The Most Exotic Physics of the Universe:

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The Most Exotic Physics of the Universe

• Bright matter and Bright energy.
• The largest Free Energy of the Universe.
• Almost all the Baryons of the Universe.
• Physics at the event horizon (GR).
• The most energetic matter, (CRs).
• Non relativistic, relativistic, and
  magneto-hydrodynamics.
• Particles, fields, and ultimately Information.
• The Ultimate Physics Sandbox

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A Massive Black Hole,A Keplerian accretion
disk,An ??? Dynamo, Helical Magnetic Jets,
Radio Lobes, Cosmic Rays and A Magnetized
Universe

• Stirling Colgate, Hui Li, Philipp Kronberg,
  Nathan Currrier, LANL
• Vladimir Pariev, U. Wis.

I believe that all these phenomena are tightly
connected by a sequence of physical phenomena.
Each one is critical, but perhaps only partially
understood.
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The starting point A thin, flat rotation curve
(FRC, Mr) proto-galactic disk forms with a
central black hole.

• Close to the MBH, where Mass (MBH) gt Mass
  (disk,ltr) must be Keplerian, i.e., with large
  differential rotation and thin,
• H10-4 r. Possibly a thick, ADAF disk, rlt 10
  rg .
• 2) A Keplerian disk allows the possibility of two
  instabilities
• semi-coherent, 2-D transport of both angular
  momentum and poloidal magnetic flux by 2-D,
  semi-coherent vortices, the RVI instability. This
  transport, radially, is faster than (3-D)
  turbulence by the ratio (r/H) 104.
• (B) An ??? dynamo creates an exponential in time,
  coherent, poloidal and toroidal magnetic flux,
  which grows to a back-reaction limit.

4
The best calculation of a Rossby vortex unstable
disk, Li et al.2001
7 orbits Entropy change 10-5
3 orbits Entropy change 10-1
Why? Only 2-D transport likely satisfies the
necessary angular momentum and magnetic flux
transport in the disk near the MBH.
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Weather vortices, Rossby waves in earths
atmosphere our local accretion disk wave length
gt 100 H, H atmosphere scale height 10 km.
Radial pressure gradient makes RVI transport of
atmospheric angular momentum.
/
Thermal convection radial flow
Accretion disk, H/r 10-4, 3-D turbulent
diffusion Diff (H cs/3) cm2/s. Time for the
diffusion of angular momentum r2 / Diff (r/H)
(3r/cs) 108 years (life-time of quasar), even
at small r 0.03 pc 1017 cm, or at 3x10-3 of
MBH mass. Instead we have 2-D diffusion, x 104
faster.
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Radio lobes must be magnetic and with a very
large magnetic flux. There must be a dynamo.
Hydra A, Faraday rotation, plus and minus,
and within x-ray cluster density, B10-4G and
polarized. Field radio lobe Polarization. Synchr
otron emission. Faraday rotation. X-rays from
comptonized black body radiation. Minimum
energy Ee ne B2 /8 ? , ? 104
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X-rays (polarized), collimation r/L 10-3The
jets feed the lobes with small loss.X-rays must
be magnetic synchrotron emission min E B104
G, ? 104. Lobes B10-4 G, ? 104.
Pictoris-A
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Thin Disk, H/r 10-4 and a few stars The
helicity of the dynamo.
A disk is thin, H/r 10-4, because the disk
black body radiation temperature is small in
equilibrium with viscous heating regardless of
the mechanism. (A thick ADAF disk may exist, r
lt 10 rg, T 100 Mev).
In addition a few stars, 10-3 mass fraction,
the metalicity, or 105 stars remain in orbit
plunging through the disk making plumes of hot
and then cooling matter, the origin of the broad
emission and absorption lines and the helicity of
the dynamo.
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The Ideal Helicity
Water flow experiment, Beckley et al. APJ 2003
Helicity is a coherent rotation and translation,
1/4 turn. h v . curl v A plume that
translates axially and rotates in the same
direction every time an average angle of pi/2
radians is an ideal source of helicity. Magnetic
plumes have no mass and hence no torque.
Side view
Top view, Rotating frame
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Dynamo Theory Flux, Mean Field, Simulation
Numerical simulation of the ??? dynamo. Axial
vector representation.
Pariev, IV, Colgate, SA., and Finn, JM., 2007,
APJ, 658 129
1012 turns, e10000000 (no seed)
2 plumes, a pair, every 6 revolutions gives
positive gain. Gain 0.06 ???????? turn.
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A Flux Conversion Picture
Poloidal flux
Return flux
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The ????????? Experiment
Azimuthal multiplication B? Rm/2? Bradial
20 Bradial
1011 turns, gain e1010, i.e., no seed field
needed. Back reaction limited.
1 meter diameter, stable Couette flow Re 2x107
, Rm 120, Helicity a pair of driven plumes
in liquid sodium. Power 20 kw at 70 Hz. Slip
rings for power and capacitative data
transmission.
Stable Couette flow Differential rotation.
Keplerian Disk, 10 pc rg 3 AU, 4 x 1013
cm Helicity plumes from Star-disk collisions
Helicity pulsed jets In rotating frame.
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Toroidal Magnetic Flux is Advected into the Black
Hole
Poloidal current is interupted at the event
horizon. A displacement current, dE/dt, replaces
Jz , and the Azimuthal flux enters the horizon as
a giant photon.
Azimuthal flux does not accumulate inside the
disk.
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Poloidal Magnetic Flux Accumulatesby Advection
independent of the BH.
(possible frame dragging)
Azimuthal flux must cross the poloidal flux by
diffusion, presumably (2D), RVI? The result is
the release of the advection energy making a
pair fire ball, T, h? few hundred Kev, or
perhaps an ADF disk.
Pair fireball, ne ltlt n??? 2-D diffusion allows
matter and B??-flux to cross poloidal flux.
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How the dynamo makes a helix
A dynamo generates poloidal and toroidal
flux. The Keplerian motion winds up the poloidal
flux outside the disk and makes a force-free
helix, (jet). Instability makes a spheromak, a
radio lobe, the magnetic fields of the universe
. The Keplerian motion winds up the internal
radial flux within the disk making an enhanced
toroidal field. The plumes driven by star disk
collisions are a unique source of helicity that
translates and rotates by ?/? this toroidal
flux into the poloidal plane. Two coherent
fluid motions make the dynamo possible.
Turbulence must be weak.
Force-free field Grad-Safronoff J(perpendicular)
0 J(parallel) curl B Not a mass-dominated
jet. Hui Li et al., 2001, ApJ., 561,915 A
self-luminous force-free Helix, 1018 amperes.
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Formation of helix
Idealized stabilized pinch
Bz Bo
(An approximation)
-
-
B? Bo (r0/r)


