2002 May 1MURI VMG mini-workshop1` Solar MURI Vector Magnetogram Mini-Workshop Using Vector Magnetograms in Theoretical Models: Plan of Action.

Slides:

Advertisements

Similar presentations

Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.

Advertisements

Time Series of Magnetograms: Evolution, Interpretations, Inferring Flows G. Fisher, Y. Li, B. Welsch.

Inductive Flow Estimation for HMI Brian Welsch, Dave Bercik, and George Fisher, SSL UC-Berkeley.

The Magnetic & Energetic Connection Between the Photosphere & Corona Brian Welsch, Bill Abbett, George Fisher, Yan Li, Jim McTiernan, et al. Why do we.

Can We Determine Electric Fields and Poynting Fluxes from Vector Magnetograms and Doppler Shifts? by George Fisher, Brian Welsch, and Bill Abbett Space.

Resolving the 180 Degree Ambiguity in Vector Magnetic Fields T. Metcalf.

SHINE Campaign Event: 1-2 May 1998 Brian Welsch (& Yan Li) Space Sciences Laboratory, UC Berkeley Introduction: Data, Context, etc. Work: Completed & Ongoing.

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.

1 A New Technique for Deriving Electric Fields from Sequences of Vector Magnetograms George H. Fisher Brian T. Welsch William P. Abbett David J. Bercik.

Local Data-driven MHD Simulations of Active Regions W.P. Abbett MURI 8210 Workshop Mar 2004.

Estimating Electric Fields from Sequences of Vector Magnetograms George H. Fisher, Brian T. Welsch, William P. Abbett, and David J. Bercik University of.

HMI & Photospheric Flows 1.Review of methods to determine surface plasma flow; 2.Comparisons between methods; 3.Data requirements; 4.Necessary computational.

A General Cone Model Approach to Heliospheric CMEs and SEP Modeling Magnetogram-based quiet corona and solar wind model The SEPs are modeled as a passive.

M3 Session AIA/HMI Science Meeting D-1 : M3-Magnetic Field Data Products Data Product Development Session Chairs: R. Larsen/Y. Liu Status: [draft]

HMI – Synoptic Data Sets HMI Team Meeting Jan. 26, 2005 Stanford, CA.

Free Magnetic Energy: Crude Estimates by Brian Welsch, Space Sciences Lab, UC-Berkeley.

MSU Team: R. C. Canfield, D. W. Longcope, P. C. H. Martens, S. Régnier Evolution on the photosphere: magnetic and velocity fields 3D coronal magnetic fields.

1 SDO/HMI Products From Vector Magnetograms Yang Liu – Stanford University

Estimating Electric Fields from Vector Magnetogram Sequences G. H. Fisher, B. T. Welsch, W. P. Abbett, D. J. Bercik University of California, Berkeley.

Coupled Models for the Emergence of Magnetic Flux into the Solar Corona W. P. Abbett UC Berkeley SSL G. H. Fisher, Y. Fan, S. A. Ledvina, Y. Li, and D.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Modeling Active Region Magnetic Fields on the Sun W.P. Abbett Space Sciences Laboratory University of California, Berkeley.

Tucson MURI SEP Workshop March 2003 Janet Luhmann and the Solar CISM Modeling Team Solar and Interplanetary Modeling.

Free Energies via Velocity Estimates B.T. Welsch & G.H. Fisher, Space Sciences Lab, UC Berkeley.

Incorporating Vector Magnetic Field Measurements into MHD models of the Solar Atmosphere W.P. Abbett Space Sciences Laboratory, UC Berkeley and B.T. Welsch,

Determining flows from magnetic field evolution An outline of the approach we’ve adopted at UCB (Welsch, Fisher, Abbett, Regnier)

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Inductive Local Correlation Tracking or, Getting from One Magnetogram to the Next Goal (MURI grant): Realistically simulate coronal magnetic field in eruptive.

Understanding the Connection Between Magnetic Fields in the Solar Interior and the Solar Corona George H. Fisher Space Sciences Laboratory UC Berkeley.

