Space Monkeys and How to Destroy Them

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Space Monkeys and How to Destroy Them

• Presenter Paul Edmon
• Graduate Student Colloquium
• 2-27-08

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Overview

• Space Monkeys and the Threat to Spacetime
• History of Anti-Space Monkey Warfare
• Current Advances in Anti-Space Monkey Weaponry
  and Tactics

Courtesy of Anne-arky
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MHD, Radiative Transfer, and Particle Acceleration

• Presenter Paul Edmon
• Graduate Student Colloquium
• 2-27-08

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Who Am I?

• 4th Year Graduate Student
• Advisor Tom Jones
• Currently ABD
• Live Over in Beautiful Walter Library
• Work on Numerical Modeling of Particle
  Acceleration in Astrophysical Shocks

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Curriculum Vitae

• BS in Physics from University of Washington
• Advisor Jeff Wilkes
• Washington Area Large Telescope Array
• Interests
• Physics Particle Acceleration, MHD and Plasmas,
  Radiation, Nuclear Physics, Kinematics
• Astronomy Sun and Stars, Solar and Stellar Wind,
  Magnetosphere, Supernovae, Novae, Colliding
  Galaxies, Binaries, AGN, Planets and Moons,
  Cosmic Rays, Astrometry
• Other History, Mythology, Music, Theology,
  Philosophy, Technology, and General Nerdiness

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Work at the U of M

• Cosmicp Radiation Code
• Modeling SN 1006 (Preliminary Oral Exam)
• Modeling Type Ia Supernovae (Paper In Progress)
• Emissions from CR MHD Shocks (ICRC Paper)
• AstroBEAR and 2-D CR Acceleration in Stellar
  Winds and Supernovae (In Progress)

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Cosmicp

• A General Purpose Non-Thermal Radiation Code
• Processes Included in Cosmicp
• Synchrotron
• Inverse Compton (IC)
• Bremsstrahlung
• Photopair Production
• Photopion Production
• Proton-Proton Interactions
• Photodisintegration
• Catastrophic Losses
• Knock-on Electrons
• Coulomb and Ionization Losses
• Decay Processes

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Cosmicp Test GZK

• Greisen-Zatsepin-Kuzmin cutoff (Greisen 1966,
  Zatsepin Kuzmin 1966)
• Loss mechanism off of the CMB involving Photopair
  and Photopion production
• Limits the range that UHECR can travel and what
  can produce them

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Cosmicp Test Galactic Losses
Plasma
Plasma
Photopair
Synchrotron
Ionization
Bremsstrahlung
ICE
Proton-Proton
Photopion
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Diffusive Shock Acceleration (DSA)

• Model
• A thermal population of protons enter the shock
• Protons from the high energy tail diffuse through
  the shock scattering off of Alfvén waves
• Maximum possible accelerated energy is limited by
  the physical extent of the system and gyroradius
  of the proton

u1
u2
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CRASH

• DSA Model by Kang Jones (2006)
• CRASH (Cosmic-Ray Amr SHock)
• AMR shock code for Quasi-Parallel Shocks
• Flexible momentum binning
• Uses Sedov-Taylor similarity solutions for
  initialization
• Uses Bohm-like diffusion and is spherically
  symmetric
• Use CRASH and Cosmicp to model Supernova Remnants
  (SNR)
• Confirm Theory
• Get a handle on how real life SNRs behave and
  what to expect from them

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Supernova Ia and SN1006

• Supernova Ia
• Detonation of a White Dwarf
• The resulting SNR expands into a relatively
  undisturbed ISM
• SN1006 (Winkler et al. 2003)
• Went off in AD 1006
• G.326.614.6
• D2.2kpc
• z555pc
• R6.8kpc
• R10pc
• Vs2800 km/s

Courtesy of J. Hughes et al.
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Model for SN1006

• Age 1000 years
• Radius 10 pc
• Electron-Proton Ratio 1100
• 4 Part Ambient Photon Field (Model taken from
  Bloemen 1985)

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Case A
ICE
Synchrotron
p0 Decay
Bremsstrahlung
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Supernova Ia Models

• Based on CRASH runs by Kang (2006)
• Used a 4 part Ambient Photon Spectra
  (Schlickeiser 2002)
• Times plotted are t.6, 1, 3, 6, 10

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Overall Photon Spectra
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Phase Space Movie
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SNIa Discussion

• Should see gamma-rays from pion decay in the
  region between 100 MeV and 1 GeV if the ambient
  density is over .01 cm-3
• One can estimate the magnetic field strength of
  the shock by taking the ratio of the peak
  synchrotron power to the peak IC power
• The first order electron energy loss model
  matches the integrated spectrum well but fails to
  properly replicate the spatial profiles

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The Future AstroBEAR and CGMV

• Coarse Grained finite Momentum Volume (CGMV)
  (Jones Kang 2005)
• Solves the Diffusion-Convection equation with an
  order of magnitude less bins
• Takes advantage of the fact that the particle
  spectrum is going to be a power-law
• Works with the first two moments of the
  Diffusion-Convection equation
• Astronomical Boundary Embedded Adaptive
  Refinement (AstroBEAR) (Cunningham et al. 2007)
• AMR version of MHD TVD

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Kelvin-Helmholtz (Weak Field)

• Magnetic Field Movie Goes Here

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Kelvin-Helmholtz (MA5)

• Magnetic Field Movie Goes Here

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The Plan

• Make CosmicBEAR by adding CGMV to AstroBEAR
• Currently working on magnetic field matching
  across a boundary
• Model 2-D DSA
• Stellar Winds
• Colliding Stellar Winds
• Supernova Type II
• Get Ph.D.
• Stop Space Monkeys from Destroying Spacetime
• This is Madness!

Courtesy of the HESS Collaboration
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THIS IS SPARTA!!!