2. what can we learn from observations vahe petrosianth- · vahe petrosian stanford university work...
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Particle Acceleration in Astrophysics 2. What can we learn from observations
Vahe Petrosian
Stanford University
Work based on several PhD theses and collaborations with post doctoral fellows and colleagues
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Plasma properties
Turbulence spectrum
wave-particle interactions
Shock
Background density
Radiating electron spectrum
Acceleration Radiation Observation
The Problem
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Plasma properties
Turbulence spectrum
wave-particle interactions
Shock
Background density
Radiating electron spectrum
Acceleration Radiation Observation
The Forward Fitting Method
Forward Fitting
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Plasma properties
Turbulence spectrum
wave-particle interactions
Shock
Background density
Radiating electron spectrum
Acceleration Radiation Observation
The Inversion Method
Inverse process
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I. Description of a nonparametric inversion methodII. Applications of the Inversion Method A. Cosmic Rays and Supernova Remnant Spectra B. Solar Flare Hard X-ray emissions III. Some Interesting Puzzles of Ion acceleration A. Extreme enhancement of 3He and Heavy ions B. Electron spectra at Flare sites and observed at Earth
Outline
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Back to the Leaky Box Model (Steady State)
Two unknowns Therefore we need two spectral information
1. Accelerated Particle Flux 2. Escaping Particle Flux These Give the escape time
If there is no B convergence from this we can get
Then integration of the kinetic equation over E gives
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Back to the Leaky Box Model (Steady State)
Two unknowns Therefore we need two spectral information
1. Accelerated Particle Flux 2. Escaping Particle Flux These Give the escape time
from which we get Then integration of the kinetic equation over E gives
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Transport and Spectrum of Escaping Particles An Important Special Case
If particles lose all their energy in the transport region then
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Transport and Spectrum of Escaping Particles An Important Special Case
RecallRecall that
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Transport and Spectrum of Escaping Particles An Important Special Case
RecallRecall that
From These we can get the effective acceleration rate
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Plasma properties
Turbulence spectrum
wave-particle interactions
Shock
Background density
Radiating electron spectrum
Acceleration Radiation Observation
The Inversion MethodFor radiating sources the first step is to obtain particle
spectrum fromphoton spectrum
Inverse process
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We need to invert this to obtain
There are two methods that work well when the cross section is a simple function of photon and particle energies like bremsstrahlung and synchrotron. IC more complex but approximation can be used satisfying this requirements.
1. Generalized Inversion method by Piana et al.
2. The Johns-Lin method of matrix inversion
The Inversion MethodFor radiating sources the first step is to obtain particle
spectrum fromphoton spectrum
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Using Observed Radiation and Cosmic Ray Spectra
II-A. Application to Acceleration of Electrons in Supernova Remnants
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Supernova Remnant and Cosmic Ray ObservationsA. Toy Model
Sun
Cosmic-rays Observed near Earth This gives SNR radiation Observed near Earth gives
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Supernova Remnant and Cosmic Ray ObservationsA. Toy Model
Sun
Cosmic-rays Observed near Earth This gives SNR radiation Observed near Earth gives
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Spectra of Accelerated ElectronsFrom Radio and X-ray (and gamma-ray?) Observations
Hui, Li et al. 2010
Lazendic et al. 2004
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Effective Spectra of Escaping ElectronsTwo Interpretation of the Bump
Klein-Nishina Effect in IC Losses Nearby Pulsar Stawarz, Petrosian & Blandford Fermi Collabor. Abdo et al.
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Effective Spectra of Escaping ElectronsTwo Interpretation of the Bump
Klein-Nishina Effect in IC Losses Nearby Pulsar Stawarz, Petrosian & Blandford Fermi Collabor. Abdo et al.
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Escape Time: Two Methods
A.
B.