Estimating Free Energy in AR 8210 Acknowledgements Graham Barnes (Colarado Research Associates, NWRA) Ravi Belur (Dept. of Physics, Montana State Univ)

Finding Photospheric Flows with I+LCT or,“Everything you always wanted to know about velocity at the photosphere, but were afraid to ask.” B. T. Welsch,

1Yang Liu1997 May 12 Event The 1997 May 12 Event Yang Liu – Stanford University

Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.

Summary of workshop on AR May One of the MURI candidate active regions selected for detailed study and modeling.

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)

Measuring, Understanding, and Using Flows and Electric Fields in the Solar Atmosphere to Improve Space Weather Prediction George H. Fisher Space Sciences.

The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Flows in NOAA AR 8210: An overview of MURI progress to thru Feb.’04 Modelers prescribe fields and flows (B, v) to drive eruptions in MHD simulations MURI.

Flows and the Photospheric Magnetic Field Dynamics at Interior – Corona Interface Brian Welsch, George Fisher, Yan Li, & the UCB/SSL MURI & CISM Teams.

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Data-Driven Simulations of AR8210 W.P. Abbett Space Sciences Laboratory, UC Berkeley SHINE Workshop 2004.

Jan. 27, 2005HMI team meeting The Minimum Energy Fit The Slowest Motion Required by Induction Dana Longcope Montana State University Work supported by.

Space Weather Forecast With HMI Magnetograms: Proposed data products Yang Liu, J. T. Hoeksema, and HMI Team.

NLFFF Energy Measurement of AR8210 J.McTiernan SSL/UCB.

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.

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.

Active Region Flux Transport Observational Techniques, Results, & Implications B. T. Welsch G. H. Fisher

1 A New Technique for Deriving Electric Fields from Sequences of Vector Magnetograms George H. Fisher Brian T. Welsch William P. Abbett David J. Bercik.

B. T. Welsch Space Sciences Lab, Univ. of California, Berkeley, CA J. M. McTiernan Space Sciences.

Using Simulations to Test Methods for Measuring Photospheric Velocity Fields W. P. Abbett, B. T. Welsch, & G. H. Fisher W. P. Abbett, B. T. Welsch, & G.

Sung-Hong Park Space Weather Research Laboratory New Jersey Institute of Technology Study of Magnetic Helicity and Its Relationship with Solar Activities:

UCB MURI Team Introduction An overview of ongoing work to understand a well observed, eruptive active region, along with closely related studies…..

Summary of UCB MURI workshop on vector magnetograms Have picked 2 observed events for targeted study and modeling: AR8210 (May 1, 1998), and AR8038 (May.

Luhmann1 An NSF Science and Technology Center led by Boston University, involving solar partners at SAIC, U of Colorado, BU, HAO, Stanford, NRL, AFRL,

The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.

LINE OF SIGHT MAGNETIC FIELD EVOLUTION & DATA ANALYSIS Dandan Ye.

Frontiers in Modeling Magnetic Flux Emergence and the Development of Solar Eruptive Activities Organizers: Mark Linton and Yuhong Fan SHINE Liaison: KD.

Newark, Wiegelmann et al.: Coronal magnetic fields1 Solar coronal magnetic fields: Source of Space weather Thomas Wiegelmann, Julia Thalmann,

Practical Calculation of Magnetic Energy and Relative Magnetic Helicity Budgets in Solar Active Regions Manolis K. Georgoulis Research Center for Astronomy.

Nonlinear force-free coronal magnetic field extrapolation scheme for solar active regions Han He, Huaning Wang, Yihua Yan National Astronomical Observatories,

Coronal magnetic fields Thomas Wiegelmann, MPI for Solar-System Research, (Former: MPI für Aeronomie) Katlenburg-Lindau Why are coronal magnetic fields.

Session 10 SHINE Workshop, June 23-27, 2008 Vector Magnetic Data Input into Global Models (Session 10) Chairs: Marc DeRosa and Ilia Roussev Working Group.

