2 Apologies from Ed and Karl-Heinz
Chip Manchester, Fang Fang, Bill Abbett, Bart van der Holst Patterns of Large- Scale Flux Emegence Patterns of Large- Scale Flux Emegence.
Modeling the Magnetic Field Evolution of the December Eruptive Flare Yuhong Fan High Altitude Observatory, National Center for Atmospheric Research.
Can We Determine Electric Fields and Poynting Fluxes from Vector Magnetograms and Doppler Shifts? by George Fisher, Brian Welsch, and Bill Abbett Space.
Emerging Flux Simulations Bob Stein A.Lagerfjard Å. Nordlund D. Benson D. Georgobiani 1.
Chip Manchester 1, Fang Fang 1, Bart van der Holst 1, Bill Abbett 2 (1)University of Michigan (2)University of California Berkeley Study of Flux Emergence:
Using Photospheric Flows Estimated from Vector Magnetogram Sequences to Drive MHD Simulations B.T. Welsch, G.H. Fisher, W.P. Abbett, D.J. Bercik, Space.
Simulations of Emerging Magnetic Flux in Active Regions W. P. Abbett Space Sciences Laboratory University of California, Berkeley.
SHINE The Role of Sub-Surface Processes in the Formation of Coronal Magnetic Flux Ropes A. A. van Ballegooijen Smithsonian Astrophysical Observatory.
Convection Simulations Robert Stein Ake Nordlund Dali Georgobiani David Benson Werner Schafenberger.
Solar Magneto-Convection: Structure & Dynamics Robert Stein - Mich. State Univ. Aake Nordlund - NBIfAFG.
Free Energies via Velocity Estimates B.T. Welsch & G.H. Fisher, Space Sciences Lab, UC Berkeley.
Understanding the Connection Between Magnetic Fields in the Solar Interior and the Solar Corona George H. Fisher Space Sciences Laboratory UC Berkeley.
Supergranulation-Scale Simulations of Solar Convection Robert Stein, Michigan State University, USA Aake Nordlund, Astronomical Observatory, NBIfAFG, Denmark.
Center for Space Environment Modeling Ward Manchester University of Michigan Yuhong Fan High Altitude Observatory SHINE July.
SSL (UC Berkeley): Prospective Codes to Transfer to the CCMC Developers: W.P. Abbett, D.J. Bercik, G.H. Fisher, B.T. Welsch, and Y. Fan (HAO/NCAR)
Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.
M1-H2: Magnetic Activity Science Goals and Approaches DRAFT! Chair(s): Abbett/Hoeksema/Komm.
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Data-Driven Simulations of AR8210 W.P. Abbett Space Sciences Laboratory, UC Berkeley SHINE Workshop 2004.
Helicity as a Component of Filament Formation D.H. Mackay University of St. Andrews Solar Theory Group.
Modeling the Dynamic Evolution of the Solar Atmosphere: C4: HMI-AIA Team Meeting: Bill Abbett SSL, UC Berkeley.
Using Photospheric Flows Estimated from Vector Magnetogram Sequences to Drive MHD Simulations B.T. Welsch, G.H. Fisher, W.P. Abbett, D.J. Bercik, Space.
Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March.
The Effect of Sub-surface Fields on the Dynamic Evolution of a Model Corona Goals :  To predict the onset of a CME based upon reliable measurements of.
MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.
The Physical Significance of Time-Averaged Doppler Shifts Along Magnetic Polarity Inversion Lines (PILs) Brian Welsch Space Sciences Laboratory, UC-Berkeley.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
Solar Rotation Lab 3. Differential Rotation The sun lacks a fixed rotation rate Since it is composed of a gaseous plasma, the rate of rotation is fastest.
Coronal Heating of an Active Region Observed by XRT on May 5, 2010 A Look at Quasi-static vs Alfven Wave Heating of Coronal Loops Amanda Persichetti Aad.
Winds and Currents in the Oceans
SLIDE SHOW 3 B changes due to transport + diffusion III -- * * magnetic Reynold number INDUCTION EQUATION B moves with plasma / diffuses through it.
Decay of a simulated bipolar field in the solar surface layers Alexander Vögler Robert H. Cameron Christoph U. Keller Manfred Schüssler Max-Planck-Institute.
The Solar Wind.
3D simulations of solar emerging flux ISOBE Hiroaki Plasma seminar 2004/04/28.
Magneto-Hydrodynamic Equations Mass conservation /t = − ∇ · (u) Momentum conservation (u)/t =− ∇ ·(uu)− ∇ −g+J×B−2Ω×u− ∇ · visc Energy conservation /t.
Karen Meyer University of St Andrews Scotland 1 st year PhD student (3 months in)
Emerging Flux Simulations & semi-Sunspots Bob Stein A.Lagerfjärd Å. Nordlund D. Georgobiani 1.
Effect of solar chromospheric neutrals on equilibrium field structures - T. Arber, G. Botha & C. Brady (ApJ 2009) 太陽雑誌会ー 22/01/10.
Physics 681: Solar Physics and Instrumentation – Lecture 22 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.
SHINE Formation and Eruption of Filament Flux Ropes A. A. van Ballegooijen 1 & D. H. Mackay 2 1 Smithsonian Astrophysical Observatory, Cambridge,
Moving Magnetic Features (MMFs) Jun Zhang National Astronomical Observatories Chinese Academy of Sciences Collaborators: Sami Solanki and Jingxiu Wang.
Shock heating by Fast/Slow MHD waves along plasma loops
WG1-1: Sub-surface Structure and Evolution Motivation: A research program on space weather that ignores the sub-photospheric evolution of magnetic fields.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.
Photospheric Flows and Structures Mark Rast Laboratory for Atmospheric and Space Physics Department of Astrophysical and Planetary Sciences University.
What we can learn from active region flux emergence David Alexander Rice University Collaborators: Lirong Tian (Rice) Yuhong Fan (HAO)
Horizontal Flows in the Photosphere and the Subphotosphere in Two Active Regions Yang Liu, Junwei Zhao, Peter W. Schuck.
Axel Brandenburg & Jörn Warnecke NorditaStockholm  loop emergence –Buoyant rise –Many scale heights –Twist needed Dynamo –bi-helical field Emergence.
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
THE DYNAMIC EVOLUTION OF TWISTED MAGNETIC FLUX TUBES IN A THREE-DIMENSIONALCONVECTING FLOW. II. TURBULENT PUMPING AND THE COHESION OF Ω-LOOPS.
Helicity Thinkshop 2009, Beijing Asymmetry of helicity injection in emerging active regions L. Tian, D. Alexander Rice University, USA Y. Liu Yunnan Astronomical.
Numerical Simulations of Solar Magneto-Convection
Ward Manchester University of Michigan
Solar Surface Magneto-Convection and Dynamo Action
Solar Wind and CMEs with the Space Weather Modeling Framework
Magnetic Helicity in Emerging Active Regions: A Statistical Study
October 14, Wednesday 12. Solar Convection
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
Wave heating of the partially-ionised solar atmosphere
From the Convection Zone to the Heliosphere
Helioseismic data from Emerging Flux & proto Active Region Simulations
Introduction to Space Weather
Preflare State Rust et al. (1994) 太陽雑誌会.
Supergranule Scale Convection Simulations
Presentation transcript:

