Cross-Sectional Properties of Coronal Loops and Their Implications Henry “Trae” Winter III with Chester Curme.

Slides:



Advertisements
Similar presentations
Global Simulations of Astrophysical Jets in Poynting Flux Dominated Regime Hui Li S. Colgate, J. Finn, G. Lapenta, S. Li Engine; Injection; Collimation;
Advertisements

The effects of canopy expansion on chromospheric evaporation driven by thermal conductions fronts Authors: F. Rozpedek, S. R. Brannon, D. W. Longcope Credit:
Low-Energy Coronal Sources Observed with RHESSI Linhui Sui (CUA / NASA GSFC)
The Color Glass Condensate and RHIC Phenomenology Outstanding questions: What is the high energy limit of QCD? How do gluons and quarks arise in hadrons?
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.
SH13A-2240 Automatic Detection of EUV Coronal Loops from SDO-AIA Data Alissa N. Oppenheimer¹ ( ), A. Winebarger², S. Farid³,
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.
Ryan Payne Advisor: Dana Longcope. Solar Flares General  Solar flares are violent releases of matter and energy within active regions on the Sun.  Flares.
Evolution of Magnetic Helicity in the Corona During Flux Emergence Anna Malanushenko, Humed Yusuf, Dana Longcope.
Extrapolation vs. MHD modeling Hardi Peter Kiepenheuer-Institut Freiburg, Germany Contribution to the discussions at the SDO workshop / Monterey Feb 2006.
Quiescent Loop Heating Profiles with AIA Henry (Trae) Winter, Kerry Neal, Jenna Rettenmayer, & Piet Martens Montana State University--Bozeman.
MRT workshop, August 10, 2004 Active-region magnetic structures and their perturbations by flares H.S. Hudson SSL/UCB.
The Hunt for a Link : Quantitative Connections Between Magnetic Fields and EIT Coronal Wave/CME Properties Prepared by James R. Robertson J.R. In conjunction.
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.
Chromospheric diagnostics using RHESSI visibilities Marina Battaglia & Eduard Kontar.
Predicting Coronal Emissions with Multiple Heating Rates Loraine Lundquist George Fisher Tom Metcalf K.D. Leka Jim McTiernan AGU 2005.
Tackling the coronal heating problem using 3D MHD models with spectral synthesis Solar eclipse, , Wendy Carlos & John Kern  observational constraints.
Solar Physics & upper Atmosphere Research Group University of Sheffield A possible method for measuring the plasma density profile along coronal loops.
SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no. C9] HMI/AIA science teams meeting; Monterey; Feb
Properties of Prominence Motions Observed in the UV T. A. Kucera (NASA/GSFC) E. Landi (Artep Inc, NRL)
Feb. 2006HMI/AIA Science Team Mtg.1 Heating the Corona and Driving the Solar Wind A. A. van Ballegooijen Smithsonian Astrophysical Observatory Cambridge,
1 L. Perivolaropoulos Department of Physics University of Ioannina Open page
Magnetic Waves in Solar Coronal Loops Ryan Orvedahl Stony Brook University Advisor: Aad van Ballegooijen Center for Astrophysics.
Thermal Diagnostics of Elementary and Composite Coronal Loops with AIA Markus J. Aschwanden & Richard W. Nightingale (LMSAL) AIA/HMI Science Teams Meeting,
1. Background2. Flux variation3. Polarity reversal4. Electron evolution5. Conclusions The role of coronal mass ejections in the solar cycle evolution of.
Brookhaven Science Associates U.S. Department of Energy Neutrino Factory / Muon Collider Collaboration Meeting March 17-19, 2008, FNAL, Batavia, IL Target.
Twist & writhe of kink-unstable magnetic flux ropes I flux rope: helicity sum of twist and writhe: kink instability: twist  and writhe  (sum is constant)
Magnetic configurations responsible for the coronal heating and the solar wind Hwanhee Lee 1, Tetsuya Magara 1 1 School of Space research, Kyung Hee University.
Helicity: where it comes from and what it tells us Dana Longcope, MSU Anna Malanushenko, MSU/LMSAL 8/11/10Canfield-fest Thanks: Graham Barnes, CoRA B.
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.
Solar eclipse, , Wendy Carlos and John Kern Structure of solar coronal loops: from miniature to large-scale Hardi Peter Max Planck Institute for.
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.
Instant Tomography of Active Regions Markus J. Aschwanden Jean-Pierre Wuelser, Nariaki Nitta, & James Lemen (LMSAL) STEREO Science Working Group Meeting.
Where is Coronal Plasma Heated? James A. Klimchuk NASA Goddard Space Flight Center, USA Stephen J. Bradshaw Rice University, USA Spiros Patsourakos University.
Jet/environment interactions in FR-I and FR-II radio galaxies Judith Croston with Martin Hardcastle, Mark Birkinshaw and Diana Worrall.
Cross-Sectional Properties of Coronal Loops 1. Abstract In this work we present some preliminary results from an assessment of coronal loop cross sections.
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.
Evolution of Emerging Flux and Associated Active Phenomena Takehiro Miyagoshi (GUAS, Japan) Takaaki Yokoyama (NRO, Japan)
Modelling the radiative signature of turbulent heating in coronal loops. S. Parenti 1, E. Buchlin 2, S. Galtier 1 and J-C. Vial 1, P. J. Cargill 3 1. IAS,
Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,
Materials Learning Objectives. Lesson 1 1.Understand that there is a huge variety of materials 2.Understand that there is a small number of elements from.
Coronal Loops Workshop 6, La Roche-en-Ardenne, Belgium, Jun 2013 Density of active region outflows derived from Fe XIV 264/274 Naomasa KITAGAWA &
“ 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.
Feb. 3-5, 20034th Solar-B science meeting1 Corona-Photosphere Connection with Spectropolarimeter Yukio Katsukawa (Univ. of Tokyo)
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.
Prominence Dynamics: the Key to Prominence Structure Judy Karpen Naval Research Laboratory SVST.
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,
Flare-Associated Oscillations Observed with NoRH Ayumi Asai (NSRO) Nobeyama Symposium 2004 : 2004/10/26.
Using Forward Folding of SERTS and Yohkoh Data to Estimate the Electron Densities of Coronal Plasma J.T. Schmelz & H.D. Winter III Presented by Henry (Trae)
Centre for Astrophysics Space- and time-dependent heating of solar coronal loops S. W. Higgins & R. W. Walsh
A Numerical Study of the Breakout Model for Coronal Mass Ejection Initiation P. MacNeice, S.K. Antiochos, A. Phillips, D.S. Spicer, C.R. DeVore, and K.
Shine 2004, A. Sterling CME Eruption Onset Observations: Dimmings Alphonse C. Sterling NASA/MSFC/NSSTC.
2 nd Solaire Network Meeting Catania, January 2009 Investigating the characteristics of coronal loop heating by 1D hydrodynamic simulations R.
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:
Differential Rotation of coronal BP and Source Region of their Magnetic Fields H. Hara NAOJ 2011 Jun 29 Leverhulme – Probe the Sun 1 st Workshop at MSSL.
November 18, 2008Jonathan Cirtain SCIENCE & MISSION SYSTEMS Solar-C Plan ‘A’ Coronal observations Jonathan Cirtain MSFC/NASA November 18, 2008.
Nanoflare Properties in the Solar Corona
P.Zacharias1, S. Bingert2 & H. Peter2 1ISSI, Bern, Switzerland
The Loop Width Distribution – Are we Hitting Rock Bottom
Studying Transition Region Phenomena with Solar-B/EIS
Flare-Associated Oscillations Observed with NoRH
Downflow as a Reconnection Outflow
Sakai, J. I., Nishi, K., and Sokolov, I. V. ApJ, 2002, 576, 1018
Presentation transcript:

