shocks and fermi-i acceleration. non-relativistic shocks p 1, 1, t 1 p 0, 0, t 0 vsvs p 1, 1, t 1 p...
TRANSCRIPT
![Page 1: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/1.jpg)
Shocks andFermi-I Acceleration
![Page 2: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/2.jpg)
Non-Relativistic Shocks
p1, 1, T1 p0, 0, T0
vs
p1, 1, T1 p0, 0, T0
v0 = -vs
Stationary Frame
Shock Rest Frame
v1
![Page 3: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/3.jpg)
Particle Acceleration at Strong ShocksGeneral Idea:
Particles bouncing back and forth across shock front:
At each pair of shock crossings, particles gain energy
<E / E> = (4/3) V/c = U/c
p2, 2 p1, 1
U = vs
Stationary frame of ISM
v2 = (1/4) v1 v1 = -U
Shock rest frame
v1 1 = v2 2
1 / 2 = 1/4
Rest frame of shocked material
v2 ‘ = (3/4) Uv1‘ = (3/4) U
Write E = E0 = (1 + U/c) E0 ; = 1 + U/c
![Page 4: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/4.jpg)
Particle Acceleration at Strong Shocks (cont.)
Flux of particles crossing the shock front in either direction:
Fcross = ¼ Nc
Downstream, particles are swept away from the front at a rate :
NV = ¼ NU
p2, 2 p1, 1
U
Stationary frame of ISM
v2 = (1/4) v1 v1 = U
Shock rest frame
v1 1 = v2 2
1 / 2 = 1/4
Rest frame of shocked material
v2 ‘ = (3/4) Uv1‘ = (3/4) U
Probability of particle to remain in the acceleration region:
P = 1 - (¼ NU)/(¼ Nc) = 1 – (U/c)
![Page 5: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/5.jpg)
Particle Acceleration at Strong Shocks (cont.)
Energy of a particle after k crossings:
E = k E0
=> ln (N[>E]/N0) / ln (E/E0) = lnP / ln
or N(>E)/N0 = (E/E0)lnP/ln
Number of particles remaining:
N = Pk N0
=> N(E)/N0 = (E/E0)-2
![Page 6: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/6.jpg)
More General CasesWeak nonrelativistic shocks
p > 2
Relativistic parallel shocks:
p = 2.2 – 2.3
Relativistic oblique shocks:
Almost any spectral index possible
U
BU
U B U
![Page 7: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/7.jpg)
Diffusive Shock Acceleration
b afr
![Page 8: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/8.jpg)
Diffusive Shock Acceleration
![Page 9: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/9.jpg)
Electron Spectra from Diffusive Shock Acceleration
= *rg = Pitch-angle scattering mean free path
Moderately sub-luminal (1HT = 1x/cosBf1 < 1)
Marginally sub-luminal (1HT = 1x/cosBf1 ~ 1)
(Summerlin & Baring 2012)
![Page 10: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/10.jpg)
Asymptotic Particle Spectral Index
n
(Summerlin & Baring 2012)
![Page 11: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/11.jpg)
Effects of Cooling and Escape
= - ( ne) + Qe (,t) - ______ __∂ne (,t)
∂t∂
∂.
Radiative and adiabatic losses
Escape
______ne (,t)tesc,e
Particle injection (acceleration on very
short time scales)
Evolution of particle spectra is governed by the Continuity Equation:
![Page 12: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/12.jpg)
Effects of Cooling and Escape (cont.)
Assume rapid particle acceleration:
Q(, t) = Q0 -q 1 < < 2
Fast Cooling :
tcool << tdyn, tesc for all particles
N(
)
(q+1)
F(
)
q/2
Particle spectrum:Synchrotron or
Compton spectrum:
![Page 13: Shocks and Fermi-I Acceleration. Non-Relativistic Shocks p 1, 1, T 1 p 0, 0, T 0 vsvs p 1, 1, T 1 p 0, 0, T 0 v 0 = -v s Stationary Frame Shock Rest Frame](https://reader036.vdocuments.site/reader036/viewer/2022062511/5516c24f550346a25b8b6126/html5/thumbnails/13.jpg)
Effects of Cooling and Escape (cont.)
Assume rapid particle acceleration:
Q(, t) = Q0 -q 1 < < 2
Slow Cooling :
tcool << tdyn, tesc only for particles with > b
N(
)
q
(q+1)
b
F(
)
q
q/2
b
Particle spectrum:Synchrotron or
Compton spectrum:
11