Cosmic Rays Liz Puchnarewicz Mullard Space Science Laboratory University College London www.mssl.ucl.ac.uk.

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Presentation transcript:

Cosmic Rays Liz Puchnarewicz Mullard Space Science Laboratory University College London

What are they? photons = light packets atomic fragmen ts proton neutro n electro n ion …moving very fast!! atom

Stripping an atom

ion = “stripped” nucleus massive (compared to protons, neutrons and electrons. And photons) positively charged

Energizing to CRs photons mass-less, v=speed of light particles e -p+n Z+ light medium heavy … so need to accelerate particles to speeds close to the speed of light

Accelerating particles How are particles pushed to the speed of light? Slung out by the enormous gravitationa l potentials of black holes Thrown out by massive stellar explosions - supernova e Dragged out by intense electric and magnetic fields – eg in pulsars

hydrogen helium Supernovae silicon carbon helium iron

hydrogen helium Supernovae carbon silicon helium iron

Supernovae

Crab Nebula Hubble (red) and Chandra (blue) composite of the Crab Nebula. The progenitor star went supernova about 1000 years ago.

A cosmic blast wave M. DeBord, R. Ramaty and B. Kozlovsky (GSFC), R. Lingenfelter (UCSD), NASAGSFC NASA Atoms are torn from the brownish bands of dust by shock waves (represented by orange rings). The shocks in the expanding blast wave then accelerate the atoms to near light speeds firing them into interstellar space like cosmic bullets.

Supermassive black holes Black holes in quasars throw out particles at near- light speeds and produce high-E photons

Pulsars Light cylinder Open magnetosphere r=c/  B Closed magnetosphere Neutron star mass = 1.4 solar masses radius = 10 km B = 10 to 10 Tesla 49

Pulsars – the movie

A bit of history First discovered during high altitude balloon flights by Victor Hess 1912 Pierre Auger discovered extensive air showers 1938 Enrico Fermi proposed cosmic ray shock accelerators 1949 GZK cutoff proposed1966 Highest energy cosmic ray ever (3x10 20 eV) observed by the Fly’s Eye 1991

Air showers 00    e-e- e+e+

Cerenkov radiation

Whipple Next generation is VERITAS = 7 Whipple array 10m  -ray telescope – Cerenkov radiation detector 248 mirrors Largest and most sensitive - so far

The cosmic ray leg Below the knee – Milky Way sources (supernovae, pulsars) Knee to ankle – Galaxies and quasars Ankle - ??

Fly’s Eye

EUSO ESA mission - planned for launch 2009 Observes fluoresence in Earth’s atmospher e

OWL Orbiting Wide-angle Light-collectors

Nightglow

Global warming by cosmic rays not many cosmic rays lots of cosmic rays

The End For more information, visit: 7/ htm ml