r1
r0
I? Bo amperes/cm length Iz 5 ro Bo 1018
amperes
Energy (Bo2/8?)(?r02)(12 ln(r0/r1)) Inductance
L L0 (12 ln(r0/r1)) very, very insensitive
to r1 .
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Current Carrier Starvation

• Force-free helical field pressure, PltltB2/8??
• J

gtgt J
grad P B0 J
Power J E
B02 c or 1020 volts/turn.
E ?J
Bc 3 x 106 volts/cm or r0 E 1020 volts/turn.
If ne r02 c lt I if r0 3 rg 1014 cm, then
ne 0.1/cc .
This is called an interruption in tokamak
research A beam of 105 amperes, 1/2 the
azimuthal field energy, at 10 Mev per proton,
drills a hole in the liner and the director
general is fired.
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Why current carrier starvation?
5. A. Dimits et al., Phys. Rev. Lett. 77, 71
(1996). 6. Z. Lin et al., Science 281, 1835
(1998). 7. W. Dorland et al., Phys. Rev. Lett. 85
5579 (2000). 8. J. Candy, R. E.Waltz, Phys. Rev.
Lett. 91, 045001(2003). The lines of force
wander out, run-aways, v , follow the lines
out particles returning must emit their
magnetic moment, v the hard way, a diode.
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Total Energy of Cosmic Rays

• -2.7, galaxy
• -2.6 extra galactic
• Spallation 10 loss
• per e-fold

WCR 8x1015 ergs cm-3 X 1074 cm3 8x1059
ergs
Progressive leakage from Galaxy to
metagalaxy Protons to iron to protons
Acceleration in force-free fields
dN/N - G?dE/E , N N0 E-G
CRs lossed to voids in 1/100 Hubble time. ?
GZK cut-off
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What to think about

• The initial mass distribution FRC or Keplerian?
• The Transport of angular momentum 2-D or 3-D?
• The production of magnetic flux a coherent or
  incoherent dynamo?
• The loss or accumulation of magnetic flux in the
  MBH?
• The winding of external flux to make a helix.
  Where are the turns made, stability?
• The conversion of magnetic energy to particle
  energy, E parallel acceleration?

