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HESS: RXJ1713 First resolved

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

Slide 15

Have g-rays from p0 decay been discovered?

Have g-rays from p0 decay been discovered?

Slide 16

Milagro (TeV) Diffuse Source

Milagro (TeV) Diffuse Source

Slide 17

Active Galactic Nuclei

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

Slide 20

GZK

GZK

Slide 21

Cosmogenic neutrinos are guaranteed if primaries are nucleons.

Cosmogenic neutrinos are guaranteed if primaries are nucleons.

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

Slide 22

GZK

GZK

Slide 23

GRBs

GRBs

Slide 24

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

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

Slide 25

Active Galactic Nuclei

Slide 26

Generic GRB Explosion Models

Generic GRB Explosion Models

Slide 27

Lorentz Invariance Violation

Lorentz Invariance Violation

Bounds on energy dependence of the speed of light can be used to place

constraints on the effective energy scale for quantum gravitational effects.

E2-c2p2~E2x(E/EQG)a - This may be modified in some quantum gravity

models.

This has the important observational consequence that this will give

rise to energy dependent delays between arrival times of photons.

Slide 28

Galactic Microquasars

Galactic Microquasars

Slide 29

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