WG2 Sessions SHINE Workshop, July 30–August 3, K.D. Leka: “Promises and Reality of Analysis Using Magnetic Field Data” Gave update on present and.

1 Yongliang Song & Mei Zhang (National Astronomical Observatory of China) The effect of non-radial magnetic field on measuring helicity transfer rate.

A Method for Solving 180 Degree Ambiguity in Observed Solar Transverse Magnetic Field Huaning Wang National Astronomical Observatories Chinese Academy.

SDO-meeting Napa, Wiegelmann et al: Nonlinear force-free fields 1 A brief summary about nonlinear force-free coronal magnetic field modelling.

Driving 3D-MHD codes Using the UCSD Tomography

Estimating Free Energy in AR 8210

Observations of December 2006 events

Presentation transcript:

2002 May 1MURI VMG mini-workshop1` Solar MURI Vector Magnetogram Mini-Workshop Using Vector Magnetograms in Theoretical Models: Plan of Action

2002 May 1MURI VMG mini-workshop2` Overview of the plan Phase I 1.Analyze available data for 1998 May 1 event 2.Construct coronal magnetic equilibria 3.Develop velocity inversion methods 4.Test velocity inversion methods 5.Study a second (simpler) event Phase II 1.Carry out MHD simulations 2.Couple coronal and IP codes Phase III 1.Validation of modelling using available solar and IP data

2002 May 1MURI VMG mini-workshop3` Analyze available data for 1998 May 1 event 1.Generate a sequence of IVM magnetograms for the 1998 May 1 23:40 UT halo CME event (AR 8210), time cadence ~15 min (too slow ?), before, during, and after eruption. (Regnier) 2.Estimate the magnetic field uncertainties.(Metcalf, Leka) 3.Determine line of sight and transverse velocities. (Welsch, Metcalf) 4.Analyze the global solar (Li, Liu) and IP (Li, Luhmann) context (spatial, temporal) of this event, time scale ~ several days, including previous and following events. 5.Make an instrument vs time array on WWW (Li)

2002 May 1MURI VMG mini-workshop4` Construct coronal magnetic equilibria 1.Build force-free magnetic field models for each magnetogram, combined with a potential extrapolation of MDI data. (Regnier) 2.Build magnetostatic models from the same magnetograms (Heinemann). 3.Compare force-free magnetic field models to available coronal imaging data (Canfield, Metcalf) 4.Compare connectivity of force-free models to that of point charge models (Regnier, Longcope, Leka)

2002 May 1MURI VMG mini-workshop5` Develop velocity inversion methods 1.Use vertical component of induction equation to derive velocity fields (Longcope, Fisher, Welsch) 2.Constrain the solutions by minimizing total kinetic energy (ditto)

2002 May 1MURI VMG mini-workshop6` Test velocity inversion methods 1.Generate fake magnetogram sequences from the MHD simulations (Abbett, Fisher) 2.Use velocity inversion techniques to infer velocities from these sequences (ditto + Welsch) 3.Compare photospheric boundary velocities from the simulation to those inferred from the inversion (same as 2) 4.Explore implications of magnetogram uncertainties through Monte Carlo methods (same as 2). 5.Compare velocities from the inversion to IVM observations (Welsch, Metcalf, Abbett, Fisher)

2002 May 1MURI VMG mini-workshop7` Study a second (simpler) event (Liu) 1.Identify a simpler solar and IP event for analysis (1997 May 12 halo CME in AR8038 ?). 2.Produce a vector magnetogram (Solar Flare Telescope / Mitaka ?) sequence for this event. 3.Carry out an analysis parallel to that of the 1998 May 1 event (no velocity observations available – or use LCT methods for v_t, MDI for v_l?) (Liu + Welsch)

2002 May 1MURI VMG mini-workshop8` Carry out MHD simulations Do Zeus AMR simulations using real magnetic field data near time of CME using synoptic magnetic field solutions as boundary condition. (Berkeley mafia) Couple coronal and interplanetary codes (Abbett, Ledvina, Odstrcil)