Soft-Hard Soft Spectral Behaviour From Dynamic Reconnection Test Particle Calculations C. A. Burge 1, P. Petkaki 2, A.L.MacKinnon 3 1. Department of Physics.

Slides:

Advertisements

Similar presentations

Masuda Flare: Remaining Problems on the Looptop Impulsive Hard X-ray Source in Solar Flares Satoshi Masuda (STEL, Nagoya Univ.)

Advertisements

Investigating the Origin of the Long-Duration High- Energy Gamma-Ray Flares Gerry Share, Jim Ryan and Ron Murphy (in absentia) Steering Committee Overseer.

Thick Target Coronal HXR Sources Astrid M. Veronig Institute of Physics/IGAM, University of Graz, Austria.

FLARING ENERGY RELEASE Lyndsay Fletcher University of Glasgow EPS Plasma Meeting, Sofia, June

Energy Release and Particle Acceleration in Flares Siming Liu University of Glasgow 9 th RHESSI Workshop, Genova, Italy, Sep

Solar flares and accelerated particles

Low-Energy Coronal Sources Observed with RHESSI Linhui Sui (CUA / NASA GSFC)

Chapter 18 The Electromagnetic Spectrum and Waves

Radiation & Photometry AS4100 Astrofisika Pengamatan Prodi Astronomi 2007/2008 B. Dermawan.

Hard X-Ray Footpoint Motion in Spectrally Distinct Solar Flares Casey Donoven Mentor Angela Des Jardins 2011 Solar REU.

“Physics at the End of the Galactic Cosmic-Ray Spectrum” Aspen, CO 4/28/05 Diffusive Shock Acceleration of High-Energy Cosmic Rays The origin of the very-highest-energy.

Relations between concurrent hard X-ray sources in solar flares M. Battaglia and A. O. Benz Presented by Jeongwoo Lee NJIT/CSTR Journal Club 2007 October.

Electron Acceleration at the Solar Flare Reconnection Outflow Shocks Gottfried Mann, Henry Aurass, and Alexander Warmuth Astrophysikalisches Institut Potsdam,

Flare energy and fast electrons via Alfvén waves H. S. Hudson & L. Fletcher SSL/Berkeley and Glasgow U. Predictions for Hinode/SOT flare observations.

Auroral dynamics EISCAT Svalbard Radar: field-aligned beam  complicated spatial structure (

Institute of Astronomy, Radio Astronomy and Plasma Physics Group Eidgenössische Technische Hochschule Zürich Swiss Federal Institute of Technology, Zürich.

+ Hard X-Ray Footpoint Motion and Progressive Hardening in Solar Flares Margot Robinson Mentor: Dr. Angela DesJardins MSU Solar Physics Summer REU, 2010.

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

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

Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson,

It is possible that reconnection can occur multiple times along CS Plasmoids form as magnetic ‘islands’ between X-points Due to density and.

Dissipation of Alfvén Waves in Coronal Structures Coronal Heating Problem T corona ~10 6 K M.F. De Franceschis, F. Malara, P. Veltri Dipartimento di Fisica.

GLOBAL ENERGETICS OF FLARES Gordon Emslie (for a large group of people)

Soft-hard-soft spectral behavior observed by RHESSI and HXRS Hugh Hudson Frantisek F a rnik ESPM-10 meeting Prague, Sept. 11, 2002.

Spectral analysis of non-thermal filaments in Cas A Miguel Araya D. Lomiashvili, C. Chang, M. Lyutikov, W. Cui Department of Physics, Purdue University.

Institute of Astronomy, Radio Astronomy and Plasma Physics Group Eidgenössische Technische Hochschule Zürich Swiss Federal Institute of Technology, Zürich.

Magnetic Reconnection Rate and Energy Release Rate Jeongwoo Lee 2008 April 1 NJIT/CSTR Seminar Day.

Solar Energetic Particles -acceleration and observations- (Two approaches at the highest energy) Takashi SAKO Solar-Terrestrial Environment Laboratory,

RHESSI and global models of flares and CMEs: What is the status of the implosion conjecture? H.S. Hudson Space Sciences Lab, UC Berkeley.

Wave Nature of Light and Quantum Theory

Physics of fusion power Lecture 7: particle motion.

Space and Astrophysics Generation of quasi- periodic pulsations in solar flares by MHD waves Valery M. Nakariakov University of Warwick United Kingdom.

Injection of κ-like suprathermal particles into DSA Kang, Hyesung et al. arXiv: by Zhang Xiao,

Electromagnetic Waves Chapter Introduction: Maxwell’s equations Electricity and magnetism were originally thought to be unrelated Electricity.

Multiwavelength observations of a partially occulted solar flare Laura Bone, John C.Brown, Lyndsay Fletcher.

Modelling of the Effects of Return Current in Flares Michal Varady 1,2 1 Astronomical Institute of the Academy of Sciences of the Czech Republic 2 J.E.

Compelling Theoretical Issues Driven by Observations / Theoretical Wish List of Observations WG5 Hamish Reid.

Evidence for chromospheric heating in the late phase of solar flares David Alexander Lockheed Martin Solar and Astrophysics Lab. Collaborators: Anja CzaykowskaMPI.

Lyndsay Fletcher, University of Glasgow Ramaty High Energy Solar Spectroscopic Imager Fast Particles in Solar Flares The view from RHESSI (and TRACE) MRT.

Footpoint behavior Hugh Hudson UCB Galileo science meeting Nobeyama, July 12, 2002.

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

Coronal hard X-ray sources and associated decimetric/metric radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA) S.R Kane G. Hurford.

