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

Slides:

Advertisements

Similar presentations

RHESSI Investigations of the Neupert Effect in Solar Flares Brian R. Dennis AAS/SPD Meeting 6 June 2002.

Advertisements

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

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.

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

Microwave and hard X-ray imaging observations of energetic electrons in solar flares: event of 2003 June 17 Kundu, M R., Schmahl, E J, and White, S M.

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

Hard X-ray Production in a Failed Filament Eruption David, Alexander, Rui Liu and Holly R., Gilbert 2006 ApJ 653, L719 Related Paper: Ji. H. et al., 2003.

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.

Imaging with subcollimator 1. Dec 6, 2006 white light flare Hinode/SOT image during the main HXR peak! SOT resolution.

White-Light Flares: TRACE and RHESSI Observations H. Hudson (UCB), T. Metcalf & J. Wolfson (LMSAL), L. Fletcher & J. Khan (Glasgow)

Hard X-rays associated with CMEs H.S. Hudson, UCB & SPRC Y10, Jan. 24, 2001.

+ 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.

9th RHESSI Workshop, Sept. 1-5, 2009, Genova On Broken-up Spectra of RHESSI Flares Y. P. Li & W. Q. Gan Purple Mountain Observatory.

RHESSI Observations of the 29-Oct-2003 Flare. 29-Oct-2003 General Info 29-OCT-03 GOES Start: 20:37, Peak: 20:49, End 21:01 Size X10 Position S19W09 (AR486)

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

White-Light Flares: TRACE and RHESSI Observations H. Hudson (UCB), J. Wolfson (LMSAL) & T. Metcalf (CORA)

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.

FLARE ENERGETICS:TRACE WHITE LIGHT AND RHESSI HARD X-RAYS* L. Fletcher (U. Glasgow), J. C. Allred (GSFC), I. G. Hannah (UCB), H. S. Hudson (UCB), T. R.

Coronal HXR sources a multi-wavelength perspective.

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,

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

White-Light Flares and HESSI Prospects H. S. Hudson (UCB and SPRC) March 8, 2002.

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

The Yohkoh observations of solar flares Hugh Hudson UCB.

Late-phase hard X-ray emission from flares The prototype event (right): March 30, 1969 (Frost & Dennis, 1971), a very bright over-the-limb event with a.

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

Group V: Report Regular Members: K. Arzner, A. Benz, C. Dauphin, G. Emslie, M. Onofri, N. Vilmer, L. Vlahos Visitors: E. Kontar, G. Mann, R. Lin, V. Zharkova.

White-Light Flares via TRACE and RHESSI: Death to the thick target? H. Hudson, plus collaboration with J. Allred, I. Hannah, L. Fletcher, T. Metcalf, J.

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.

Energy-height relation for hard X-ray footpoint sources observed by RHESSI. TOMASZ MROZEK ASTRONOMICAL INSTITUTE, WROCŁAW UNIVERSITY.

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.

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

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.

High Resolution Imaging and EUV spectroscopy for RHESSI Microflares S. Berkebile-Stoiser 1, P. Gömöry 1,2, J. Rybák 2, A.M. Veronig 1, M. Temmer 1, P.

5 th RHESSI workshop, Locarno. WG 4 Report Participants: Steven ChristeSäm Krucker Brian DennisMonique Pick Lyndsay FletcherEd Schmahl Peter GallagherManuela.

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

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

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

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

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.

SH 51A-02 Evolution of the coronal magnetic structures traced by X-ray and radio emitting electrons during the large flare of 3 November 2003 N.Vilmer,

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

A Local Reacceleration Thick Target Model (LRTTM) (a modification of the Collisional Thick Target Model CTTM -Brown 1971) Brown, Turkmani, Kontar, MacKinnon.

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.

STUDY OF A DENSE, CORONAL THICK TARGET SOURCE WITH THE MICROWAVE DATA AND 3D MODELING Gregory Fleishman, Yan Xu, Gelu Nita, & Dale Gary 03/12/2015.

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

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.

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

Dong Li Purple Mountain Observatory, CAS

Physics of Solar Flares

Marina Battaglia, FHNW Säm Krucker, FHNW/UC Berkeley

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

RHESSI and H study of the X4 Flare of 3 Nov 2003

RHESSI Spectral Analysis of the 1N/M1.9 flare of 20 October 2003

TRACE Downflows and Energy Release

Teriaca, et al (2003) ApJ, 588, SOHO/CDS HIDA/DST 2002 campaign

Chromospheric and Transition Region Dynamics

Nonthermal Electrons in an Ejecta Associated with a Solar Flare

Presentation transcript:

Joint session WG4/5 Points for discussion: - Soft-hard-soft spectral behaviour – again - Non-thermal pre-impulsive coronal sources - Very dense coronal loops (~ cm -3 ) and other dense structures - Coronal sources that decrease in altitude (sometimes as footpoints approach), then increase - tiny inferred size of flare footpoints  high beam flux and implications

30-50 keV intensity keV / keV intensity ratio keV / keV intensity ratio Correlation between impulsive phase intensity and spectral hardness - ubiquitous Spectral soft – hard - soft

GOES 1-8 A DERIVATIVE Non-thermal preflare coronal sources

RHESSI Preflare Maps 3-12 keV (color): keV (contours) 01:07:00-01:08:30 01:08:00-01:10:30 01:11:00-01:12:30 Coronal source

RHESSI SPECTRA 5-50 keV Thermal+broken powerlaw Preflare period: 01:02:00-01:11:00 Broken powerlaw extends down to 5 keV Thermal component never dominates EM and T are poorly determined Chisquare ~ 1 if EM=0 White = photons, Green = thermal model, Red = broken powerlaw, Purple = background (NB similar source in July 23 rd 2002 event)

Dense coronal sources Substantial high energy emission in corona: thermal and radio observations allow estimate of density – cm keV30-50 keV keV 20 July 2002, pixon image reconstruction

Descending loop top sources Time evolution: blue  white Footpoints: keV Loop top: keV

H  footpoint separation HXR source ‘height’ Descending loop top sources – with decreasing footpoint separation

Flare footpoints – white light observations WL coincides with HXR source locations – sizes at resolution of TRACE (few px = few 1000 km  area ~ cm 2 )

M2.2 flare Predicted ‘evaporation’ velocity as function of beam flux Using A= cm 2 Using A= cm 2