Looking for the heating function of solar coronal loops Miriam Ritchie 1 and Rahul Sharma 2 MSU Solar Physics REU – 2011 Petrus (Piet) Martens 3, Joseph.

Slides:

Advertisements

Similar presentations

The Science of Solar B Transient phenomena – this aim covers the wide ranges of explosive phenomena observed on the Sun – from small scale flaring in the.

Advertisements

Evaporation driven by thermal conduction Heidi Dritschel REU student working in collaboration with Sean Brannon and Professor Longcope at MSU.

RHESSI observations of LDE flares – extremely long persisting HXR sources Mrozek, T., Kołomański, S., Bąk-Stęślicka, U. Astronomical Institute University.

Solar Physics & Space Plasma Research Centre University of Sheffield Ionization diagnostics of solar magnetic structures Dr Gary Verth

The effects of canopy expansion on chromospheric evaporation driven by thermal conductions fronts Authors: F. Rozpedek, S. R. Brannon, D. W. Longcope Credit:

Science With the Extreme-ultraviolet Spectrometer (EIS) on Solar-B by G. A. Doschek (with contributions from Harry Warren) presented at the STEREO/Solar-B.

SJC 2/28/2002Steady Flows Detected in EUV Loops 1 Steady Flows Detected in Extreme-Ultraviolet Loops Winebarger, A.R., Warren, H., van Ballegooijen, A.

Estimating the Chromospheric Absorption of Transition Region Moss Emission Bart De Pontieu, Viggo H. Hansteen, Scott W. McIntosh, Spiros Patsourakos.

Jaroslav Dudík 1,2 Elena Dzifčáková 3, Jonathan Cirtain 4 1 – DAMTP-CMS, University of Cambridge 2 – DAPEM, FMPhI, Comenius University, Bratislava, Slovakia.

MSU Solar Physics REU Jennifer O’Hara Heating of Flare Loops With Observationally Constrained Heating Functions Advisors Jiong Qiu, Wenjuan Liu.

X-Ray Observation and Analysis of a M1.7 Class Flare Courtney Peck Advisors: Jiong Qiu and Wenjuan Liu.

Ryan Payne Advisor: Dana Longcope. Solar Flares General  Solar flares are violent releases of matter and energy within active regions on the Sun.  Flares.

Sub-THz Component of Large Solar Flares Emily Ulanski December 9, 2008 Plasma Physics and Magnetohydrodynamics.

Characterizing Thermal and Non- Thermal Electron Populations in Solar Flares Using RHESSI Amir Caspi 1,2, Säm Krucker 2, Robert P. Lin 1,2 1 Department.

Quiescent Loop Heating Profiles with AIA Henry (Trae) Winter, Kerry Neal, Jenna Rettenmayer, & Piet Martens Montana State University--Bozeman.

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.

Solar Turbulence Friedrich Busse Dali Georgobiani Nagi Mansour Mark Miesch Aake Nordlund Mike Rogers Robert Stein Alan Wray.

1 Chromospheric UV oscillations depend on altitude and local magnetic field Noah S. Heller and E.J. Zita, The Evergreen State College, Olympia, WA

Coronal Loop Oscillations Seen in Unprecedented Detail by SDO/AIA Rebecca White and Erwin Verwichte University of Warwick, Centre for Fusion, Space and.

How Does a Coronal Loop’s Geometry Relate to its Other Properties? An Exploration of Non-Thermal Particle Effects on Simulated Loop Structures Chester.

Alfvén Waves in the Solar Corona S. Tomczyk, S. Mclntosh, S. Keil, P. Judge, T. Schad, D. Seeley, J. Edmondson Science, Vol. 317, Sep., 2007.

08__050610_SCIP/SEB_PSR_Delivery.1 Temperature and Density Diagnostics with SECCHI EUVI J.S. Newmark Naval Research Laboratory (202)

Predicting Coronal Emissions with Multiple Heating Rates Loraine Lundquist George Fisher Tom Metcalf K.D. Leka Jim McTiernan AGU 2005.

