Sigmoid: A Twisted Tale of Flux and Fields By Tyler Behm Mentors: Antonia Savcheva Ed DeLuca.

Slides:

Advertisements

Similar presentations

SPD June 16, 2003 Separators: Fault Lines in the Magnetic Field Dana Longcope Montana State University.

Advertisements

Lecture 9 Prominences and Filaments Filaments are formed in magnetic loops that hold relatively cool, dense gas suspended above the surface of the Sun,"

1 A New Model of Solar Flare Trigger Mechanism Kanya Kusano (Hiroshima University) Collaboration with T.Maeshiro (Hiroshima Univ.) T.Yokoyama (Univ. of.

The magnetic nature of solar flares Paper by E.R. Priest & T.G. Forbes Review presented by Hui Song.

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.

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

A solar eruption driven by rapid sunspot rotation Guiping Ruan, Yao Chen, Shuo Wang, Hongqi Zhang, Gang Li, Ju Jing, Xing Li, Haiqing Xu, and Haimin Wang.

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:

1 Hinode Coordinated Observations: Plasma Composition Photospheric composition ~ 1 in coronal hole (CH) -> fast wind Coronal composition ~1.5-3 in active.

Active Region Evolution and the Removal of Magnetic Helicity by CMEs Len Culhane Mullard Space Science Laboratory University College London.

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

Evolution of Magnetic Helicity in the Corona During Flux Emergence Anna Malanushenko, Humed Yusuf, Dana Longcope.

Simulation of Flux Emergence from the Convection Zone Fang Fang 1, Ward Manchester IV 1, William Abbett 2 and Bart van der Holst 1 1 Department of Atmospheric,

Chip Manchester 1, Fang Fang 1, Bart van der Holst 1, Bill Abbett 2 (1)University of Michigan (2)University of California Berkeley Study of Flux Emergence:

Modelling the Global Solar Corona: Filament Chirality Anthony R. Yeates and Duncan H Mackay School of Mathematics and Statistics, University of St. Andrews.

Jonathan A. Constable University of St Andrews Solar REU Presentation 2009 A flux rope model for CME initiation over solar cycle 23 Jonathan Constable.

Modeling the Neupert Effect in Flares: Connecting Theory and Observation Andrea Egan Advisors: Dr. Trae Winter and Dr. Kathy Reeves.

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

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.

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

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

Magnetic Helicity • Magnetic helicity measures

Solar-B XRT XRT-1 The Science and Capability of the Solar-B / X-Ray Telescope Solar-B XRT Presenter: Ed DeLuca Smithsonian Astrophysical Observatory.

Modelling X-ray Bright Points on the Quiet Sun. Parameter fitting to a Coronal Heating solution. Matthew Chantry Mentor: Aad van Ballegooijen University.

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

Kathy Reeves Harvard-Smithsonian Center for Astrophysics Terry Forbes University of New Hampshire Partitioning of energy in a loss-of-equilibrium CME model.

Dr. Alexei A. Pevtsov Helicity on the Sun. If you worry about publicity Do not speak of Current Helicity Jan Stenflo.

Asymmetric Magnetic Reconnection in Coronal Mass Ejection Current Sheets Crystal L. Pope Elmhurst College Advisors: Nick Murphy & Mari Paz Miralles Harvard-Smithsonian.

Magnetic Waves in Solar Coronal Loops Ryan Orvedahl Stony Brook University Advisor: Aad van Ballegooijen Center for Astrophysics.

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

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

Can the coronal field’s susceptibility to emergence-induced eruption be estimated? SSPVSE Discussion Group B, Wed., 19 Oct B. Welsch, Space Sciences.

1 Magnetic waves in sheared field regions E.J. Zita, The Evergreen State College, Olympia, WA Abstract How do magnetohydrodynamic (MHD) waves change.

Data-Driven MHD Modeling of CME Events

RT Modelling of CMEs Using WSA- ENLIL Cone Model

Estimating Free Magnetic Energy from an HMI Magnetogram by Brian T. Welsch Space Sciences Lab, UC-Berkeley Several methods have been proposed to estimate.

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.

MAGNETIC TWIST OF EUV CORONAL LOOPS OBSERVED BY TRACE RyunYoung Kwon, Jongchul Chae Astronomy Program, School of Earth and Environmental Science Seoul.

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.

Determining the Location of Open Magnetic Field Areas in Active Regions and their Potential as Sources of the Slow Solar Wind J. L. Culhane 1, S.J. Edwards.

Probing Energy Release of Solar Flares M. Prijatelj Carnegie Mellon University Advisors: B. Chen, P. Jibben (SAO)

Will it Fit? A Comparison of Asymmetric Magnetic Reconnection Models and Observations Drake Ranquist Brigham Young University Advisors: Mari Paz Miralles.

Calculating Magnetic Energy in Active Regions Using Coronal Loops for AR and AR Presentation by, Joseph B. Jensen.

1 Searching for Alfvén Waves John Yoritomo The Catholic University of America Mentor: Dr. Adriaan van Ballegooijen The Smithsonian Astrophysical Observatory.