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This is what is there
Hydra radio lobes (inside) Rotation Measure
---B E (B2/8???x Vol 1058 ergs
3C219 Radio Lobe, (intergalactic)
MBH c2 1062 ergs, Source of energy
field
Hy
High z
clusters
Hydra radio lobes outside the Hydra Cluster, E
1060 ergs. (Burbidge, 1953) min energy B2/8?
ne? mec2 ? 3x 104 B 10-5G.
1 Mpc Frequency 1010 Hz Llobe
1045-46 ergs/s few MBH c2 / 108 years
Galaxy energy 1055 ergs Insignificant energy
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2-D vortices and 3-D Turbulence
3-D turbulence will not make a MBH accretion
disk, will not transport angular momentum fast
enough in a thin, (H/r 10-4 ) disk. (c/4) aT4
(area) dM/dt c2. 3-D turbulence will not make a
dynamo but will dissipate magnetic flux faster
than dynamo gain, i.e., turbulence makes
resistivity. (Three liquid sodium
experiments). Ddiff (1/3) ?turbvturb ?
resistivity. Helmholtz shear instability ,
vturb vshear /3. Then magnetic Reynolds number
of unconstrained shear flow Rmshear vshear
?turb / ? 9, a value 1/2 Rmcritical of
optimum dynamo flow, (Dudley-James). A liquid
sodium experimental demonstration of an ???
dynamo is being attempted. The most efficient
mechanism for the transport of angular momentum
by purely hydrodynamic means in a thin
(rotating) atmosphere is 2-D vortices, i.e.,
Rossby vortices, RVI. Best example is weather on
earth. An experimental demonstration is being
attempted with a Rankine-Hilsch tube.
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Self-gravity waves and Rossby vortices in an
Accretion disk
Galaxy formation starts with the invisid collapse
of a uniform, constant omega rotating gaseous
cloud leading to a flat rotation curve disk and
Self Gravity Instabilities. Only after a
neutron star or BH forms will a Keplerian disk
appear.
2-D calculations, Keplerian, radial pressure,
gradient, Numerical dissipation, 10-7 per
turn. Alpha few . Hui Li, et al., 2001, ApJ
551, 874.
2-D calculations, self gravity, Flat rotation
curve, m r , Sigma 1/r .. N. Currier, SAC,
in rev.
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Dynamo Differential rotation, plumes, and
star-disk collisions
Poloidal flux lines, - 1 Mpc Foot prints wound
1012 times in 108 years Gain exp(1010) a
google, i.e., no seed needed..
105 stars in orbit, 10-3 metalicity, covering
factor 1. The sum of these loops of flux
104 per turn polloidal flux.
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The whole Enchilada, (105 stars in orbit 10-3
mass fraction metalicity)
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A water simulation Experiment to demonstrate the
Formation of helicity by the rotation of
plumes rising In a rotating frame. (Beckley et
al., 2003, ApJ.,599,702).
Helicity, H v (curl v), is necessary, but not
sufficient for an ????dynamo Need just 1/4
turn, not 100.
Expanding Plumes
Plume unwinds relative to frame.
Mixing, steady plume
Pulsed jet
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The black hole selectively advects toroidal
flux.No Back-reaction limit Plume pressure gt
Btoroidal2/8?
Inductance L 106 henries I 1018 amperes L
dI/dt 1020 volts Current closes through fire
ball. T 100 kev, ??????? ohms. Fire Ball
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Poloidal flux accumulates up to the back-reaction
limit of the BH (???of the Black Hole 377
ohms) Back-reaction limitPlume pressure
Bpoloidal2/8?
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The drive, clutches, belts Break, tachometers --
Outer cylinder, Motor, electronics Oil
heater-resevoir,
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?-phase dynamo, experiment, MRI and Stable
Couette Flow
Pipe flow turbulence torque
Measured torque
Ekman torque, theory
First the ??gain Rm/2? 20 . Second MRI
makes weak turbulence. With Rm 120, 6 modes
will be excited. Does this turbulence create a
dynamo of gain gt 10-4 ?? Third add driven
plumes do they create a dynamo with a gain gt
10-4 ?? Expect gain 6 x 10-2 ? (Pariev)
Measured torque 10 of pipe flow turbulent
stress, pipe flow stress cf v2 , cf 1/400
at Rey 107. Ekman flow creats a smaller torque,
balanced by weak, (back ground) turbulence. The
experiment was designed on the basis of Ekman
torque alone. No tubulence is created by
Keplerian flow alone.
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Pariev, Vladimir, et al. Magnetohydrodynamics
38,129 astro-ph/0112541 2007, ApJ., 658, 120, 129
Numerical simulation of the ????dynamo.
Gain 0.06 ? Calculated three ways Flux
deformation Mean field theory Vector potential
numerical simulation.
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The Rossby Vortex Instability, (Hui Li)
Transport of Angular Momentum
Transport is progressive, R, not diffusive by
MFP H, the thickness of the disk. Critical
thickness, cooling, ?critical 100 g/cm3
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Hilsch tube experimentExpect to reproduce the
hot and cold stream with a free-running turbine.
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Filament Supported by Magnetic Pressure
32 Mpc
Ryu, Kang, Bierman
Structure formation supported by Magnetic
pressure. B2/8? in-fall pressure From the
voids. B 10-6 G. Helix makes x5 this flux, lost
to voids. Faraday Rm bkg requires 25 reversals
per Mpc.
void
galaxies
cluster
tCR 108 years lt tGZK
Emax 1022 eV
In situ acceleration isotropic
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Summary of Astrophysics

• The largest free energy is due to black hole
  formation.
• 2) Angular momentum from structure formation
  determines this energy.
• 3) Dynamo and twist converts this energy into
  force-free magnetic energy.
• 4) A fraction of this magnetic energy is
  converted to cosmic rays.
• 5) Flux and cosmic rays are lost to the voids.
• 6) Magnetic pressure maintains and alters cosmic
  structures.

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Summary of physical processes
2-D vortices make a large enough diffusion
coefficient for a MBH accretion disk. 3-D
turbulence is too small. Star-disk collisions
make sufficient coherent helicity that combined
with Keplerian differential rotation makes a
dynamo. The back-reaction limit is determined by
the plume pressure and limiting polloidal
flux. Azimuthal flux is advected into MBH
producing a pair fire-ball. Current carrier
starvation by MBH gravity and tangled field
loss converts force-free field to accelerated
particles.