Winds of cool supergiant stars driven by Alfvén waves

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

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

Reconstructing Active Region Thermodynamics Loraine Lundquist Joint MURI Meeting Dec. 5, 2002.

EUV signatures of small scale heating in loops Susanna Parenti SIDC-Royal Observatory of Belgium, Be.

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

MSU Solar Physics Group RHESSI and Max Millennium Reuven Ramaty High Energy Solar Spectroscopic Imager TRACE Transition Region And Coronal Explorer SSEL’s.

MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.

Hydrostatic modelling of active region EUV and X-ray emission J. Dudík 1, E. Dzifčáková 1,2, A. Kulinová 1,2, M. Karlický 2 1 – Dept. of Astronomy, Physics.

990901EIS_RR_Science.1 Science Investigation Goals and Instrument Requirements Dr. George A. Doschek EIS US Principal Investigator Naval Research Laboratory.

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

The Solar Corona Steven R. Spangler Department of Physics and Astronomy University of Iowa.

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.

High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.

Solar Applications of the Space Weather Modeling Framework R. M. Evans 1,2, J. A. Klimchuk 1 1 NASA GSFC, 2 GMU February 2014 SDO AIA 171 Å.

Age dependence of EM in AR Cores... and... Some thoughts on the Accuracy of Atomic Data Helen Mason, Durgesh Tripathi, Brendan O’Dwyer and Giulio Del Zanna.

Short period MHD waves in the solar corona

Flare Thermal Energy Brian Dennis NASA GSFC Solar Physics Laboratory 12/6/20081Solar Cycle 24, Napa, 8-12 December 2008.

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.

Standard DEM: Consider a imaging instrument with M EUV filters (for the EUVI Fe bands M = 3). The measured intensity in one image pixel is given by DEM.

Solar Atmosphere A review based on paper: E. Avrett, et al. “Modeling the Chromosphere of a Sunspot and the Quiet Sun” and some others [Alexey V. Byalko]

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

Modelling Magnetic Reconnection and Nanoflare Heating in the Solar Corona The Coronal Heating Problem George Biggs Advisors: Mahboubeh Asgari-Targhi &

“ HINODE workshop” Zhanle Du & Huaning Wang 杜占乐王华宁中科院国家天文台 (NAOC) December 9, 2007 Problem of coronal temperature diagnostics 2007 年 12 月 8-10 日北京九华山庄.

Emission measure distribution in loops impulsively heated at the footpoints Paola Testa, Giovanni Peres, Fabio Reale Universita’ di Palermo Solar Coronal.

Determining the Heating Rate in Reconnection Formed Flare Loops Wenjuan Liu 1, Jiong Qiu 1, Dana W. Longcope 1, Amir Caspi 2, Courtney Peck 2, Jennifer.

Flare Prediction and the Background Corona Coronal Diagnostic Spectrometer Wolter-Schwarzschild Type 2 telescope Two separate spectrometers- the Normal.

XRT and EIS Observations of Reconnection associated Phenomena D. Shiota, H. Isobe, D. H. Brooks, P. F. Chen, and K. Shibata

Analysis of the Temperature and Emission Measure of Solar Coronal Arcades and Test of Flare/Arcade Loop Length ( Yamamoto, Shiota, Sakajiri, Akiyama, Isobe,

Shock heating by Fast/Slow MHD waves along plasma loops

On the spectroscopic detection of magnetic reconnection evidence with Solar B – I. Emission line selection and atomic physics issues P. F. Chen 1,2, H.

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

The Slow Solar Wind Tom Holzer NCAR/HAO NCAR/HAO.

Investigating a complex X-class flare using NLFFF modeling

Zurab Vashalomidze (1) In collaboration with

P.Zacharias1, S. Bingert2 & H. Peter2 1ISSI, Bern, Switzerland

Dong Li Purple Mountain Observatory, CAS

Emission measure distribution from plasma modeling

Diagnosing kappa distribution in the solar corona with the polarized microwave gyroresonance radiation Alexey A. Kuznetsov1, Gregory D. Fleishman2 1Institute.