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

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

I. INTRODUCTION Gas Pressure Magnetic Tension Coronal loops are thin and bright structure of hot plasma emitting intense radiation in X-ray and EUV. (1)

1 Introduction: Onset of solar flares and coronal mass ejections Yokoyama, T. Dept. Earth & Planetary Science, University of Tokyo Isobe, H. Univ. Tokyo.

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

New England Space Science Meeting 3 Feb 1, 2006 Implications of Reconnection Nathan Schwadron Feb 1, 2006.

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,

III. APPLICATIONS of RECONNECTION Yohkoh Bright Pts Loops Holes A magnetic world T=few MK 1. Coronal Heating.

Evolutionary Characteristics of Magnetic Helicity Injection in Active Regions Hyewon Jeong and Jongchul Chae Seoul National University, Korea 2. Data and.

Magnetic Helicity and Solar Eruptions Alexander Nindos Section of Astrogeophysics Physics Department University of Ioannina Ioannina GR Greece.

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

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,

Finding the Source of Ion Beams in the Solar Wind Hanna Kristensen Advisors: Justin Kasper and Mike Stevens.

Initiation of Coronal Mass Ejections: Implications for Forecasting Solar Energetic Particle Storms Ron Moore, Alphonse Sterling, David Falconer, John Davis.

Sweet Solar SAP: Boiling Down the Thermal Energy Content of Supra-Arcade Plasma Ashley Armstrong Advisor: Dr. Kathy Reeves Solar REU Summer 2012.

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:

2. Method outline2. Method outline Equation of relative helicity (Berger 1985): - : the fourier transform of normal component of magnetic field on the.

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,

Investigating a complex X-class flare using NLFFF modeling

Ward Manchester University of Michigan

Abstract We simulate the twisting of an initially potential coronal flux tube by photospheric vortex motions. The flux tube starts to evolve slowly(quasi-statically)

Presentation transcript:

Sigmoid: A Twisted Tale of Flux and Fields By Tyler Behm Mentors: Antonia Savcheva Ed DeLuca

Etymology Sigm- Sigma -oid Having the shape or form of

Talk Outline Part 1: Background What is the “S” made of? How do sigmoids evolve with time? How can we study sigmoids? Part 2: REU Research Finding best fit model Cross-sections and QSL maps

What is the “S” made of? Cooled plasma suspend by coiled magnetic fields Gold, T., and Hoyle, F., Mon. Not. R. astron. Soc, 120, 89 (1961)

How do sigmoids evolve with time? Magnetic reconnection 68% of erupting active regions are sigmoids

How can we study sigmoids? Force-Free PotentialLinearNonlinear NLFFF Modeling Sigmoid Cross- Section Lorent z Pressure

Tyler’s Work Significance and Goals Goals Find best fit NLFFF model in axial/polodial flux space Generate mapping of field divergence (QSL) Significance Place boundaries on energy in field Estimate helicity; Predict stability of sigmoid Russell and Elphic, 1979

Tyler’s Work Step 1: Make Models LOS Magnetogram  Fields XRT Images  Coronal Loops (ie Flux) Span polodial/axial flux parameter space Magneto-friction relaxation Both are Aug 4, 2010

Tyler’s Work Step 2: Find Best Fit Aug 4, models to span flux parameter space Goodness = Less distance from field to flux = Green (on left charts) Unstable

Tyler’s Work Step 3: Make Sure It’s Stable Best Fit Model Higher Flux Model Aug 4, 2010

Tyler’s Work Step 4: Make Quasi-Separatrix Layers If B-fields were heads of hair… QSL’s would be parted hairlines. QSL

Tyler’s Work Step 4: Make Quasi-Separatrix Layers Aug 4, 2010 Free Energy = 6.0×10 31 erg Helicity = -5.2×10 42 Mx 2 Aug 10, 2010 Free Energy = 3.4×10 31 erg Helicity = -2.3×10 42 Mx 2

Tyler’s Work Step 4: Make Quasi-Separatrix Layers Aug 4, 2010 Free Energy = 6.0×10 31 erg Helicity = -5.2×10 42 Mx 2 Aug 10, 2010 Free Energy = 3.4×10 31 erg Helicity = -2.3×10 42 Mx 2

Conclusion What is the “S” made of? Magnetically floated, cool coronal plasma How do sigmoids evolve with time? Magnetic reconnection and CMEs How can we study sigmoids? NLFFF Modeling + 1 intern = 2 sigmoids modeled

Special Thanks NSF REU solar physics program at CfA, grant number ATM for funding Kathy, Marie, and all REU organizers Antonia and Ed for excellent mentorship Aad for the Coronal Modeling Software CfA for hospitality Trae, Jonathan, and Alisdair for computer help

References Importance of Sigmoid Studies: Canfield et al. (1999, 2007) NLFFF Modeling: Savcheva, Van Ballegooijen (2009) QSL’s: Domoulin, Hénoux, Priest, Mandrini (1996) Illustrations: solarmuri.ssl.berkeley.edu/~hhudson/cartoo ns/