Your Name Your Title Your Organization (Line #1) Your Organization (Line #2) 2005-12-31 About technique of alignment and stacking of TGF Vybornov V. Pozanenko.

Slides:



Advertisements
Similar presentations
SPHINX DATA ANALYSIS Magdalena Gryciuk Astronomical Institute, University of Wroclaw Space Research Centre, Polish Academy of Sciences I SOLARNET SPRING.
Advertisements

RHESSI Investigations of the Neupert Effect in Solar Flares Brian R. Dennis AAS/SPD Meeting 6 June 2002.
Solar System Science Flares and Solar Energetic Particles Terrestrial Gamma-Ray Flashes Cosmic-ray interactions with Earth, Sun, Moon, etc. Plans: Optimization.
Terrestrial Gamma-Ray Flashes (TGFs) Observed with Fermi-GBM G. J. Fishman 1, M. S. Briggs 2, and V. Connaughton 2 -for the GBM TGF Team 1 NASA-Marshall.
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.
Workshop „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, RHESSI and SPIRIT Instruments”, 6 – 8 December 2005, Wrocław Spectroscopy Department.
Solar flares and accelerated particles
Page 1 Cristina Chifor (a) Ken Phillips (b), Brian Dennis (c) a) DAMTP, University of Cambridge, UK b) Mullard Space Science Lab, UK c) NASA/GSFC, Maryland,
Solar flare hard X-ray spikes observed by RHESSI: a statistical study Jianxia Cheng Jiong Qiu, Mingde Ding, and Haimin Wang.
satelliteexperimentdetector type energy band, MeV min time resolution CGRO OSSE NaI(Tl)-CsI(Na) phoswich 0.05–10 4ms COMPTELNaI0.7–300.1s EGRET TASCSNaI(Tl)1-2001s.
Hard X-Ray Footpoint Motion in Spectrally Distinct Solar Flares Casey Donoven Mentor Angela Des Jardins 2011 Solar REU.
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.
Page 1 18-OCT-2004 RHESSI Data Analysis Workshop RHESSI Reuven Ramaty High Energy Solar Spectroscopic Imager Use or disclosure of data contained on this.
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.
RHESSI Observations of Gamma- Ray Lines from Solar Flares Albert Y. Shih 1, David M. Smith 2, Robert P. Lin 1, Richard A. Schwartz 3, Gerald H. Share 4,
F.Fuschino, F.Longo et al AGILE view on TGF F. Fuschino, F. Longo, M. Marisaldi, C. Labanti, M. Galli, G. Barbiellini on behalf of the AGILE team.
+ Hard X-Ray Footpoint Motion and Progressive Hardening in Solar Flares Margot Robinson Mentor: Dr. Angela DesJardins MSU Solar Physics Summer REU, 2010.
Working Group 2 - Ion acceleration and interactions.
Terrestrial Gamma-ray Flashes. Gamma Ray Astronomy Beginning started as a small budget research program in 1959 monitoring compliance with the 1963 Partial.
RHESSI/GOES Observations of the Non-flaring Sun from 2002 to J. McTiernan SSL/UCB.
RHESSI/GOES Xray Analysis using Multitemeprature plus Power law Spectra. J.McTiernan (SSL/UCB)
RHESSI/GOES Xray Analysis using Multitemeprature plus Power law Spectra. J.McTiernan (SSL/UCB) ABSTRACT: We present spectral fits for RHESSI and GOES solar.
Reuven Ramaty 1937 – RHESSI people UC Berkeley (Bob Lin) NASA GSFC (Brian Dennis) Paul Scherrer Institute (Alex Zehnder) Co-Is Benz, Brown, Emslie,
Accelerator hall of the S- DALINAC – electron energies from 2 to 130 MeV available – cw and pulsed beam operation possible – source for polarized electron.
Page 1 18-APR-2002 RHESSI Data Analysis Workshop RHESSI Reuven Ramaty High Energy Solar Spectroscopic Imager Use or disclosure of data contained on this.
RHESSI Background Spectra Vs Time. Qlook_bck Spectra have 491 energy channels, 1/3 keV resolution from 3 to 100 keV, 1 keV from 100 to 300 keV. Accumulated.
Temporal Variability of Gamma- Ray Lines from the X-Class Solar Flare of 2002 July 23 Albert Y. Shih 1,2, D. M. Smith 1, R. P. Lin 1,2, S. Krucker 1, R.
Spectrum of Accelerated Particles Derived from the MeV Line Data in Some Solar Flares Leonty I. Miroshnichenko (1, 2), Evgenia V. Troitskaia (3),
Confirmation of extended annihilation-line emission in 2005 January 20 flare: Earth occultation. DayNight.
Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,
AGATA Demonstrator Test With a 252 Cf Source: Neutron-Gamma Discrimination Menekşe ŞENYİĞİT.
GLAST Simulations Theodore E. Hierath Louisiana State University August 20, 2001.
The Project of Space Experiment with Wide Field Gamma-Ray Telescope (“GAMMASCOPE”) Skobeltsyn Institute of Nuclear Physics, Moscow State University.
