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November 11, 1935 Explorer II , a 113,000 cubic foot helium

November 11, 1935 Explorer II , a 113,000 cubic foot helium balloon ascends to a record 22,066 m while collecting atmospheric and cosmic ray data. May 11, 1950

joan-blackburn
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November 11, 1935 Explorer II , a 113,000 cubic foot helium

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  1. November 11, 1935Explorer II, a 113,000 cubic foot helium balloon ascends to a record 22,066 m while collecting atmospheric and cosmic ray data. May 11, 1950 A Naval Research Viking research rocket fired from the U.S.S. Norton Sound near Jarvis Island in the Pacific collects cosmic ray and pressure and temperature data. 1952-57James A. Van Allen (The University of Iowa) reports the first high altitude survey of total cosmic-ray intensity and latitude variation of heavy nuclei in primary cosmic radiation, from his “Rockoon” (balloon-launched rocket).

  2. July 31, 1961 NASA funds high-altitude balloon measurements of the proton and alpha-particle spectrum of primary cosmic radiation conducted by the University of Chicago above Uranium City, Saskatchewan, Canada. July 1969 Apollo 11 astronauts trap cosmic ray particles on exposed aluminum foil, returned to earth for analysis of its elemental and isotopic composition. With no atmosphere or magnetic fieldof its own, the moon’s surface provides a constant bombardment of particles.

  3. December 1972 Apollo 17’s lunar surface cosmic ray experiment measured the flux of low energy particles in space (foil detectors brought back to Earth for analysis.. October 26, 1973 IMP-8 launched. Continues today measuring cosmic rays, Earth’s magnetic field, and the near-Earth solar wind from a near-circular, 12-day orbit (half the distance to the moon). October 1975 to the present GOES (Geostationary Orbiting Environmental Satellite) An early warning system which monitors the Sun's surface for flares. 1977 The Voyager 1 and 2 spacecraft are launched. Each will explore acceleration processes of charged particles to cosmic ray energies.

  4. July 1992 SAMPEX (Solar Anomalous and Magnetospheric Particle Explorer) into polar orbit. By sampling interplanetary and magnetospheric particles, contributes to our understanding of nucleosynthesis and the acceleration of charged particles. July 1992 IMAX (Isotope Matter-Antimatter eXperiment) balloon- borne superconducting magnetic spectrometer measured the galactic cosmic ray abundances of protons, anti-protons, hydrogen, and helium isotopes. August 25, 1997 Advanced Composition Explorer (ACE) was launched!

  5. Primary Cosmic Ray Flux (particles/m-2 sec) Solar System Composition (relative number of atoms) Atomic Number (Z) Element Hydrogen (H) 1 1.00 640 Helium (He) 2 6.8  10-294 Lithium, beryllium, boron 2.6  10-9 1.5 Carbon, Nitrogen, Oxygen 1.2  10-36 Iron (Fe) 26 3.4  10-50.24 All heavier atoms 1.9  10-60.13

  6. 50mm Cosmic ray strikes a nucleus within a layer of photographic emulsion

  7. Primary cosmic ray Mostly photons, electrons and muons at Earth’s surface

  8. A 1019 eV Extensive Air Shower 100 billion particles at sea level 89% photons 10% electrons ~1% muons 12 km 6 km 6 km

  9. The Cosmic Ray Energy Spectrum Cosmic Ray Flux (1 particle per m2-sec) (1 particle per m2-year) (1 particle per km2-year) Energy (eV)

  10. Refrigerator cold CO2 bubble (887 mph) 0.02 eV Room temperature nitrogen N2 (1160 mph) 0.03 eV Atoms in sun’s MILLION DEGREE surface 0.50 eV Energy given to each single electron when accelerated by AA battery 1.5 eV Electrons accelerated by your television picture tube (traveling ~1/3 speed of light) 30,000 eV Fermi National Lab’s high energy protons 1,000,000,000,000 eV

  11. Recall: 1 joule = 6.2 x 1018 eV Superball bounced over your house 4 x 1017 eV Pitched baseball4 x 1020 eV Slammed hockey puck 1 x 1021 eV The highest energy Cosmic Rays are SUBATOMIC particles carrying the energy of MACROSCOPIC objects! 4 x 1021 eV = 60 joules

  12. The Cosmic Ray Energy Spectrum FERMILAB’s protons Bounced Superball Pitched baseball Hockey Puck Energy (eV)

  13. Two possible sources of cosmic rays Colliding galaxies Active galactic nucleus

  14. GZK Cutoff 1966 - K. Greisen - G.T.Zatsepin & V.A.Kuz’min showed the recently discovered cosmic microwave background radiation (CMBR) effectively makes the universe opaque to sufficiently high energy cosmic particles.

  15. GZK Cutoff 1966 - K. Greisen - G.T.Zatsepin & V.A.Kuz’min   p For example: p*+0p ++n and similar resonances yield attenuation lengths mere 10s of Mega parsecs for cosmic ray protons with E>1019 eV. Center of (our) Virgo supercluster is approximately 20 Mpc away All E>1019 eV primaries must originate within 100 Mpc of the earth

  16. AGASA Energy [eV] ICRC2001 news AGASA: 717 HiRes:7 2 events above1020eV

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