Reconnection of Loops and Open Field Lines

Slides:



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

The Hemispheric Pattern of Filaments and Consequences for Filament Formation Duncan H Mackay Solar Physics Group University of St. Andrews.
The Independency of Stellar Mass-Loss Rates on Stellar X-ray Luminosity and Activity Space Telescope Science Institute – 2012.
Agenda: Here comes the sun April 10 1.Learning Target: I can make a presentation of one aspect of solar study to teach other astronomers about the sun.
1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.
Using HMI to Understand Flux Cancellation by Brian Welsch 1, George Fisher 1, Yan Li 1, and Xudong Sun 2 1 Space Sciences Lab, UC-Berkeley, 2 Stanford.
The Sun Astronomy 311 Professor Lee Carkner Lecture 23.
Synoptic maps and applications Yan Li Space Sciences Laboratory University of California, Berkeley, CA HMI team meeting, Jan 27, 2005, Stanford.
Reconstructing Active Region Thermodynamics Loraine Lundquist Joint MURI Meeting Dec. 5, 2002.
Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.
Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,
Using HMI to Understand Flux Cancellation by Brian Welsch 1, George Fisher 1, Yan Li 1, and Xudong Sun 2 1 Space Sciences Lab, UC-Berkeley, 2 Stanford.
Helicity as a Component of Filament Formation D.H. Mackay University of St. Andrews Solar Theory Group.
Solar Wind Model at LMSAL AIA/HMI Science Team Meeting Session S3 15 February 2006 Marc DeRosa.
Distinguishing Eruptive from Non-Eruptive Solar Active Regions Manolis K. Georgoulis JHU/APL Johns Hopkins Rd., Laurel, MD Durham, NH, 06/27/06.
1 Pedagogical Review on Solar Cycles King-Fai Li Caltech GPS, YL Yung Group Jan 17, 2007.
Chapter 32 Maxwell’s Equations # “Magnetism of Matter” skipped.
1. Background2. Flux variation3. Polarity reversal4. Electron evolution5. Conclusions The role of coronal mass ejections in the solar cycle evolution of.
Prediction on Time-Scales of Years to Decades Discussion Group A.
Physics of fusion power
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
Kinematics and coronal field strength of an untwisting jet in a polar coronal hole observed by SDO/AIA H. Chen, J. Zhang, & S. Ma ILWS , Beijing.
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.
1 Magnetostatics. 2 If charges are moving with constant velocity, a static magnetic (or magnetostatic) field is produced. Thus, magnetostatic fields originate.
Synchronic Magnetic Maps - the Inner Boundary Condition for the Heliosphere David Hathaway NASA Marshall Space Flight Center 2011 August 2 – Space Weather.
CSI /PHYS Solar Atmosphere Fall 2004 Lecture 09 Oct. 27, 2004 Ideal MHD, MHD Waves and Coronal Heating.
SLIDE SHOW 3 B changes due to transport + diffusion III -- * * magnetic Reynold number INDUCTION EQUATION B moves with plasma / diffuses through it.
The Solar Orbiter mission Solar Orbiter represents a new approach to solar studies. –A huge increase in discovery space The payload consists of a suite.
Conclusions Using the Diffusive Equilibrium Mapping Technique we have connected a starting point of a field line on the photosphere with its final location.
Sun is NOT a normal gas B and plasma -- coupled (intimate, subtle) behaves differently from normal gas: 2. MHD Equations Sun is in 4th state of matter.
Magnetohydrodynamic simulations of stellar differential rotation and meridional circulation (submitted to A&A, arXiv: ) Bidya Binay Karak (Nordita.
Recent Progress in Understanding The Sun’s Magnetic Dynamo David H. Hathaway NASA/MSFC National Space Science and Technology Center 2004 April 28 University.
II. MAGNETOHYDRODYNAMICS (Space Climate School, Lapland, March, 2009) Eric Priest (St Andrews)
