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Neutrino Astronomy
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SNRs

Slide 12

HESS: RXJ1713

HESS: RXJ1713

First resolved

TeV g-ray image of a

Shell type SNR (Resolution ~10 arcmin)

Acceleration source of Cosmic Rays, but is it evidence of

Protons?

Slide 13

HESS: RXJ1713  Molecular Clouds

HESS: RXJ1713 Molecular Clouds

Slide 14

RXJ1713 Spectrum

RXJ1713 Spectrum

In favor of p0:

no cut-off in the

HE tail of HESS

spectrum

signal from the

direction of

molecular clouds

See HESS Talk Tuesday Afternoon

Slide 15

Have g-rays from p0 decay been discovered?

Have g-rays from p0 decay been discovered?

En Nn (En) =  Eg Ng (Eg)

1 <  <

8

transparent

source

p0 = p+ = p-

accelerator

beam dump

(hidden source)

n flux predicted observed g-ray flux

~40 per km2 RX J1713-3946

per year (galactic center)

Slide 16

Milagro (TeV) Diffuse Source

Milagro (TeV) Diffuse Source

See Milagro Talk Tues Afternoon

Slide 17

Produces cosmic ray beam

Produces cosmic ray beam

Radiation field:

Active Galactic Nuclei

Slide 18

Active Galactic Nuclei (AGN)

Active Galactic Nuclei (AGN)

Slide 19

VLA image of Cygnus A

VLA image of Cygnus A

See Monday Morning AGN Session

Slide 20

GZK

GZK

g

p

n

p

n

n

n

E = 6 x10 19 eV

E ~4 x 10 19 eV

p + gCMB → p+ + n

= (ncmb s p + g )-1

l= 10 Mpc

Cutoff above 50 EeV

Slide 21

GZK

GZK

Cosmogenic neutrinos are guaranteed if primaries are nucleons.

May be much larger fluxes, for some models, such as topological defects

Slide 22

GZK

GZK

See Monday PM + Thurs AM Sess.

Slide 23

GRBs

GRBs

Slide 24

GRBs

GRBs

Shocks: external collisions with interstellar material or internal collisions when slower material is overtaken by faster in the fireball.

See Wed AM+ Thu PM GRB sessions

Slide 25

e-

e-

p+

R < 108 cm

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