Chapter 21 Electromagnetic Waves. General Physics Exam II Curve: +30.

Reconnection rates in Hall MHD and Collisionless plasmas

1 Physics of GRB Prompt emission Asaf Pe’er University of Amsterdam September 2005.

Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,

Energetic electrons acceleration: combined radio and X-ray diagnostics

Electron inertial effects & particle acceleration at magnetic X-points Presented by K G McClements 1 Other contributors: A Thyagaraja 1, B Hamilton 2,

Recent results in cosmic ray physics and their interpretation

Radiation spectra from relativistic electrons moving in turbulent magnetic fields ＹｕｔｏＴｅｒａｋｉ & Fumio Takahara Theoretical Astrophysics Group Osaka Univ.,

Simulation Study of Magnetic Reconnection in the Magnetotail and Solar Corona Zhi-Wei Ma Zhejiang University & Institute of Plasma Physics Beijing,

Marcin Gruszecki S. Vasheghani Farahani, V. Nakariakov, T. Arber Magnetacoustic shock formation near a magnetic null point.

Today’s Papers 1. Flare-Related Magnetic Anomaly with a Sign Reversal Jiong Qiu and Dale E. Gary, 2003, ApJ, 599, Impulsive and Gradual Nonthermal.

Particle Acceleration by Relativistic Collisionless Shocks in Electron-Positron Plasmas Graduate school of science, Osaka University Kentaro Nagata.

Probing Electron Acceleration with X-ray Lightcurves Siming Liu University of Glasgow 9 th RHESSI Workshop, Genova, Italy, Sep

MHD wave propagation in the neighbourhood of a two-dimensional null point James McLaughlin Cambridge 9 August 2004.

Introduction In a solar flare, charged particles (for example fast electrons) are accelerated along magnetic field lines in the solar atmosphere, travelling.

MHD and Kinetics Workshop February 2008 Magnetic reconnection in solar theory: MHD vs Kinetics Philippa Browning, Jodrell Bank Centre for Astrophysics,

Flare Ribbon Expansion and Energy Release Ayumi ASAI Kwasan and Hida Observatories, Kyoto University Explosive Phenomena in Magnetized Plasma – New Development.

What is the Origin of the Frequently Observed v -5 Suprathermal Charged-Particle Spectrum? J. R. Jokipii University of Arizona Presented at SHINE, Zermatt,

Particle acceleration by direct electric field in an active region modelled by a CA model CA modelAcceleration modelParticle distributionConclusionsIntroductionX-ray.

Physics of Solar Flares

Marina Battaglia, FHNW Säm Krucker, FHNW/UC Berkeley

Two Years of NoRH and RHESSI Observations: What Have We Learned

Series of high-frequency slowly drifting structure mapping the magnetic field reconnection M. Karlicky, A&A, 2004, 417,325.

SMALL SEP EVENTS WITH METRIC TYPE II RADIO BURSTS

Heavy-Ion Acceleration and Self-Generated Waves in Coronal Shocks

Coronal Loop Oscillations observed by TRACE

The spectral evolution of impulsive solar X-ray flares

Periodic Acceleration of Electrons in Solar Flares

Presentation transcript:

Soft-Hard Soft Spectral Behaviour From Dynamic Reconnection Test Particle Calculations C. A. Burge 1, P. Petkaki 2, A.L.MacKinnon 3 1. Department of Physics & Astronomy, University of Glasgow, Glasgow, G12 8QQ. 2. British Antarctic Survey, Cambridge, CB3 0ET. 3. DACE, University of Glasgow, Glasgow,G3 6NH.

SHS Spectral Pattern SHS = hardening of the X- ray spectrum of a flare as the HXR flux increases. The spectrum softens again as the flux decreases. Ubiquitous in solar flare HXR spectra-a clue to the electron accelerator? Hudson & Fárník (2002)‏

What Causes SHS? Theories include: Electric field induced by electrons causing reduction in number of low- energy electrons, and causing hardening of photon spectrum.(Zharkova & Gordovskyy 2006)‏ Changes in escape length of fast electrons could produce SHS behaviour. (Benz 1976, Grigis & Benz 2006)‏ Variation in proportion of thermal & nonthermal photons.(Aschwanden 2004)‏ Increase in efficiency of acceleration mechanism.(Aschwanden 2004)‏

X Type Neutral Point Linear waves traveling through a region including a magnetic null point become dissipative phenomena around the null (e.g. Craig and McClymont, 1991; Hassam, 1992; MacLaughlin and Hood, 2004). Near the null a large, localised electric field develops. Particles can become decoupled from the magnetic field and be freely accelerated in a suitably collisionless plasma. This linear reconnection is intrinsically time- dependent, with frequency depending on magnetic field strength, system scale and resistivity. Craig & McClymont (1991)‏

X Type Neutral Point B x = y ; B y = x electrons with initial conditions chosen randomly from a spatially uniform, Maxwellian distribution with T= 5 x 10 6 K. We normalise speeds to c & times to the electron gyroperiod at the boundary. Final energy distributions were generated after t=5360 (1s for typical coronal conditions).

Particle Trajectories

SHS Spectral Pattern: Thick Target

SHS Spectral Pattern: Thin Target

Spectral Index Variation: Thin Target

SHS Spectral Pattern

Numbers of accelerated electrons and maximum energies attained (hence HXR spectral hardness) maximise for an intermediate range of ω. Continuously varying ω will produce SHS behaviour. This model is simple and idealised, but is interesting as several acceleration regions may exist in a flare. Conclusions