Modeling the Sun’s global magnetic field Karel Schrijver SHINE 2006 "[The] most important attitude is to find which forgotten physical processes are responsible.
Evolution of Magnetic Fields from the Sun’s Surface to the Heliopause of one Solar Cycle Nathan Schwadron, Boston University.
Electromagnetic Induction. Induced current/emf(voltage) Current or voltage produced by a changing magnetic field.
Physics 681: Solar Physics and Instrumentation – Lecture 22 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.
Solar Magnetic Field Reversal V J Pizzo SHINE Workshop August 18, 2002.
Variability of the Heliospheric Magnetic Flux: ICME effects S. T. Lepri, T. H. Zurbuchen The University of Michigan Department of Atmospheric, Oceanic,
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.
Solar Wind Helium Abundance and the Minimum Speed of the Solar Wind
What we can learn from active region flux emergence David Alexander Rice University Collaborators: Lirong Tian (Rice) Yuhong Fan (HAO)
Diary of a Wimpy Cycle David H. Hathaway 1 and Lisa Upton 2,3 1 NASA/Marshall Space Flight Center/Science Research Office 2 Vanderbilt University 3 University.
Solar Activity Level Estimation and Solar Activity Prediction Xin Huang Huaning Wang Liyun Zhang
SOHO/ESA/NASA Solar cycle - modeling and predicting Petri Käpylä NORDITA AlbaNova University Center Stockholm, Sweden Stockholm, 2nd Feb 2007 SST NASA.
CME rate: 1/3 (4) day -1 at solar min (max) [LASCO CME catalogue. Yahsiro et al., 2005] |B| at 1 AU: 5 (8) nT at solar min (max) [OMNI data] D (fraction.
Time-Dependence (structuring) of the Alpha-to-Proton Ratio (A He ) in the Solar Wind at 1 AU: Initial results, Implications, and Speculations Harlan E.
Magnetic Reconnection in Solar Flares
Nicholeen Viall NASA/GSFC
The Sun Essential Question: What are the properties of the Sun?
Determination of the North-South Heliospheric Magnetic Field from Inner-Corona Closed-Loop Propagation B.V. Jackson Center for Astrophysics and Space Sciences,
Ward Manchester University of Michigan
The Magnetosphere Feifei Jiang, UCLA
Predictions for solar cycle 25
K. Galsgaard1, A.L. Haynes2, C.E. Parnell2
Magnetic Induction Review of Chapter 22.
October 14, Wednesday 12. Solar Convection
Solar cycle variation of the heliospheric magnetic field
From the Convection Zone to the Heliosphere
Induction Equation Diffusion term Advection term
Introduction to Space Weather
How does the solar atmosphere connect to the inner heliosphere?
MDI Global Field & Solar Wind
The Sun Chapter 17.
Deposition and Removal
Let’s look in detail at each of these four ways of using flux change or motion to produce an emf. Method 1…
Electromagnetic Induction
Taiyou Zasshikai on May 17, 2004
Magnetic fields in ADs Magnetic “flux tube”.
Presentation transcript:

Reconnection of Loops and Open Field Lines

Wang, J. -M. ,, J. Lean, and N. R. Sheeley, Jr Wang, J.-M.,, J. Lean, and N. R. Sheeley, Jr., The long-term variation of the Sun’s open magnetic flux, Geophys. Res. Lett., 27, 505-508, 2000.

Heliospheric Current Sheet

Location of Current Sheet During Solar Cycle Sanderson et al. 2001.

Interchange Reconnection

Diffusion through Reconnection Recently reconnected fieldline, in motion

Transport Equation Open magnetic flux, Bopen (the number of open field lines per unit of surface area) u is the convection velocity, e.g. due to differential rotation.

Diffusion Terms Diffusion due to convective motions: dh is the length of a lane; dt is the time for convection along dh. Diffusion due to reconnection with loops: is the mean squared loop length; t is the characteristic reconnection time; Bloop is the average magnetic field strength in loops. Diffusion due to reconnection in the canopy: kcanopyBopen