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

Slides:



Advertisements
Similar presentations
2006/4/17-20 Extended 17 th SOT meeting Azimuth ambiguity resolution from dBz/dz M. Kubo (ISAS/JAXA), K. Shimada (University of Tokyo), K. Ichimoto, S.
Advertisements

Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
Study of Magnetic Helicity Injection in the Active Region NOAA Associated with the X-class Flare of 2011 February 15 Sung-Hong Park 1, K. Cho 1,
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
CME/Flare Mechanisms Solar “minimum” event this January For use to VSE must be able to predict CME/flare Spiro K. Antiochos Naval Research Laboratory.
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
The Relation between Filament Skew Angle and Magnetic Helicity of Active Regions Masaoki HAGINO, Y.J. MOON (Korea Astronomy and Space Science Institute)
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Resolving the 180 Degree Ambiguity in Vector Magnetic Fields T. Metcalf.
Coronal Boundaries of Active Regions Derived From Soft X-ray Images.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
Free Magnetic Energy: Crude Estimates by Brian Welsch, Space Sciences Lab, UC-Berkeley.
1 Chromospheric UV oscillations depend on altitude and local magnetic field Noah S. Heller and E.J. Zita, The Evergreen State College, Olympia, WA
FALL 2007CSTR Journal Club Emergence of Small-Scale Magnetic Loops in the Quiet Sun Internetwork R. Centeno, H Socas-Navarro, B. Lites, M. Kubo High Altitude.
September 2006 CISM All Hand Meeting Progress in the Past Year and Plan for Next Year Yang Liu and the Solar Group in Stanford University
Incorporating Vector Magnetic Field Measurements into MHD models of the Solar Atmosphere W.P. Abbett Space Sciences Laboratory, UC Berkeley and B.T. Welsch,
Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.
Subsurface Evolution of Emerging Magnetic Fields Yuhong Fan (HAO/NCAR) High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR)
Onset of Coronal Mass Ejection Due to Loss of Confinement of Coronal Flux Ropes Y. Fan & S.E. Gibson HAO, National Center for Atmospheric Research High.
Detecting and Tracking of Mesoscale Oceanic Features in the Miami Isopycnic Circulation Ocean Model. Ramprasad Balasubramanian, Amit Tandon*, Bin John,
Changes of Magnetic Structure in 3-D Associated with Major Flares X3.4 flare of 2006 December 13 (J. Jing, T. Wiegelmann, Y. Suematsu M.Kubo, and H. Wang,
Stokes Inversion 180  Azimuth Ambiguity Resolution Non-linear Force-free field (NLFFF) Extrapolation of Magnetic Field Progress in Setting up Data Processing.
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.
Free Magnetic Energy in Solar Active Regions above the Minimum-Energy Relaxed State (Regnier, S., Priest, E.R ApJ) Use magnetic field extrapolations.
Study of magnetic helicity in solar active regions: For a better understanding of solar flares Sung-Hong Park Center for Solar-Terrestrial Research New.
Connecting coronal structure to photospheric origins Active region (sunspot) evolution and solar rotation well define long term, persistent, coronal streamers.
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.
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
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.
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Instrumental & Technical Requirements. Science objectives for helioseismology Understanding the interaction of the p-mode oscillations and the solar magnetic.
Science Data Products – HMI Magnetic Field Images Pipeline 45-second Magnetic line-of-sight velocity on full disk Continuum intensity on full disk Vlos.
The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.
Seething Horizontal Magnetic Fields in the Quiet Solar Photosphere J. Harvey, D. Branston, C. Henney, C. Keller, SOLIS and GONG Teams.
Comparison on Calculated Helicity Parameters at Different Observing Sites Haiqing Xu (NAOC) Collaborators: Hongqi, Zhang, NAOC Kirill Kuzanyan, IZMIRAN,
Coronal Mass Ejection As a Result of Magnetic Helicity Accumulation
SHINE 2008, June 23-27, Utah Observational Test of Coronal Magnetic Field Models I. Comparison with Potential Field Model Hao-Sheng Lin & Yu Liu Institute.
Magnetic Correspondence between Moving Magnetic Features and Penumbral Magnetic Fields M. Kubo and T. Shimizu ISAS/JAXA - The 6th Solar-B Science Meeting.
SHINE SEP Campaign Events: Long-term development of solar corona in build-up to the SEP events of 21 April 2002 and 24 August 2002 A. J. Coyner, D. Alexander,
Helicity Observations by Huairou Vector Magnetograph Mei Zhang National Astronomical Observatory, Chinese Academy of Sciences Plan of the Talk: 1.Huairou.
Flare Energy Build-Up in a Decaying Active Region Near a Coronal Hole Yingna Su Smithsonian Astrophysical Observatory Collaborators: A. A. van Ballegooijen,
Azimuth disambiguation of solar vector magnetograms M. K. Georgoulis JHU/APL Johns Hopkins Rd., Laurel, MD 20723, USA Ambiguity Workshop Boulder,
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
3D Spherical Shell Simulations of Rising Flux Tubes in the Solar Convective Envelope Yuhong Fan (HAO/NCAR) High Altitude Observatory (HAO) – National Center.
Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan.
SDO-meeting Napa, Wiegelmann et al: Nonlinear force-free fields 1 Nonlinear force-free field modeling for SDO T. Wiegelmann, J.K. Thalmann,
Feb. 3-5, 20034th Solar-B science meeting1 Corona-Photosphere Connection with Spectropolarimeter Yukio Katsukawa (Univ. of Tokyo)
INCIDENCE ANGLE, θ The solar incidence angle, θ, is the angle between the sun’s rays and the normal on a surface. For a horizontal plane, the incidence.
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.
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,
COSMO Large Coronagraph Preliminary Design Review
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Scientific Interests in OVSA Expanded Array Haimin Wang.
Calibration of Solar Magnetograms and 180 degree ambiguity resolution Moon, Yong-Jae ( 文 鎔 梓 ) (Korea Astronomy and Space Science Institute)
The Helioseismic and Magnetic Imager (HMI) on NASA’s Solar Dynamics Observatory (SDO) has continuously measured the vector magnetic field, intensity, and.
SHINE 2008 Vector Magnetic Fields from the Helioseismic and Magnetic Imager Steven Tomczyk (HAO/NCAR) Juan Borrero (HAO/NCAR and MPS)
Considerations on using Solar-B observations to model the coronal field over active regions Karel Schrijver, Marc DeRosa, Ted Tarbell SOT-17 Science Meeting;
A Method for Solving 180 Degree Ambiguity in Observed Solar Transverse Magnetic Field Huaning Wang National Astronomical Observatories Chinese Academy.
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
Extrapolating Coronal Magnetic Fields T. Metcalf.
Methods for automatic processing
New Iterative Method of the Azimuth Ambiguity Resolution
Mark A. Bourassa and Qi Shi
Magnetic Flux Ropes in the Solar Photosphere: The Vector Magnetic Field under Active Region Filaments B.W.Lites the Astrophysical Journal, 622: ,2005,
S/N and Polarimetry With HMI
Vector polarimetry with HMI
Scientific Collaboration of NAOC Facilities & Solar-B
Observations of emerging and submerging regions with ASP and Solar-B
Presentation transcript:

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under sponsorship of the National Science Foundation. An Equal Opportunity/Affirmative Action Employer. Azimuth Ambiguity Resolution Workshop Introduction Bruce W. Lites High Altitude Observatory National Center for Atmospheric Research CSAC/HMI Workshop, Boulder, September September 2005

Azimuth Ambiguity Fundamentals Bruce Lites, CSAC/HMI Ambiguity Resolution Workshop, September 2005 Zeeman Effect produces linear polarization for a transverse magnetic field: Note the degeneracy of the polarization wrt the sense of the transverse field (up or down in this case).

The “local solar frame” (one axis normal to the solar surface) is the preferred reference frame for physical interpretation For fields measured away from disk center, the ambiguity of the azimuth in the observer’s frame affects both the local frame azimuth and inclination to the vertical The azimuth ambiguity must be resolved for many problems that depend on vector field measurements: Extrapolation of fields to higher layers Flux emergence and decay Active region evolution ………… Why We Concern Ourselves with the Azimuth Ambiguity

Ambiguity resolution necessitates adding more physical information to that provided by the Zeeman Effect alone. Additional information on the physical system: Field connectivity (H , X-ray, EUV, ….) Solenoidal condition  B = 0 Scattering polarization (in chromospheric lines) ….Others (add to the list at this workshop!) Ad-hoc physical assumptions: Closest approach to potential field Force-Free field assumption (currents parallel to B) Minimize vertical currents (spatial continuity) Assumptions on physical structure of field topology (e.g., plage fields usually close to vertical, orientation gradients at location of strong field gradients, …..)

Ambiguity Resolution – “There Is No Magic Bullet” As of yet, none of the class of additional physical information provides us with a reliable ambiguity resolution Some ad-hoc physical assumptions do better, but still fail in particular circumstances Ad-hoc assumptions can be patently wrong (e.g., the assumption of a force-free field in photosphere is often incorrect) Data quality and analysis techniques strongly affect the local frame azimuth, hence the ambiguity resolution Manual (human interaction) adjustment is sometimes required for any extant method (what are the assumptions involved?)

Workshop Goals (Personal View) Further our collective understanding of the methods that are available Examine the strengths and weaknesses of the methods Compare, to the extent possible, the accuracy and usefulness of available methods Assess the utility of various methods for bulk, automatic processing of data from HMI, Solar-B, SOLIS, ….. Discuss possibilities for future advances Recommend a course for further study (Another workshop? Working groups?)

Note: Agenda purposefully left open to allow ample time for discussions and comparisons.

Some Logistical Information: Proceedings: We will post all presentations and summaries on the web. Please give your presentations to Steve Tomczyk. Money: Those of you being reimbursed from NCAR for travel expenses, please see Louise Beierle at this morning’s coffee break. She will have travel vouchers, etc. for you to sign. Dinner tonight: We will break into smaller groups for dinner at various restaurants. We will meet in front of the Residence Inn at 19:00 to arrange transportation and select restaurants.