Progress Toward Measurements of Suprathermal Proton Seed Particle Populations J. Raymond, J. Kohl, A. Panasyuk, L. Gardner, and S. Cranmer Harvard-Smithsonian.

Phillip Chamberlin Solar Flares (303) University of Colorado

Collisional lines: diagnostics & results

Differential Emission Measure

search of Alfvén waves in faculae

Periodic Acceleration of Electrons in Solar Flares

Presentation transcript:

Looking for the heating function of solar coronal loops Miriam Ritchie 1 and Rahul Sharma 2 MSU Solar Physics REU – 2011 Petrus (Piet) Martens 3, Joseph Plowman 3, Jason Scott 3 1 University of St. Andrews, 2 Udaipur Solar Observatory, 3 Montana State University

Outline  Project background & theory.  Data & Instruments.  Analysis.  Current project status.  Next…  Acknowledgments

Project Background Coronal Heating : Conversion of free magnetic energy into thermal energy. Coronal Heating Wave Heating (AC) Foot point shuffling. MHD wave propagation High Alfven wave flux Non-uniform heating ratio Magnetic Reconnection (DC) B – field stressesReconnection eventsFlares – NanoflaresUniform heating rates

Coronal Heating Requirement Radiative Loss (ER) Conductive Loss (EC) Heating Source (EH)

Hydrostatic Scale Height Thermal Pressure Gravitational Stratification Momentum eq; Height ‘h’ above surface; Therefore, solution of energy balance eq. becomes

For a static coronal loop; energy eq. is: Rosner – Tucker – Vaiana (RTV) scaling laws, RTV’s approx. of constant pressure, no gravity and uniform heating.

Instruments and Data Sources Instruments AIA/SDOEIS/Hinode EIS: Scanning spectrograph Limited cadence, field of view High spectral resolution AIA: High cadence, resolution Full-disk Low spectral resolution.

Data Sources Extreme-Ultraviolet Imaging Spectrometer (EIS) Atmospheric Imaging Assembly (AIA) Used IDL : vso_search & vso_get

Region Identification Criteria for selecting loops:  Stable.  Non Flaring.  Away from limb.  Observed in EIS with 1 arc-second slit ID. Data Processing: Converted EIS and AIA level – 1.fits files into.map files.

Co-Alignment To ensure similar pixel locations on EIS and AIA datasets.

Co-alignment Check Widget Interface for Loading Map Applications WILMA, a GUI written by Trae Winter & Jason Scott used to select points for above.

Picking Points

Loop straightening Using a loop straightening tool gave a better idea of the geometry of the loop.

Background Subtraction

Density diagnostics  Involved finding intensity ratio of density sensitive emission lines.  Highly important for estimating pressure balance, energy and ‘filling factor.’ CHIANTI corresponding intensity ratios and density

Gaussian fitting for intensity profile  The fitting of gaussians resolved wavelength blending;  Gave us fit_struc files to work with.

Density plots .fit_struc files were converted into.map file.  Loops were straightened from these files.  Background intensities were subtracted.  A code “get_dens_195.pro” finds the corresponding densities

Density profile comparison

What next… Temperature profile: By using EM Loci method for isothermal loops or by Differential Emission Measurements (DEMs) for multi-thermal loops. Pressure: By ideal gas law, using temperature and densities found and loop length. All these parameters can provide an estimate of heating function from scaling law.

Acknowledgements We are grateful to our mentor Prof. Petrus (Piet) Martens, Joseph Plowman and Jason Scott for all their patience and help throughout the summer, and the Solar Physics group for the opportunity. Thank you to the other REUs for a great summer. Thank you Eric for everything. To the Grad-Students for making us believe; “Nullum magnum ingenium sine mixtura dementiae fuit” "No great genius has existed without a mixture of madness"