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Solar Shadow Simulation Study with Particle Energy Distribution Analysis

This study simulates solar shadows using Liouville’s theorem and isotropic C.R.s at Earth. Backwards-going C.R.s are generated, and new runs are conducted with parametrization of Milagro effective area. Sun and Moon positions are tracked every 100 seconds for 1 year, with energy spectra analysis and event generation on a grid. Various simulations are run with different magnetic fields and angular resolutions to compare results with MC data. Conclusions suggest the significant impact of Milagro resolution on shadow shape and sensitivity to B fields at smaller scales.

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Solar Shadow Simulation Study with Particle Energy Distribution Analysis

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  1. Simulating the Solar Shadow Allen I. Mincer NYU LANL 12/18/06

  2. Stoermer Rule, as Modified by Henrici, adapted by AIM

  3. Some More Calculation Details • Using Liouville’s theorem, isotropic C.R.s + B fields give isotropic C.R.s at Earth, unless absorbed, so • Generate backwards going C.R.s from Milagro to Sun or Moon. Shadow if Sun or Moon is hit.

  4. New Runs • Built in parametrization of MC of Milagro effective area and angular resolution from /data/links/G4MCData/Milagro/sets/20/proton/scattering_0.99_AbsL30m_ScatL50m/linkdirtrig/G4_proton_006769.trig.dat.gz • 1 year, take Sun/Moon position every 100 seconds. • For each position, select energy from E-2.7 spectrum starting at 0.1 TeV. • For each position generate 1.6K events centered on the vertices of a 40 x 40 grid ± 10 degrees around straight line to Sun/Moon : 0.1 degree steps in Θ, ΦcosΘ. • -> 5 x 108particles tracked per run. • Weight events by effective area. • Run varying fields: B Earth only, B Earth + Sun dipole parallel to Earth’s dipole, B Earth + Sun dipole perp. to Earth’s dipole. • Run with and without angular resolution

  5. MC/Data Compare θ distribution Thanks Brian!

  6. Shadowed Particle Energy Sun Shadowed Particle energy Moon Shadowed Particle energy

  7. Shadow with no B field/resolution

  8. No B No Res, No Res, NoB, All

  9. No B No Res, No Res, NoB, All

  10. Sum over 1.2 degree radius bins

  11. Sum over 1.2 degree radius bins

  12. Sum over 1.2 degree radius bins Sun Tot B Moon Tot B Sun Rot B

  13. Shadow Shape

  14. Conclusions: • Solar large scale shadow shape is overwhelmingly determined by Milagro resolution. • Small scale (~1 degree) shape may have more sensitivity to B field • Shadow depth is determined to first order by whether particles strike sun. ie., strength of field. Next effect in MC is scattering out of 10 degrees. • How sensitive to real differences? • Next Step – Look at data, then depending on how rich data statistics are: • Build in realistic fields to test. • Build in better Milagro resolution

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