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

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

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

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

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

R. P. Lin Physics Dept & Space Sciences Laboratory University of California, Berkeley The Solar System: A Laboratory for the Study of the Physics of Particle.

Solar flares and accelerated particles

The Focusing Optics X-ray Solar Imager (FOXSI) Steven Christe 1, S. Krucker 2, L. Glesener 2, S. Ishikawa 3, B. Ramsey 4, T. Takahashi 3, R.P. Lin 2 1.

TRACE and RHESSI observations of the failed eruption of the magnetic flux rope Tomasz Mrozek Astronomical Institute University of Wrocław.

A flare compilation Lots of people including Louise Harra, Lidia van Driel Gesztelyi, Chris Goff, Sarah Matthews, Len Culhane, Cristina Mandrini, Pascal.

Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003.

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

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

Super-Hot Thermal Plasmas in Solar Flares

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,

+ 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.

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.

Hard X-ray footpoint statistics: spectral indices, fluxes, and positions Pascal Saint-Hilaire 1, Marina Battaglia 2, Jana Kasparova 3, Astrid Veronig 4,

Measuring the Temperature of Hot Solar Flare Plasma with RHESSI Amir Caspi 1,2, Sam Krucker 2, Robert P. Lin 1,2 1 Department of Physics, University of.

Inverse Problems in Solar Imaging Spectroscopy - Future Applications G.J. Hurford Space Sciences Lab University of California, Berkeley Vienna 20 July.

Solar Energetic Particle Production (SEPP) Mission Primary Contacts: Robert P. Lin (UC Berkeley), John L. Kohl (Harvard-Smithsonian CfA) Primary Science.

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

Search for X-ray emission from coronal electron beams associated with type III radio bursts Pascal Saint-Hilaire, Säm Krucker, Robert P. Lin Space Sciences.

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

RHESSI OBSERVATIONS OF FLARE FOOTPOINTS AND RIBBONS H. Hudson and M. Fivian (SSL/UCB)

Evidence of Thick Reconnection Layers in Solar Flares John Raymond Work with A. Ciaravella, Y.-K. Ko and J. Lin White Light and UV Observations Apparent.

Inversions of Flaring Radio Emissions. Gregory D. Fleishman.

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

Hard X-ray Diagnostics of Solar Eruptions H. Hudson SSL, UC Berkeley and U. Of Glasgow.

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

Computation of centroid locations in photon and electron maps Marco Prato Pure and Applied Mathematics Department University of Modena and Reggio Emilia,

Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,

Magnetic Reconnection Rate and RHESSI Hard X-Ray Imaging Spectroscopy of Well Resolved X-class Flares Yan Xu, Ju Jing, Wenda Cao, and Haimin Wang.

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

WG 1 Summary Techniques and Applications. WG1 sessions New algorithms: UV smooth, electron maps Source locations Source sizes Source fluxes (imaging spectroscopy)

Co-spatial White Light and Hard X-ray Flare Footpoints seen above the Solar Limb: RHESSI and HMI observations Säm Krucker Space Sciences Laboratory, UC.

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

Thermal, Nonthermal, and Total Flare Energies Brian R. Dennis RHESSI Workshop Locarno, Switzerland 8 – 11 June, 2005.

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

Loop-top altitude decrease in an X-class flare A.M. Veronig 1, M. Karlický 2,B. Vršnak 3, M. Temmer 1, J. Magdalenić 3, B.R. Dennis 4, W. Otruba 5, W.

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

IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.

RHESSI and Radio Imaging Observations of Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD G. Trottet, Observatoire.

Studies on the 2002 July 23 Flare with RHESSI Ayumi ASAI Solar Seminar, 2003 June 2.

Source sizes and energy partition from RHESSI imaging and spectroscopy Alexander Warmuth Astrophysikalisches Institut Potsdam.

Energetic electrons acceleration: combined radio and X-ray diagnostics

NoRH Observations of RHESSI Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD E.J.Schmahl, Dept. of Astronomy, University.

Hard X-ray and radio observations of the 3 June 2007 flare Nicole Vilmer Meriem Alaoui Abdallaoui Solar Activity during the Onset of Solar Cycle

Joint session WG4/5 Points for discussion: - Soft-hard-soft spectral behaviour – again - Non-thermal pre-impulsive coronal sources - Very dense 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.

Spectral Breaks in Flare HXR Spectra A Test of Thick-Target Nonuniform Ionization as an Explanation Yang Su NASA,CUA,PMO Gordon D. Holman.

