SHENIE : S imulation of H igh E nergy N eutrino I nteracting with the E arth

VHENTW, 4/25/206 M.A. Huang

SHENIE: Simulation of High Energy Neutrino

Interacting with the EarthM.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 ([email protected]),

mailto:[email protected]


What is SHENIE

SHENIE means

goddess in Mandarin!


UHE- fluxes

So many UHE- fluxes, how to detect them?

Traditional detector technologyNuTel & CRTNT

New techniquesRadioSound wave

Need MC simulation for

neutrino interacting with

the Earth!


Target: Mauna Loa, Hawaii Big Island, USA http://hep1.phys.ntu.edu.tw/nutel/P. Yeh, et al., Modern Physics Lett. A.19, 1117-1124, (2004).

Mauna Loa

View from Hualalai

See NuTel talk by Bob Y. Hsiung


Target: Mt. Wheeler, Nevada, USA. (prototype in construction)

Z. Cao, M.A. Huang, P. Sokolsky, Y. Hu, J. Phys. G, 31, 571-582, (2005)

Highlight of the year 2005 by J PG

See CRTNT talk by Zhen Cao


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

1

2

3

4

5

6

7

Dep

th (

km

)Halite (rock salt)• L(<1GHz) > 500 m w.e.• Depth to >10km• Diameter: 3-8 km• Veff ~ 100-200 km3 w.e.• No known background• >2 steradians possible

Antenna array

Figure comes from Peter Gorham, talk in SLAC SalSA workshop, 2005.


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 28

th 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)

2

E

dE

E

dx

P

dPEE

dx

dE


Current SHENIE structure

CC/NC

leptons

hadronse

New event

N

Y

Propagation thru. Earth

Tauola

Enter DSR E

e

h

N

Y

EnterDSR Y

shower Esh

N

Exit DSRYN

CC :

decay

dE/dx

dE/dx

EDirection,position

E


Coordinate system

Global : Isotropic distribution

of & path length L and tot

al depth

Local :User supplied

topological map• Altitude (East, North)

X: geometric EastY: geometric NorthZ: Vertical

(geodetic) outward

L

R

L=2Rsin


Earth ModelSpherical Earth, R =

6371.2 KmDensity/composition

profileMaterial around

detector can be selected from 4 materials.


DSR

DSR: Detector Sensitive RegionFor 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.

Salt dome

1 km

5 km

Std. rock


-N interaction

CC/NC total cross-section determine interaction probability.W–resonance can be

added by usersNon-Standard model

cross-section can be implemented as external data file

• G.L. Lin, M.A. Huang, C.H. Iong, work in progress


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)

XX Tau loss by

~ 0.16% at E > 2.51017 eV.


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 If decay inside Earth, E-lab is calculated and are re-pro

pagated 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 i

s number of secondary particles which generate shower.

Esh-CM

Mean energy~ 0.5


Consistence check Use several methods to calculate tau flux passing throug

h 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 MC method produce results si

milar to analytical method. Conditions used in MC:

105 GeV < E < 1010 GeV N=3107

~1.10 1020 cm-2 s-1 sr-1

N=2979 (at E > 105 GeV) Mean conversion efficiency 9.

9310-5

Total fluxes 2.710-17 (cm2 sr s)-1 ; Equivalent to 8.5 events/(km2 sr yr) Should multiply trigger effici

ency 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 For GZK neutrinos, Slightly move to lower en

ergy due to large energy loss.

MC simulation conditions: 105 GeV < E < 1012 GeV N=508294 ~1.521022 cm-2 s-1 sr-1

N=5969 (at E > 105 GeV) Mean conversion efficienc

y 1.1710-2

Total fluxes 3.910-19 (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

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 SLA

C SalSA workshop, Mar. 2005.


Results -1cos vs. shower energy: all 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.


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 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.

SHENIE : S imulation of H igh E nergy N eutrino I nteracting with the E arth

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