Simulation of Flux Emergence from the Convection Zone Fang Fang 1, Ward Manchester IV 1, William Abbett 2 and Bart van der Holst 1 1 Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI Space Sciences Laboratory, University of California, Berkeley, CA 94720

2 Flux Emergence WorkshopAug 23rd, 2011 Outline Introduction Simulation Steps Results – Coupling of the Magnetic Flux and Convective Flows Vertical Flows Horizontal Flows – Magnetic Flux Cancellation – Magnetic and Energy Fluxes Conclusions

3 Flux Emergence WorkshopAug 23rd, 2011 Emergence of Solar Magnetic Flux Parnell et al The power-law distribution implies that either all surface magnetic features are generated by the same mechanism, or that they are dominated by surface processes leading to a scale- free distribution.

4 Flux Emergence WorkshopAug 23rd, 2011 MHD Equations Solve modified MHD equations with BATSRUS Q e : Energy source term, including radiative cooling and coronal heating (Abbett 2007) Tabular Equation of State (Rogers 2000) Closed Lower Boundary

5 Flux Emergence WorkshopAug 23rd, 2011 Simulation Domain Vertical stratification of density and temperature Domain of 30×30×42 Mm 3 With 56 million cells Flux Rope

6 Flux Emergence WorkshopAug 23rd, 2011 Convection Zone Convective granules with dimension of 1 Mm, upflowing speed of 1 km/s Intergranular plasma with downflowing speed of 2 km/s The movie above shows the 1-hour evolution of the structure of Uz at the photosphere.

7 Flux Emergence WorkshopAug 23rd, 2011 Initial Magnetic Flux Rope Initial flux rope at Z = -10 Mm surrounded by downflowing (blue) and upflowing (red) plasma.

8 Flux Emergence WorkshopAug 23rd, 2011 Outline Introduction Simulation Steps Results – Coupling of the Magnetic Flux and Convective Flows Vertical Flows In the convection zone In the near-surface layers

9 Flux Emergence WorkshopAug 23rd, 2011 Emergence of the Magnetic Flux The movie shows the structure of Bx on the X = 0 plane, the cross-section cut of the flux rope. The flux rope approaches the photosphere at 2.5 hours after the initialization.

10 Flux Emergence WorkshopAug 23rd, 2011 The Emerged Flux Rope

11 Flux Emergence WorkshopAug 23rd, 2011 Formation of the Sunspots - 1 The large-scale downflows in the convection zone forms and maintains the bipoles. The movie shows the evolution of Uz on the Y=0 plane with lines indicating the magnetic field lines.

