SHENIE

SHENIE: Simulation of High Energy Neutrino Interacting with the Earth: 

SHENIE: Simulation of High Energy Neutrino Interacting with the Earth M.A. Huanga, Y.L. Hongb, C.H. Iongbc, G.L. Linb (a) General Education Center, National United University, 1, Lien-da, Kung-ching Li, Miao-Li, 36003, TAIWAN (b) Institute of Physics, National Chiao-Tung University, 1001 Ta Hsueh Rd., Hsin-chu, 300, TAIWAN (c) Current Address: Institute of Physics, Academia Sinica, Nankang, Taipei, 105, TAIWAN Presenter: M.A. Huang (mahuang@nuu.edu.tw),

What is SHENIE: 

What is SHENIE SHENIE means goddess in Mandarin!

UHE- fluxes: 

UHE- fluxes So many UHE- fluxes, how to detect them? Traditional detector technology NuTel & CRTNT New techniques Radio Sound wave Need MC simulation for neutrino interacting with the Earth!

Slide4: 

See NuTel talk by Bob Y. Hsiung

Slide5: 

Highlight of the year 2005 by J PG See CRTNT talk by Zhen Cao

Radio array in salt dome: 

Radio array in salt dome Radio signal from EAS Large Cherenkov angle! Underground salt dome. Higher density than water/ice Good transparency to radio signal Free of artificial noise Figure comes from Peter Gorham, talk in SLAC SalSA workshop, 2005.

Previous version of SHENIE: 

Previous version of SHENIE Monte-Carlo simulation for all processes except energy loss, which use deterministic method. where decay length = E. Publications based on this version: M.A. Huang, J.J. Tseng, and G.L. Lin (7/31- 8/7, 2003) Proc. of the 28th ICRC, Tsukuba, Japan, p.1427, (2003) M.A. Huang, Proc. of the 21th International Conference on Neutrino Physics and Astrophysics (ν-2004) at Paris, French, Nucl. Phys. B (Proc. Suppl.), 143, 546, (2005); astro-ph/0412642 P. Yeh, et al., Proc. of CosPA 2003, Modern Physics Lett. A.19, 1117-1124, (2004) Z. Cao, M.A. Huang, P. Sokolsky, Y. Hu, J. Phys. G, 31, 571-582, (2005)

Current SHENIE structure: 

Current SHENIE structure

Coordinate system: 

Coordinate system Global : Isotropic distribution of  &  path length L and total depth Local : User supplied topological map Altitude (East, North) X: geometric East Y: geometric North Z: Vertical (geodetic) outward

Earth Model: 

Earth Model Spherical Earth, R = 6371.2 Km Density/composition profile Material around detector can be selected from 4 materials.

DSR: 

DSR DSR: Detector Sensitive Region For SalSA simulation: Sphere of 5 km radius, under 1km of rock. For ES telescope: DSR set on top of Earth and local topological map must be supplied.

-N interaction: 

-N interaction CC/NC total cross-section determine interaction probability. W–resonance can be added by users Non-Standard model cross-section can be implemented as external data file G.L. Lin, M.A. Huang, C.H. Iong, work in progress

Materials: 

Materials 4 materials: std. rock, water (ice), salt, iron Input particles: e/e , / , / Energy loss of  and  in 4 materials Ionization (). Pair Production, Photo-Nuclear, Bressmstrlung Soft energy loss cut at 0.01 (can be changed) Tau loss by ~ 0.16% at E > 2.51017 eV.

 decay: 

 decay  decay simulated by Randomly choose one event from a data bank of pre-simulated events current version Link to TAUOLA in near future TAUOLA simulation Fully polarized  Tauola have 22 decay modes, while PDB have 37 modes TAUOLA gives 4 momentum in CM of all decay particles Define E’cm = P║ + M Boost to lab by  = E-lab / M Secondary particle energy in lab frame E’lab = E’cm

Shower energy: 

Shower energy If  decay inside Earth, E-lab is calculated and  are re-propagated thru the rest of journey. If  decay in atmosphere, shower energy Esh is sum over Elab of hadrons or electron / gamma. The mean energy per particles is calculated by Esh/M, where M is number of secondary particles which generate shower. Esh-CM Mean energy ~ 0.5

Consistence check: 

Consistence check Use several methods to calculate tau flux passing through 100km of standard rock for two different source spectrum (AGN and GZK). MC: Use SHENIE, this work M.A. Huang, et al., paper in preparation. Semi-MC: MC in all processes except dE/dX M.A. Huang, Proc. of ν-2004 at Paris, Nucl. Phys. B, 143, 546, (2005) Analytical calculation: Solve  and  transport eq. J.J. Tseng et al., Phys. Rev. D 68, 063003, (2003). Source spectrum: AGN: A. Neronov, et al., Phys. Rev. Lett., 89, 051101 (2002) GZK: R. Engel, D. Seckel and T. Stanev, Phys. Rev. D 64, 093010 (2001). Typical Earth skimming event, =90.5, cord length ~100 km.

AGN  fluxes: 

AGN  fluxes MC method produce results similar to analytical method. Conditions used in MC: 105 GeV < E < 1010 GeV N=3107 ~1.10 1020 cm-2 s-1 sr-1 N=2979 (at E > 105 GeV) Mean conversion efficiency 9.9310-5 Total fluxes 2.710-17 (cm2 sr s)-1 ; Equivalent to 8.5 events/(km2 sr yr) Should multiply trigger efficiency and acceptance to get event rate. Both energy-dependent  energy peak at around 5~63 PeV, shower energy will peak around 10 PeV.

GZK  fluxes: 

GZK  fluxes For GZK neutrinos, Slightly move to lower energy due to large energy loss. MC simulation conditions: 105 GeV < E < 1012 GeV N=508294 ~1.521022 cm-2 s-1 sr-1 N=5969 (at E > 105 GeV) Mean conversion efficiency 1.1710-2 Total fluxes 3.910-19 (cm2 sr s)-1 ; Equivalent to 0.12 events/(km2 sr yr) energy peak at around 0.04 PeV ~1.6 EeV, Shower energy will peak around 0.1 EeV.

Underground salt dome detector: 

Underground salt dome detector Strawman array: 12 x 12 strings, 12 nodes per string (8 shown), 225 m spacing. Total volume (2.475km)3 = 15.16 km3 = 32.83 km3 of w.e. Figure and specification come from Peter Gorham, talk in SLAC SalSA workshop, Mar. 2005.

Results -1: 

Results -1 cos vs. shower energy: all events

SalSA tau events: 

SalSA tau events Showers come from several processes: decay, energy loss, CC and reverse CC. For each event, the maximum energy of sub-showers were used to identify this event.

Slide22: 

FWHM of cos distribution: -0.05 < cos < 1, i.e. 0<  < 93 FWHM of Esh: 1016.5 eV < Esh < 1018 eV. (Eth=1015 eV)

Conclusion: 

Conclusion SHENIE simulation code is “almost” finish! Still need some cosmetic works on user friendly I/O. Especially, need to work on output to ntuple. No manual or any documentation yet! For Earth skimming events: AGN tau flux ~ 8.5 events/(km2 sr yr), need detector ~ 1 km2 sr Shower spectrum peak around 1016 eV. GZK tau flux ~ 0.12 events/(km2 sr yr), need detector ~ 100 km2 sr Shower spectrum peak around 1017 eV. For underground detector such as SalSA: Shower spectrum peak around 1017 eV. -0.1 < cos <1. In a radius of 5km salt dome, tau event rate could reach ~ 2.5 events/year Highly depend on detector simulation, which is highly simplified in this study.