RHESSI Hard X-Ray Observations of an EUV Jet on August 21, 2003 Lindsay Glesener, Säm Krucker RHESSI Workshop 9, Genova September 4, 2009.

I. Evidence of Rapid Flux Emergence Associated with the M8.7 Flare on 2002 July 26 Wang H. et al. 2004, ApJ, 605, using high temporal resolution.

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

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.

UV Spectroscopy of CME Currrent Sheets John Raymond Angela Ciaravella Silvio Giordano Dave Webb.

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

Some EOVSA Science Issues Gregory Fleishman 26 April 2011.

Cycle 24 Meeting, Napa December 2008 Ryan Milligan NASA/GSFC Microflare Heating From RHESSI and Hinode Observations Ryan Milligan NASA-GSFC.

RHESSI and the Solar Flare X-ray Spectrum Ken Phillips Presentation at Wroclaw Workshop “ X-ray spectroscopy and plasma diagnostics from the RESIK, RHESSI.

Coronal X-ray Emissions in Partly Occulted Flares Paula Balciunaite, Steven Christe, Sam Krucker & R.P. Lin Space Sciences Lab, UC Berkeley limb thermal.

Scientific Interests in OVSA Expanded Array Haimin Wang.

2. Data3. Results full disk image (H  ) of the flare (Sartorius Telescope) NOAA Abstract Preflare Nonthermal Emission Observed in Microwave and.

Observations of the Thermal and Dynamic Evolution of a Solar Microflare J. W. Brosius (Catholic U. at NASA’s GSFC) G. D. Holman (NASA/GSFC)

Flare footpoints in optical and UV Lyndsay Fletcher University of Glasgow RHESSI 10, August 4 th 2010, Annapolis TRACE WL ~2s time cadence, 0.5” pixel.

Marina Battaglia, FHNW Säm Krucker, FHNW/UC Berkeley

XRT Particle Acceleration at Magnetic Reconnection Sites

Nonthermal Electrons in an Ejecta Associated with a Solar Flare

Transition Region and Coronal Explorer (TRACE)

Presentation transcript:

It is possible that reconnection can occur multiple times along CS Plasmoids form as magnetic ‘islands’ between X-points Due to density and magnetic field strength decreasing with height, the majority of plasmoids are observed to rise

?

?

Back Projection Clean Pixon Forward Fit MEM NJIT VIS-Forward Fit UV smooth Electron Map 1.Fast 2.Easy to calculate uncertainties 3.Lease details than other methods 4.Explain results carefully

First 3 moments are not always the full story. RHESSI cannot image complex sources, but visibilities may tell you that a few details are missing. RHESSI visibilities are very good at getting 1 st 3 moments of simple sources Flux, size, location

Planning a New Mission Solar Vision 2020 A theorist's assessment/wish list of the future observational needs (Gordon Emslie) Key Interests: (a) thermal vs. nonthermal (b) acceleration (c) ion energy

Problem Solved: (1) true shape of HXR spectra (2) Microflares do NOT heat the corona (3) Flare connects to CME Problem Advanced but need to dig more: (1) Thermal/Nonthermal transition in the electron distribution fucntion (2) HXR structure at very small spatial scales (3) Directivity/location of HXR sources (4) Physical parameters of acceleration region (n, T, B) (5) Electron maps, but not at stage to study variation of F(E, r, t) (6) (EM, T) analysis (7) Partion of flare energy, SEP shock-acceleration efficiency (8) Fourier-based Imaging Problem Uncovered: (1) nonthermal source in the corona (2) HXR/gamma-ray emission location different (3) gamma-ray redshift (4) Different electron spectra for radio and HXR

Some thoughts of the new RHESSI: 0.1'' at 6.7 keV Focusing X-rays (lens of Si) Multiple Satellites 32 x 32 pix HXR imaging system (Bandler) 1k x 1k HXR Camera (<50 National Lab

Current Status of RHESSI 3. Bob Lin: 2010 Mar 16, 07:27UT. Clock stopped Observation resumed on May 1, 2010 pure non-thermal loop-top source, acceleration region RHESSI now modeled up to 150 Kev RHESSI vs Hinode (Kruck, HXR kernels over G-band) Future, RHESSI will be there for the coming solar maximum the next generation will be launched around We are able to image better than before 5. GH: Regression provision in Clean to improve normalization RHESSI data base at ETHZ moved to FHNW Cloud Solar Software (Nugget #131) HESPE, High Energy Solar Physics Dara in Europe grid 1 data, <4s time resolution