1. Anisotropy of Primary Cosmic Rays
Newt Ganugapati for IJC

2. Anisotropy of Cosmic Ray Induced Muons
Anisotropy due to uneven distribution of cosmic ray Sources and process of CR propagation in the Milky way
Modulations due to the heliosphere, solar wind ,magnetic fields
Galactic effects (density gradients of CR density)
Compton getting effect (relative motion of solar system with local CR plasma, Earths orbital motion around the sun)
Two cones of excess and deficit because of magnetic mirroring effects due to the boundary between inner and outer galaxy
Deflected by GMF and are randomized by millions of years of travel

3. Tibet-III Air Shower Array
Scintillation Counters live days of HD array and live days of III array. Four fold coincidence recording more than 0.8 particles in charge. Air shower core positions is located in the array and zenith angle of arrival direction<40 degrees. Has a modal energy if 3TeV and a 0.9 degree angular resolution from Monte Carlo. 37 billion CR events were used
Lacking the absolute detector efficiency calibration in the declination direction absolute CR intensities along Dec cannot be compared. Average intensity in each Dec belt normalized to unity. Modulation is cosmic ray intensity studied for different Dec.

4. Celestial CR intensity map
I and II denote tail-in and loss-cone component while III denotes Cygnus region. HEGRA discovered a TeV gamma ray source there. We cannot tell the attribute hence interpretation that gamma ray emission is responsible for excesses cannot be ruled out. The years denote Solar Maxima and Minima (Magnetic activity)
New excess component with a 0.1% increase in this region at a significance level of 13.3SD with a 5o pixel radius

5. Local Solar Time CR Intensity Map
High multiplicity events with
coincident detector numbers
greater than 8 were adopted.
The observed dipole
anisotropy agrees very well
with the expected CG effect
Of Earth’s orbital motion
Around the sun. Heliospheric
Magnetic field and solar activity
don’t influence the multi-TeV
CR anisotropy

6. Celestial CR intensity for different CR energies
CR Energies of 4,6.2,12,50,300 TeV
respectively. Little dependency on
Energy below 12 TeV and fades away after that. Tail in component
visible after 50TeV
Multi-TeV GCR’s whose with large
gyroradii are not affected by
heliospheric magnetic field it is clear
GMF must be responsible for both
tail-in and loss cone modulations

7. Can we do better?

8. Track Type Plots
Measured RA( direct walk) for a declination band of 55o-65o

9. Direct-Walk sky-maps
Significance in equatorial coordinates,10o*10o bins smoothed

10. Summary and Conclusions
Initial studies indicate that AMANDA is sensitive to anisotropies of the primary cosmic rays
The effects observed by Super-K should be clearly observable. AMANDA could be able to measure this with a largely improved significance due to 80X larger statistics and smaller systematic uncertainties
An proper analysis would require reconstruction of all down-going events (JAMS or LLH), unfolding of seasonal effects, flare checking and improved data selection