Feb. 2006HMI/AIA Science Team Mtg.1 Determining the 3D Magnetic Field Geometry A. A. van Ballegooijen, E. E. DeLuca, M. Bobra Smithsonian Astrophysical.

Slides:

Advertisements

Similar presentations

Observations and Magnetic Field Modeling of CMEs’ Source Regions Yingna Su Harvard-Smithsonian Center for Astrophysics Collaborators: Adriaan van Ballegooijen,

Advertisements

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

Observations and NLFFF Modeling of AR Yingna Su 1,2 Collaborators: A. A. Van Ballegooijen 1, E. E. Deluca 1, Leon Golub 1 P. Grigis 1, B. Lites 3,

Jan 13, 2009ISSI1 Modeling Coronal Flux Ropes A. A. van Ballegooijen Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, U.S.A Collaborators:

A Multi-Wavelength View of an Active Region Structure around a Filament Channel L. Lundquist, 1 K. Reeves, 1 A. van Ballegooijen, 1 T. Sakao, 2 and the.

Sigmoidal Active Regions on the Sun: Statistical and Detailed Studies Lily Hanson Advisors: Ed DeLuca and Antonia Savcheva

The Sun’s Dynamic Atmosphere Lecture 15. Guiding Questions 1.What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere.

The Relation between Filament Skew Angle and Magnetic Helicity of Active Regions Masaoki HAGINO, Y.J. MOON (Korea Astronomy and Space Science Institute)

Free Magnetic Energy and Flare Productivity of Active Regions Jing et al. ApJ, 2010, April 20 v713 issue, in press.

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

Comparison of NLFFF Extrapolations for Chromospheric and Photospheric Magnetograms of AR J. McTiernan SSL/UCB SHINE 2005 Workhsop.

Connections Between the Magnetic Carpet and the Unbalanced Corona: New Monte Carlo Models Steven R. Cranmer & Adriaan van Ballegooijen Harvard-Smithsonian.

Vincent Surges Advisors: Yingna Su Aad van Ballegooijen Observations and Magnetic Field Modeling of a flare/CME event on 2010 April 8.

SHINE The Role of Sub-Surface Processes in the Formation of Coronal Magnetic Flux Ropes A. A. van Ballegooijen Smithsonian Astrophysical Observatory.

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

NJIT-seminar Newark, NJITWiegelmann et al: Nonlinear force-free fields 1 Nonlinear force-free extrapolation of coronal magnetic.

Magnetic Field Extrapolations And Current Sheets B. T. Welsch, 1 I. De Moortel, 2 and J. M. McTiernan 1 1 Space Sciences Lab, UC Berkeley 2 School of Mathematics.

SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no. C9] HMI/AIA science teams meeting; Monterey; Feb

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

Preliminary Results from Nonlinear Field Extrapolations using Hinode Boundary Data Marc DeRosa (LMSAL), on behalf of the NLFFF Team* WG1 ~ SHINE 2007 *Karel.

Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.

SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no.] HMI/AIA science teams meeting; Monterey; Feb

Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,

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.

Nonlinear Force-Free Field Modeling AIA/HMI Science Team Meeting Session C2 14 February 2006 Marc DeRosa on behalf of the “NLFFF Consortium” (Karel Schrijver,

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

Free Magnetic Energy in Solar Active Regions above the Minimum-Energy Relaxed State (Regnier, S., Priest, E.R ApJ) Use magnetic field extrapolations.

Modeling the Dynamic Evolution of the Solar Atmosphere: C4: HMI-AIA Team Meeting: Bill Abbett SSL, UC Berkeley.

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

SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps C4/C6/M8HMI/AIA science teams meeting; Monterey; Feb I: C4/C6/M8:

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

EUV vs. B-field Comparisons Yingna Su Smithsonian Astrophysical Observatory Coauthours: Leon Golub, Aad Van Ballegooijen, Maurice Gros. HMI/AIA Science.

Direct Evidence of Emergence of a Helical Flux Rope under an Active- Region Prominence Joten Okamoto Kyoto Univ. ／ NAOJ JSPS Research Fellow Saku Tsuneta,

SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps C4/C6/M8HMI/AIA science teams meeting; Monterey; Feb I: C4/C6/M8:

1 What is the best way to use the chromospheric field information in coronal field extrapolation? Current state of art are nonlinear force-free extrapolations.

Instrumental & Technical Requirements. Science objectives for helioseismology Understanding the interaction of the p-mode oscillations and the solar magnetic.

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.

Observing the Sun. Corona: EUV; X-rays Chromosphere: H , UV, EUV Photosphere: near UV, Visible light, infra-red.

Extrapolation of magnetic fields

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

1Yang Liu/Magnetic FieldHMI Science – 1 May 2003 Magnetic Field Goals – magnetic field & eruptive events Yang Liu Stanford University.

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

1 3D Sun Loop Trace: A Tool for Stereoscopy of Coronal Loops for STEREO Jean Lorre Jeff Hall Paulett Liewer Parth Sheth Eric DeJong Jet Propulsion Laboratory.