12 Flux Emergence WorkshopAug 23rd, 2011 Formation of the Sunspots - 2 3D magnetic field lines colored by the local Uz.

13 Flux Emergence WorkshopAug 23rd, 2011 Convective Collapse - 1 Convective Collapse Uz at t = 4:50:00 Bz at t = 4:50:00Bz at t = 5:22:00

14 Flux Emergence WorkshopAug 23rd, 2011 Convective Collapse - 2 Downward flows produces a bulb of plasma with lower temperature, leading to a pressure imbalance with the surrounding plasma. The flux tube collapses as a result of the pressure imbalance and equilibrates with higher magnetic field up to 2 kG. The movie shows the evolution of Bz on the Y=0 plane with lines indicating the magnetic field lines.

15 Flux Emergence WorkshopAug 23rd, 2011 Outline Introduction Simulation Steps Results – Coupling of the Magnetic Flux and Convective Flows Vertical Flows Horizontal Flows Separating motion of the bipoles Rotation of the magnetic pores Shearing motion along the PILs

16 Flux Emergence WorkshopAug 23rd, 2011 Coalescence at the photosphere The movie shows the structure of Bz field with arrows representing the horizontal velocity field. The coalescence of the small-scale fluxes into the major pores facilitates the accumulation of the magnetic flux on the surface and therefore the formation of the large pores.

17 Flux Emergence WorkshopAug 23rd, 2011 Rotation of the Sunspots at the Photosphere The movie above shows the structure of Bz at the phtosphere, with arrows representing the horizontal velocity field. The positive pore shows highly sheared flows and magnetic field lines. The negative pore presents a coherent rotation.

18 Flux Emergence WorkshopAug 23rd, 2011 Horizontal flow in Convection Zone The movie above shows Bz structure at z = -3 Mm with arrows representing the horizontal velocity field. Large scale horizontal converging flow constrains the total area of the emerged flux and prevents the pores from separation. The negative polarity also shows a coherent pattern of rotation at Z= -3 Mm.

19 Flux Emergence WorkshopAug 23rd, 2011 Depth of the Rotation of Sunspot The movie shows Uy on X-Z plane with black lines showing the magnetic field lines. The coherent rotation starts to extend downward at t = 4 hrs and approaches the depth of 10 Mm in 0.5 hours. The negative polarity shows a very coherent pattern of rotation, while on the positive pore on the left, the rotation is not obvious.

20 Flux Emergence WorkshopAug 23rd, 2011 Lorentz Force Uy at t = 4:21:00 Uy at t = 5:13:00By at t = 5:13:00

21 Flux Emergence WorkshopAug 23rd, 2011 Horizontal Motion in the Corona The movies show the structure of Bz field with arrows representing the horizontal velocity field (left) and magnetic field (right) in corona.

22 Flux Emergence WorkshopAug 23rd, 2011 Magnetic Flux Total Initial Axial Flux : 1.52  Mx Z = -3 Mm:  max = 1.32  Mx (87%) Z = 0 Mm:  max = 6.85  Mx (45%) Z = 3 Mm:  max = 4.13  Mx (27%) Temporal evolution of the total magnetic fluxes

23 Flux Emergence WorkshopAug 23rd, 2011 Magnetic and Energy Fluxes Energy flux associated with horizontal motions dominates in the energy transfer from convection zone into the corona. At photosphere, the total energy transport is 7  ergs in 8 hrs. The magnetic flux emerges at the surface as bipoles with upflowing motion, then they are quickly pulled apart by the horizontal flows, and concentrate in the downdrafts.

24 Flux Emergence WorkshopAug 23rd, 2011 Large-Scale Flux Cancellation At time t=5 hours, two opposite polarities are pushed together by the horizontal flow. The convergence of these two polarities can produce highly-sheared magnetic field structure, strong gradient of magnetic field strength, and maybe shearing flow. The movie shows the evolution of photospheric Bz field with arrows representing the horizontal velocity field.

25 Flux Emergence WorkshopAug 23rd, 2011 Transverse Field during Flux Cancellation Wang et al The transverse magnetic field intensifies along the PIL after the flux cancellation.

26 Flux Emergence WorkshopAug 23rd, 2011 Conclusions The simulation illustrates the features during the flux emergence: o Dipoles are formed and maintained by the downflow drafts in the deep convection zone. o Sunspot rotation driven by Lorentz force is observed both at the photosphere and in the convection zone. The energy flux into the coronal is mainly dominated by fluxes associated with the horizontal (shearing and rotating) motion.

27 Flux Emergence WorkshopAug 23rd, 2011 References Abbett, W. P. 2007, ApJ, 665, 1469 Parnell, C. E., DeForest, C. E., Hagenaar, H. J., Johnston, B. A., Lamb, D. A., & Welsch, B. T. 2009, ApJ, 698, 75 Rogers, F. J. 2000, Physics of Plasmas, 7, 51 Wang, S., Liu, C., Liu, R., Deng, N., Liu, Y., & Wang, H. 2011, ArXiv e-prints