A Comparison Between Magnetic Charge Topology and Local Correlation Tracking of Solar Active Regions Joanna Bridge Montana State University Solar Physics.

Slides:



Advertisements
Similar presentations
Study of Sunspot Motion Associated with the 2006 Dec. 13 X3.4 Flare Shuo Wang Advisor: Chang Liu Haimin Wang.
Advertisements

MURI,2008 Electric Field Variability and Impact on the Thermosphere Yue Deng 1,2, Astrid Maute 1, Arthur D. Richmond 1 and Ray G. Roble 1 1.HAO National.
Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
Energy and Helicity Budget of Four Solar Flares and Associated Magnetic Clouds. Maria D. Kazachenko, Richard C. Canfield, Dana Longcope, Jiong Qiu Montana.
Colorado Research Associates Division, NorthWest Research Associates Magnetic Charge Topology (MCT) Analysis of NOAA AR8210 Graham Barnes NWRA/CoRA K.D.
Trough Figure 2. Entire trough used for sand transmission tests. Sound transmission in geological materials Mikel-Stites M. 1,2, Ulrich R. 2,3, El Shafie.
Hard X-Ray Footpoint Motion in Spectrally Distinct Solar Flares Casey Donoven Mentor Angela Des Jardins 2011 Solar REU.
Estimating Surface Flows from HMI Magnetograms Brian Welsch, SSL UC-Berkeley GOAL: Consider techniques available to estimate flows from HMI vector magnetograms,
Current sheets formation along magnetic separators in 3d Dana Longcope Montana State University Thanks: I Klapper, A.A. Van Ballegooijen NSF-ATM.
Title of Presentation Author 1, Author 2, Author 3, Author 4 Abstract Introduction This is my abstract. This is my abstract. This is my abstract. This.
+ Hard X-Ray Footpoint Motion and Progressive Hardening in Solar Flares Margot Robinson Mentor: Dr. Angela DesJardins MSU Solar Physics Summer REU, 2010.
MSU Solar Physics REU Jennifer O’Hara Heating of Flare Loops With Observationally Constrained Heating Functions Advisors Jiong Qiu, Wenjuan Liu.
Can We Determine Electric Fields and Poynting Fluxes from Vector Magnetograms and Doppler Shifts? by George Fisher, Brian Welsch, and Bill Abbett Space.
A Diachronic Topological Analysis of the 13th May 2005 Solar Flare William M.R. Simpson, Angela Des Jardins U NIVERSITY OF S T. A NDREWS, M ONTANA S TATE.
Ryan Payne Advisor: Dana Longcope. Solar Flares General  Solar flares are violent releases of matter and energy within active regions on the Sun.  Flares.
East-West Asymmetry of the Yohkoh Soft X-ray Corona L.W. Acton 1, D.E. McKenzie 1, A. Takeda 1, B.T. Welsch 2,and H.S. Hudson 2,3 1 Montana State University,
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.
One mask to group them all, One code to find them, One file to store them all, And in a structure bind them. William (Tolkien) Simpson m.
HMI & Photospheric Flows 1.Review of methods to determine surface plasma flow; 2.Comparisons between methods; 3.Data requirements; 4.Necessary computational.
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.
FLUX CANCELLATION IN PROMINENCE FORMATION Piet Martens Montana State University, Bozeman, MT, USA & Paul Wood University of St Andrews, Fife, Scotland.
Nonlinear Force Free Field Models for AR J.McTiernan, H.Hudson (SSL/UCB) T.Metcalf (LMSAL)
Free Energies via Velocity Estimates B.T. Welsch & G.H. Fisher, Space Sciences Lab, UC Berkeley.
Determining flows from magnetic field evolution An outline of the approach we’ve adopted at UCB (Welsch, Fisher, Abbett, Regnier)
Inductive Local Correlation Tracking or, Getting from One Magnetogram to the Next Goal (MURI grant): Realistically simulate coronal magnetic field in eruptive.
1 Synoptic Maps of Magnetic Field from MDI Magnetograms: polar field interpolation. Y. Liu, J. T. Hoeksema, X. P. Zhao, R. M. Larson – Stanford University.
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,
Coronal Holes Not As Well Behaved As We Thought Dustin Hickey Colby College ‘11 Montana State University Solar REU Program Advisor: Dana Longcope August.
Summary of workshop on AR May One of the MURI candidate active regions selected for detailed study and modeling.
LCT Active Region Survey: Preliminary Results We proposed to calculate LCT flows (Li et al. 2004, Welsch et al., 2004) in N > 30 ARs, some of which produced.