Injected Q obtained using e.g. GalpropFitting to the obseved CR spectrum
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RESULTS From Two Methods
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RESULTS: Scatering Time
Two methods of determining the coefficient or the scattering time
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Solid Curves from Escape timeDashed (SA) and Dotted (Shock) from Acceleration times
RESULTS: Scattering Time
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Scattering And Acceleration Times Interaction with Parallel Waves
Pryadko and Petrosian 1997
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Using Observed hard X-ray Spectra from Loop top and Foot points of
Flare Loops
II-B. Application to Acceleration of Electrons in Solar Flares
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Cartoon and Observation of a Flare Loop
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HXR:
Connected by Escaping Process
See Petrosian & Chen (2010)ApJ Letters, 2010, 712, 131
The Basic Solar Flare Model Relating Electrons and Photons
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Results From Inversion of the Kinetic Equation
(Petrosian & Chen, 2010 ApJ L, 712, 131)
From these we derive Energy Dependence of the diffusion rates
Both Coefficients Depend only on Observables
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Bremsstrahlung Hard X-ray Emission
Applying our inversion relations we get
and
or
Petrosian & Chen (2013) See recent astro-ph posting
The Basic Model: Relating Electrons and Photons
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RHESSI produces count visibility, Fourier component of the source
Defining electron flux visibility spectrum and count cross section
We getRegularized inversion produced smoothed electron flux visibility spectrum
Fourier Transform GivesPiana et al. 2007
Regularized Inversion of Photon Images to Electron Images
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2003 Nov 3 Flare(X3.9 class)
LT source detected up to 100-150 keV (Chen & Petrosian 2013)
HXR images by MEM_NJIT
Electron flux images by MEM_NJIT
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2003 November 3 Flare X3.9
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2005 September 8 Flare M2.1
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Escape and Scattering Times Theory and Empirical Determinations Effenberger and VP 2017 Chen & VP 2013
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Scattering And Acceleration Times Interaction with Parallel Waves
Pryadko and Petrosian 1997
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So How Do We Fix ItPossible Solutions
Weak Diffusion andConverging Field Lines at the Loop topEscape time (determined by scatterings into the loss cone) will increase with energy
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Trapped by a Magnetic Bottle
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Scattering And Acceleration Times Interaction with Parallel Waves
Pryadko and Petrosian 1997
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SUMMARY and CONCLUSIONS
1. For sources where observations give the Accelerated and Escaping Particle Spectra we can determine the basic acceleration parameters given the plasma characteristics using the newly developed inversion technique.2. The results from application to supernova remnants and cosmic ray observations are very promising.3. Application to RHESSI Imaging spectroscopic data show some new results.
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Extreme enhancement of 3He and heavy ions
III. Some Interesting Puzzle on Acceleration of Ions
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●2. SEP-Ion Spectra and 3He Enrichment “Impulsive” Events Mason et al. 2016 “Gradual” Events Desi t al. 2015
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●2. SEP ION Enrichments “Impulsive” Events Mason et al. 2016 Reames et al.
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He3, He4 Fluence RatiosNot bimodal: gradual variation with acceleration rate
Observations
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Resonant Wave-Particle Interactions4He and 3He
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B. He3, He4 Abundances and Spectra
(Liu, Petrosian and Mason, 2004 ApJ)
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He3, He4 Fluence RatiosNot bimodal: gradual variation with acceleration rate
Observations Model Results
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Flare accelerated He4 SpectraDo not agree with observed gradual events
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Diffusion Accel. Loss Escape Source by Turbulence by Shock and Turbulence
Observed SEPs
● Kinetic Equation The Leaky Box Model● Re-Acceleration at the CME Shock
Flare Accelerated Particles
Gradual or Delayed EventsRe-acceleration at the CME shock
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Solution with Source term flare accelerated electrons
Gradual or Delayed EventsRe-acceleration at the CME shock
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BUT Flare accelerated He4 Spectraafter re-acceleration at the CME-shock agree
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Numerical treatment of re-Acceleration
Re-acceleration timescales
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A. Electrons
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● 1. SEP and HXR Electron Spectra
“Impulsive; Prompt” “Gradual; Delayed” Events
Krucker et al. 2007
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● 1. SEP and HXR Electron Spectra Distributions of “Impulsive; Prompt” and “Gradual; Delayed”
VP 2016
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● 1. SEP and HXR Electron Numbers Correlations of “Impulsive; Prompt” Events only
Krucker et al. 2007
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● Escape up: SEPs ●
● Escape down: HXRs●
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● Impulsive or Prompt Events● Acceleration by Turbulence at the Flare Site
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New Direction: Motivated by two new results
Krucker et al. 2007
Strong diffusion
● Impulsive or Prompt Events● Acceleration by Turbulence only at the Flare Site
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New Direction: Motivated by two new results
Krucker et al. 2007
Weak diffusion
● Impulsive or Prompt Events● Acceleration by Turbulence only at the Flare Site
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New Direction: Motivated by two new results
Krucker et al. 2007
Relative numbers of RPP and SEP (electrons)
● Impulsive or Prompt Events● Acceleration by Turbulence only at the Flare Site
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Solution with Source term flare accelerated electrons
●Gradual or Delayed Events● Re-acceleration at the CME shock
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1. Inversion methods can determine the Fokker-Planck Coefficients directly and non parametrically from observed spectra.2. Both Shock and Stochastic Acceleration Driven by Turbulence Can Account For Many High Energy Astrophysical Phenomena.
SUMMARY and CONCLUSIONS 2
Slide 1Slide 2Slide 3Slide 4Slide 5Slide 6Slide 7Slide 8Slide 9Slide 10Slide 11Slide 12Slide 13Slide 14Slide 15Slide 16Slide 17Slide 18Slide 19Slide 20Slide 21Slide 22Slide 23Slide 24Slide 25Slide 26Slide 27Slide 28Slide 29Slide 30Slide 31Slide 32Slide 33Slide 34Slide 35Slide 36Slide 37Slide 38Slide 39A. SEPs and 3He EnrichmentSlide 41Slide 42Resonant Wave-Particle Interactions 4He and 3HeSlide 44Slide 45Slide 46Slide 47Slide 48Slide 49Slide 50Slide 51Slide 52Slide 53Slide 54Slide 55Slide 56Slide 57Slide 58Slide 59Slide 60