Cross-Sectional Properties of Coronal Loops and Their Implications Henry “Trae” Winter III with Chester Curme

Constant Cross- Section? Klimchuk et al Studied 10 SXT loops Measured an Apex to Footpoint Expansion Factor of

TRACE Loops Watko & Klimchuk, Loops Lopéz Fuentes et al, Loops

DeForest, 2007

Unresolved Structures

Lopés Fuentes et al, 2008 Countered DeForest’s argument Claimed that their method could distinguish between unresolved expanding and not expanding but resolved strands Conversation switched to theories that predict constant cross-section loops (i.e. Constant B).

How Could Loops be of Constant Cross-Section? Twist? (Klimchuk et al., 2000) Separators? (Plowman et al., 2009)

How Could Loops be of Constant Cross-Section? Emission loops (eLoops) do not actually trace field lines (Peter & Bingert, 2012)

Apex Temperature Evolution

Apex Density Evolution

Over Pressure

Synthetic Obs AIA Pixel Size Hi-C Pixel Size

Synthetic Obs AIA Pixel Size Hi-C Pixel Size

zz Width Measurements

Estimation of Width AIA171

Estimation of Width AIA 335

zz Estimation of Width “Hi-C Like”171

Estimation of Width “Hi-C Like” 335

Summary Loop geometry has an effect on fundamental loop properties such as temperature and density (pressure) Vesecky, Antiochos, and Underwood, 1979; Mariska, 1984; Schrijver, Lemen and Mewe, 1989; Dowdy, Emslie, and Moore, 1987 Modeled near-resolution, expanding loops can appear to be of constant cross-section just like those “pesky” observations Loops must be many pixels wide to make width determinations Is it safe to use magnetic fields to generate loop geometries for 1D models?

Extra Slides

See Anna Malanushenko’s Work at the SPD

How Could Loops be of Constant Cross-Section? Twist? (Klimchuk et al., 2000)

How Could Loops be of Constant Cross-Section? Separators? (Plowman et al., 2009)

How Could Loops be of Constant Cross-Section? Maybe eLoops do not trace out magnetic fields? (Peter & Bingert, 2012)

How Could Loops be of Constant Cross-Section? Peter & Bingert, 2012

What happens if loops are not of constant cross- section?

Brooks, et al 2013