Magnetogram Evolution Near Polarity Inversion Lines Brian Welsch and Yan Li Space Sciences Lab, UC-Berkeley, 7 Gauss Way, Berkeley, CA , USA.
Measuring, Understanding, and Using Flows and Electric Fields in the Solar Atmosphere to Improve Space Weather Prediction George H. Fisher Space Sciences.
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.
On the Origin of Strong Gradients in Photospheric Magnetic Fields Brian Welsch and Yan Li Space Sciences Lab, UC-Berkeley, 7 Gauss Way, Berkeley, CA ,
Flows and the Photospheric Magnetic Field Dynamics at Interior – Corona Interface Brian Welsch, George Fisher, Yan Li, & the UCB/SSL MURI & CISM Teams.
Study of magnetic helicity in solar active regions: For a better understanding of solar flares Sung-Hong Park Center for Solar-Terrestrial Research New.
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
V.I. Abramenko, V.B. Yurchyshyn, H. Wang, T.R. Spirock, P.R. Goode Big Bear Solar Observatory, NJIT Crimean Astrophysical Observatory, Ukraine
Finding the Flow Field Need flow information! –ideal evolution of coronal B(x,y,z,t) determined entirely by B(x,y,z,0) and v(x,y,0) – get v wrong and get.
2002 May 1MURI VMG mini-workshop1` Solar MURI Vector Magnetogram Mini-Workshop Using Vector Magnetograms in Theoretical Models: Plan of Action.
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.
Graph-based consensus clustering for class discovery from gene expression data Zhiwen Yum, Hau-San Wong and Hongqiang Wang Bioinformatics, 2007.
Image Renaissance Using Discrete Optimization Cédric AllèneNikos Paragios ENPC – CERTIS ESIEE – A²SI ECP - MAS France.
UNDERSTANDING DYNAMIC BEHAVIOR OF EMBRYONIC STEM CELL MITOSIS Shubham Debnath 1, Bir Bhanu 2 Embryonic stem cells are derived from the inner cell mass.
Comparison on Calculated Helicity Parameters at Different Observing Sites Haiqing Xu (NAOC) Collaborators: Hongqi, Zhang, NAOC Kirill Kuzanyan, IZMIRAN,
MRI Image Segmentation for Brain Injury Quantification Lindsay Kulkin BRITE REU 2009 Advisor: Bir Bhanu August 20, 2009.
Calculating Magnetic Energy in Active Regions Using Coronal Loops for AR and AR Presentation by, Joseph B. Jensen.
Practical Calculation of Magnetic Energy and Relative Magnetic Helicity Budgets in Solar Active Regions Manolis K. Georgoulis Research Center for Astronomy.
Analysis Magnetic Reconnection in Solar Flares: the Importance of Spines and Separators Angela Des Jardins 1, Richard Canfield 1, Dana Longcope 1, Emily.
Gesture Recognition in a Class Room Environment Michael Wallick CS766.
Is there any relationship between photospheric flows & flares? Coupling between magnetic fields in the solar photosphere and corona implies that flows.
Evolutionary Characteristics of Magnetic Helicity Injection in Active Regions Hyewon Jeong and Jongchul Chae Seoul National University, Korea 2. Data and.
Horizontal Flows in Active Regions from Multi-Spectral Observations of SDO Sushant Tripathy 1 Collaborators K. Jain 1, B. Ravindra 2, & F. Hill 1 1 National.
1 Yongliang Song & Mei Zhang (National Astronomical Observatory of China) The effect of non-radial magnetic field on measuring helicity transfer rate.
Comparison of Heliospheric Magnetic Flux from Observations and the SAIC MHD Model S. T. Lepri, The University of Michigan S. K. Antiochos, Naval Research.
A Topological Analysis of the Magnetic Breakout Model by Rhona Maclean University of St Andrews 10 th August 2004 Collaborators: Colin Beveridge, Dana.
Sweet Solar SAP: Boiling Down the Thermal Energy Content of Supra-Arcade Plasma Ashley Armstrong Advisor: Dr. Kathy Reeves Solar REU Summer 2012.
Helicity Thinkshop 2009, Beijing Asymmetry of helicity injection in emerging active regions L. Tian, D. Alexander Rice University, USA Y. Liu Yunnan Astronomical.
Hyewon Jeong, Jongchul Chae Seoul National University
MDI Level 1.8 Magnetograms
New Iterative Method of the Azimuth Ambiguity Resolution
Magnetic Topology of the 29 October 2003 X10 Flare
M.Sc. Project Doron Harlev Supervisor: Dr. Dana Ron
For a given CA II K-line index there are too few sunspots after 2000
Magnetic Configuration and Non-potentiality of NOAA AR10486
The Image The pixels in the image The mask The resulting image 255 X
Measurements of lifetimes of high-l solar p-modes in sunspots
Presentation transcript:

A Comparison Between Magnetic Charge Topology and Local Correlation Tracking of Solar Active Regions Joanna Bridge Montana State University Solar Physics REU Program August 2010 Advisors: Lucas Tarr, Dr. Dana Longcope

Presentation Overview Introduction to solar magnetic fields Developing an approach to partitioning and tracking active regions Current methods for tracking active region movement Comparing methodologies Conclusions and impacts of this research

Magnetograms depict line of sight solar magnetic fields

MDI images were taken at 96 minute intervals To track active regions, a mask is created that partitions subregions of flux Potential problems: Over several days, regions tend to disappear and reappear from time to time Labels switch seemingly arbitrarily

A reliable algorithm for pole consistency was developed

Three algorithms were used to smooth unruly data In the end, only two of the original three functions for cleaning up poles were retained Some hand-fixing of labels was required

Local Correlation Tracking (LCT) is the current method for tracking regions LCT tracks movement of individual pixels of magnetograms to determine velocities Potential problems: Underestimation of areas of stronger flux Overemphasis on weaker flux regions

Creating the mask currently relies on LCT Mask regions have commonly been generated starting with the final LCT velocity fields and advecting back to the initial mask Using this mask to analyze the effectiveness of LCT begs the question since the mask was found using LCT to begin with Our method for creating the mask depends entirely on tessellation algorithms instead of LCT, allowing for both analysis of LCT and our method

 MCT is used to approximate the flux regions as flux- weighted centroids  The mask is generated from these sources Magnetic Charge Topology (MCT) tracks source movement

Velocities can be determined by tracking pole movement Centroid velocities: [x(i+1) - x(i)] / [time(i+1) - time(i)]

Comparison between MCT and LCT showed a high degree of correlation

Further analysis confirms this agreement between the two methods

Conclusions/Impacts Finding a repeatable algorithm to create masks not using LCT is feasible and effective Comparison of LCT and MCT allows for confirmation of the validity of both methods Where MCT does not match LCT, there is a reasonable explanation for it Tracking movement of active regions comes into play in energy storage and helicity calculations

Thank you!  Acknowledgments:  Lucas Tarr  Dana Longcope  NSF  The entire solar physics group here at MSU  My cohorts here this summer