High Energy Measurements for Solar, Heliospheric, Magnetospheric, and Atmospheric Physics R. P. Lin J. Sample, A. Shih, S. Christe, S. Krucker, I. Hannah.
Lyndsay Fletcher, University of Glasgow Ramaty High Energy Solar Spectroscopic Imager Fast Particles in Solar Flares The view from RHESSI (and TRACE) MRT.
A Imaging Parameters A Imaging Parameters A
HESSI Science Objective  Impulsive Energy Release in the Corona  Acceleration of Electrons, Protons, and Ions  Plasma Heating to Tens of Millions of.
Future usage of quasi-infinite depleted uranium target (BURAN) for benchmark studies Pavel Tichý Future usage of quasi-infinite depleted uranium target.
INTERNATIONAL STANDARDIZATION ORGANIZATION TECHNICAL SPECIFICATION Space Environment (Natural and Artificial) Probabilistic model of fluences and.
X.-X. Li, H.-H. He, F.-R. Zhu, S.-Z. Chen on behalf of the ARGO-YBJ collaboration Institute of High Energy Physics Nanjing GRB Conference,Nanjing,
KIM TOLBERT THE CATHOLIC UNIVERSITY OF AMERICA AND GODDARD SPACE FLIGHT CENTER FERMI Solar Data Availability and Quicklook Plots Fermi Solar Data Analysis.
Extended emission in short gamma-ray bursts registered by SPI-ACS of INTEGRAL observatory Pavel Minaev 1, 2, Alexei Pozanenko 1, Vladimir Loznikov 1 1-
Studies on the 2002 July 23 Flare with RHESSI Ayumi ASAI Solar Seminar, 2003 June 2.
Regularized Mean and Accelerated Electron Flux Spectra in Solar Flares Eduard P. Kontar University of Glasgow Michele Piana, Anna Maria Massone (INFM,
Spectra of the Thunderstorm Correlated Electron and Gamma-Ray Measured at Aragats Bagrat Mailyan and Ashot Chilingarian.
GLAST's GBM Burst Trigger D. Band (GSFC), M. Briggs (NSSTC), V. Connaughton (NSSTC), M. Kippen (LANL), R. Preece (NSSTC) The Mission The Gamma-ray Large.
Regularized Mean and Accelerated Electron Flux Spectra in Solar Flares Eduard P. Kontar University of Glasgow Michele Piana, Anna Maria Massone (INFM,
NASA 2001 Mars Odyssey page 1 Workshop HEND Russian Aviation and Space Agency Institute for Space Research Present knowledge of HEND efficiency.
Russian Aviation and Space Agency Institute for Space Research NASA 2001 Mars Odyssey page 1 Workshop HEND Radiation environment on Odyssey and.
The Lag-Luminosity Relation in the GRB Source Frame T. N. Ukwatta 1,2, K. S. Dhuga 1, M. Stamatikos 3, W. C. Parke 1, T. Sakamoto 2, S. D. Barthelmy 2,
Observation of cosmic gamma-ray bursts and solar flares in the ''RELEC'' experiment on the ''VERNOV'' satellite.
TGF diffuse imaging and spectra as a function of altitude and location P.H.Connell University of Valencia.
RHESSI and the Solar Flare X-ray Spectrum Ken Phillips Presentation at Wroclaw Workshop “ X-ray spectroscopy and plasma diagnostics from the RESIK, RHESSI.
2001 Mars Odyssey page 1 W o r k s h o p H E N D Institute for Space Research, June , 2003 HEND physical calibrations: status report A. Kozyrev,
An electron/positron energy monitor based on synchrotron radiation. I.Meshkov, T. Mamedov, E. Syresin, An electron/positron energy monitor based on synchrotron.
Normal text - click to edit 1 Corsica N. Ostgaard 1, J. Stadsnes 1, P. H. Connell 2 T. Gjesteland 1 1) Department of Physics and Technology, University.
Fermi GBM Observations of Gamma-Ray Bursts Michael S. Briggs on behalf of the Fermi GBM Team Max-Planck-Institut für extraterrestrische Physik NASA Marshall.
Simulation of Terrestrial Gamma Ray and Neutron Flashes (Small variations of thundercloud dipole moment) L.P. Babich, Е.N. Donskoĭ, A.Y. Kudryavtsev, M.L.
A New Solar Neutron Telescope working at the International Space Station K. Koga, T. Goka (PI), H. Matsumoto, T. Obara, O. Okudaira (JAXA) Y. Muraki (Nagoya)
Fermi Gamma-ray Burst Monitor
CME – Flare Relationship A survey combining STEREO and RHESSI observations S. Berkebile-Stoiser B. Bein A.Veronig M. Temmer.
for Lomonosov-GRB collaboration
Physics of Solar Flares
Solar gamma-ray and neutron registration capabilities of the GRIS instrument onboard the International Space Station Yu. A. Trofimov, Yu. D. Kotov, V.
The Crab Light Curve and Spectra from GBM: An Update
Organizers: Mihir Desai, Joe Giacalone, Eric Christian
Study of 20 January 2005 solar flare area by certain gamma-ray lines
GRB spectral evolution: from complex profile to basic structure
GRB spectral evolution: from complex profile to basic structure
Conditions for Production of Terrestrial Gamma Ray Flashes (TGF)
Presentation transcript:

