M1.0 flare of 22 Oct 2002 RHESSI observations of the M 1.0 solar flare on 22 October 2002 A. Berlicki 1,2, B. Schmieder 1, N. Vilmer 1, G. Aulanier 1 1)

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.)

THE IMPULSIVE X-RAY RESPONSE IN FLARE FOOTPOINTS TOMASZ MROZEK WROCLAW UNIWERSITY ASTRONOMICAL INSTITUTE POLAND.

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.

Soft X-ray heating of the chromosphere during solar flares A. Berlicki 1,2 1 Astronomický ústav AV ČR, v.v.i., Ondřejov 2 Astronomical Institute, University.

Cristina Chifor SESI Student Intern 2005 Solar Physics, Code 612 NASA/Goddard Space Flight Center Mentors: Dr. Ken Phillips & Dr. Brian Dennis FE AND FE/NI.

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

Solar flares and accelerated particles

Solar flare hard X-ray spikes observed by RHESSI: a statistical study Jianxia Cheng Jiong Qiu, Mingde Ding, and Haimin Wang.

1 Plasma flows during solar flares A. Berlicki Observatoire de Paris, Section de Meudon, LESIA (Astronomical Institute of the Wrocław University, Poland)

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.

RHESSI 2003 October 28 Time Histories Falling fluxes following the peak Nuclear/511 keV line flux delayed relative to bremsstrahlung Fit to 511 keV line.

24 Oct 2001 A Cool, Dense Flare T. S. Bastian 1, G. Fleishman 1,2, D. E. Gary 3 1 National Radio Astronomy Observatory 2 Ioffe Institute for Physics and.

Solar and Stellar Flares Hugh S. Hudson SSL, UC Berkeley 1 May

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

Working Group 2 - Ion acceleration and interactions.

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)

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.

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.

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

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.

SPD May 25, 2005 RHESSI soft X-ray imaging spectroscopy H. Hudson & A. Caspi (SSL/UCB) And B. Dennis & K. Phillips (NASA/GSFC.

Spectral Analysis and Energy Estimates in M/X Flares using RHESSI and SXI Amir Caspi 1,2, Säm Krucker 2, Robert P. Lin 1,2 1 Department of Physics, University.

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

Rapid Changes in the Longitudinal Magnetic Field Associated with the July gamma -ray Flare Vasyl Yurchyshyn, Haimin Wang, Valentyna Abramenko,

Distinguishing Between Thermal and Non-Thermal Electron Populations in Solar Flares Using RHESSI Amir Caspi 1,2, Robert P. Lin 1,2 1 Department of Physics,

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

Diagnostics and constraints for relativistic electron and ion acceleration in solar flares N. Vilmer LESIA –Observatoire de Paris Ascona_June

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.

RHESSI 4-8 April 06 Origin of > 100 GHz radio emission Gérard Trottet Laboratoire d’Etudes Spatiale et d’Instrumentation en Astrophysique (LESIA) Observatoire.

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

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

4 November 2003 Kaufmann et al Two questions raised by submm- observations presented by Kaufmann et al. 2004: By what mechanism(s) is the emission.

Neupert effect RHESSI analysis ot the Neupert effect A. Berlicki, R. Falewicz 1) Observatoire de Paris, Section de Meudon, LESIA, FRANCE 2) Astronomical.

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.

RHESSI Microflares Steven Christe 1,2, Säm Krucker 2, Iain Hannah 3, R. P. Lin 1,2 1 Physics Department, University of California at Berkeley 2 Space Sciences.

Locarno, 8 June 2005Peter Gallagher (UCD) Chromospheric Evaporation Peter Gallagher University College Dublin Ryan Milligan Queens University Belfast.

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

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.

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.

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

Energetic electrons acceleration: combined radio and X-ray diagnostics

Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan.

H α and hard X-ray observations of solar white-light flares M. D. Ding Department of Astronomy, Nanjing University.

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.

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.

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

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.

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.

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.

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

Physics of Solar Flares

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

SOLAR FLARE OPTICAL SPECTROPOLARIMETRY

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

Origin of > 100 GHz radio emission

Nonthermal Electrons in an Ejecta Associated with a Solar Flare

Presentation transcript:

M1.0 flare of 22 Oct 2002 RHESSI observations of the M 1.0 solar flare on 22 October 2002 A. Berlicki 1,2, B. Schmieder 1, N. Vilmer 1, G. Aulanier 1 1) Observatoire de Paris, Section de Meudon, LESIA, FRANCE 2) Astronomical Institute of the Wrocław University, POLAND

M1.0 flare of 22 Oct 2002 The aim of the work: Why the flare emission in cool chomospheric lines (H, Ca lines) is observed for a long time during the late phase of solar flares ? What kind of heating mechanism is effective during the gradual phase of solar flares ? * Small flux of non-thermal electrons ? * Thermal conduction ? * Radiative heating by soft X-rays ? We try to explain if the non-thermal component in X-ray emission could be present during the gradual phase of solar flares.

M1.0 flare of 22 Oct 2002 MDI - cont. BBSO - H-alpha

M1.0 flare of 22 Oct 2002 I CONT (Na D1,THEMIS) B LONG (NaD1, THEMIS) HXR (RHESSI) 22 oct 2002 TRACE 195 ang. H  flare (VTT) + RHESSI

M1.0 flare of 22 Oct 2002

Thermal + non-thermal + Fe/Ni line complex (6.7 & 8 keV)

M1.0 flare of 22 Oct 2002

Thermal and non-thermal component during the gradual phase a) Thermal energy of plasma: b) Energy contained in the non-thermal electrons (thin target model): (Hudson et al. 1978, Sol. Phys. 60, 137) (for E CUT-OFF = 10 keV)  - power-law index B(x,y) – beta function  10 – X-ray flux at 10 keV [photons cm -2 s -1 keV -1 ]

M1.0 flare of 22 Oct 2002 Thermal E th and non-thermal E nth energy contained in the flare of October 22, ? ? ?

M1.0 flare of 22 Oct 2002 Conclusions: 1) During the analysed period the thermal energy is dominant, 2) Non-thermal component provide a marginal input to the total energy but it is necessary to explain the spectra between 10 and 20 keV, ? ? ? * Thin or thick target, * Distinguish between thermal and non-thermal emission at low energies, * Relation between E cut-off and the energy contained in non-thermal electrons – very sensitive !