Helicity Condensation: The Origin of Coronal/Heliospheric Structure S. K. Antiochos, C. R. DeVore, et al NASA/GSFC Key features of the corona and wind.

Flare Energy Build-Up in a Decaying Active Region Near a Coronal Hole Yingna Su Smithsonian Astrophysical Observatory Collaborators: A. A. van Ballegooijen,

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.

SDO-meeting Napa, Wiegelmann et al: Nonlinear force-free fields 1 Nonlinear force-free field modeling for SDO T. Wiegelmann, J.K. Thalmann,

Karen Meyer University of St Andrews Scotland 1 st year PhD student (3 months in)

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.

Observations and nonlinear force-free field modeling of active region Y. Su, A. van Ballegooijen, B. W. Lites, E. E. DeLuca, L. Golub, P. C. Grigis,

SHINE Formation and Eruption of Filament Flux Ropes A. A. van Ballegooijen 1 & D. H. Mackay 2 1 Smithsonian Astrophysical Observatory, Cambridge,

Scientific Interests in OVSA Expanded Array Haimin Wang.

Observations and Magnetic Field Modeling of the Flare/CME Event on 2010 April 8 Yingna Su Bernhard Kliem, Adriaan van Ballegooijen, Vincent Surges, Edward.

Observations –Morphology –Quantitative properties Underlying Physics –Aly-Sturrock limit Present Theories/Models Coronal Mass Ejections (CME) S. K. Antiochos,

Figure 5: Active regions have a complex magnetic structure consisting of multiple manetic flux systems separated by quasi-separatrix layers, or QSLs (Démoulin.

Data-constrained Simulation of CME Initiation and Propagation Antonia Savcheva ESPM 2014 September 11, 2014 Collaborators: R. Evans, B. van der Holst,

Considerations on using Solar-B observations to model the coronal field over active regions Karel Schrijver, Marc DeRosa, Ted Tarbell SOT-17 Science Meeting;

Coronal Magnetic Field – Force-Free Field and Topology CSI 769 / ASTR 769 Lect. 04, Feb. 14 Spring 2008 References: Aschwanden: Chap. 5.3 – 5.6 Articles:

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

Observations and NLFFF Modeling of AR Yingna Su 1,2 Collaborators: A. A. Van Ballegooijen 1, E. E. Deluca 1, Leon Golub 1 P. Grigis 1, B. Lites 3,

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

Observations of Filament Channels by Hinode/XRT and STEREO

Investigating a complex X-class flare using NLFFF modeling

NLFFF Energy Measurement of AR8210

Vector polarimetry with HMI

Scientific Collaboration of NAOC Facilities & Solar-B

Presentation transcript:

Feb. 2006HMI/AIA Science Team Mtg.1 Determining the 3D Magnetic Field Geometry A. A. van Ballegooijen, E. E. DeLuca, M. Bobra Smithsonian Astrophysical Observatory Cambridge, MA

Feb. 2006HMI/AIA Science Team Mtg.2 Field Extrapolation AIA Objective #1 (energy input, storage, and release) requires knowledge of 3D coronal magnetic structure and dynamics. One approach is to “extrapolate” observed vector fields into the corona, using nonlinear force free field (NLFFF) modeling: Practical difficulties: nonlinear problem limited sensitivity of B trans 180-degree ambiguity photosphere is not force free (Bt-phot ≠ Bt-corona) At present, there is no good method for extrapolating strongly sheared fields.

Feb. 2006HMI/AIA Science Team Mtg.3 Developing Extrapolation Methods Extrapolating photospheric vector fields does not work well for filament channels where sheared field is “elevated” into chromosphere. Need observational constraints on chromospheric fields. Need to include non-force-free photospheric conditions into models. Test case (see poster): -- Add vertical force at z = 2 Mm to simulate non-force-free condition. -- Construct 3D model (“A”) with the highly sheared field. -- Extract “observed” chromospheric vector field (z = 4 Mm). -- Reconstruct 3D field (“B”) by extrapolating chromospheric field (uses magneto-frictional relaxation and injection of horizontal field at z = 0 based on the error ΔB = B obs – B model in chromosphere). -- Method gives a good fit to “observed” vector field.

Feb. 2006HMI/AIA Science Team Mtg.4 Developing Extrapolation Methods Test case: chromospheric vector field (blue=“observed”, black=model) A: B: BBSO+MDI, 2005/10/10, 17:30UT

Feb. 2006HMI/AIA Science Team Mtg.5 Use H-alpha Fibrils?

Feb. 2006HMI/AIA Science Team Mtg.6 NLFFF Modeling Tasks Develop methods/codes for extrapolating vector fields in spherical geometry, covering large area on the Sun (reduce the effects of side boundaries); models must extend to large height ~ 2.5 Rsun. Develop methods for including observational constraints on chromospheric fields and effects of non-force-free photosphere. Test NLFFF methods/codes using synthetic vector-field data. Test NLFFF models using TRACE data. Can models reproduce the observed coronal loop structures? Develop quantitative methods for comparing 3D models with observed coronal loops and Hα filaments.