Your Name Your Title Your Organization (Line #1) Your Organization (Line #2) About technique of alignment and stacking of TGF Vybornov V. Pozanenko A. Minaev P. Space Research Institute Moscow, Russia 24 September 2014, TEPA-2014

2 Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) Launched in germanium detectors Energy band 3 keV — 17 MeV Orbit: 600 км, 38° Spectral resolution 3 keV at ~1 MeV Write each photon Scientific goals: Investigation of physics of solar flares and penetration accelerated particles from the Sun Investigation of gamma-ray bursts

3 Idea of stacking method Problem: Each event has too little number of counts to build time profile and spectrum Method: Counts stacking to increase statistics (under assumption that all events have the same nature) pluses: there is possibility to build and study averaged time profile and spectrum in any event group minuses: lose information about each event and its individual features Example event from the RHESSI TGF catalog

4 Stacking method: moving total Moving total of counts with window 0.2 ms window

5 Stacking method: search of event center search central time of event in window with max. number of counts Window with max. numbers of counts calculating central time t0t0

6 Stacking method: event alignment Alignment the event from of event central time

7 Stacking method: stacking + + normalized time profile

8 Stacking method: check method correctness If resulting time profile is averaged time profile? ?≈?≈ + + N hypothetical time profile normalized time profile

9 Stacking method: Monte-Carlo simulation of event like TGF + + Event as a non-homogeneous Poisson process +... normed time profile Function of non-homogeneous Poisson process rate Lewis & Shedler, 1978

10 Stacking method: Monte-Carlo simulation of event like TGF real simulated

11 Stacking method: test the method Dependence of stacking method error from event power correspond to faintest group in the catalog

12 A method of building of time profiles and spectra of TGF based on event stacking has been worked out Method correctness was tested in Monte-Carlo simulation Error of the method for faintest TGFs from the RHESSI catalog is no more then 10% Results

13 Thank you for attention!