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Propagation of Supersymmetric Charged Slepton at High Energies. Shufang Su • U. of Arizona. M.H. Reno, I. Sarcevic and S. Su hep-ph/0503030. M sl =250 GeV M wino =250 GeV. . earth. . . ~. ~. . . . . earth. N. ~. l. ~. q. ~. ~. . . Motivation. -.

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propagation of supersymmetric charged slepton at high energies

Propagation of Supersymmetric Charged Slepton at High Energies

Shufang Su • U. of Arizona

M.H. Reno, I. Sarcevic and S. Su

hep-ph/0503030

motivation
Msl=250 GeV

Mwino=250 GeV

earth

~

~

earth

N

~

l

~

q

~

~

Motivation

-

Neutrino telescopes have great potential

to probe new physics beyond SM

Gravitino LSP

Stau NLSP

Albuquerque, Chacko

and Burdman (2003)

Larger production rate

smaller production rate

 = 2.197£ 10-6 sec

c=659 meter

Larger effective detector volumn

stau propagation

stau energy loss
stau energy loss

-

  • Discovery potential for neutrino telescope depends on the stau lifetime and range
  • Crucial to determine the energy loss of the high energy stau as it traverse the earth

stau propagation

stau energy loss1
energy

ionization energy loss

Constant: =2 £ 10-3 cm2/g

radiative energy loss

m,  , more later …

c = E / ()

stau energy loss

-

Average energy loss of a particle traversing distance X

WhenE ¿,

i.e. E ¿ 4 £ 105 GeV £ (msl/150 GeV)

Stau range determined by

ionization energy loss or lifetime c

stau propagation

radiative energy loss
radiative energy loss: 

-

  • photonuclear
  • bremsstrahlung
  • pair production

stau propagation

radiative energy loss1
muon

Stau: mass dependence

/ 1/m

radiative energy loss: 

-

Stau

/ 1/m2

stau propagation

stau range x e e 0
E ¿

m=250 GeV

m=150 GeV

E À

E0=106 GeV

stau range: X(E, E0)

-

m=250 GeV

lifetime

lifetime

m=250 GeV

m=150 GeV

m=150 GeV

E0=103 GeV

stau propagation

comparison
Xus / XABCComparison

-

  • InAlbuquerque, Chacko and Burdman (2003)
  • Rescale from:
  •  = 0.8 £ 10-6 cm2/g
  • stau=9.5 £ 10-9 (150 GeV/mstau) cm2/g
  • No energy dependence

?

Improve the potential of neutrino

telescopes for detecting metastable stau

stau propagation

conclusion
Conclusion

-

  • Stau radiative energy loss  is dominated by

photo-nuclear and pair production

    • Photonuclear and pair: / 1/m
    • Bremsstrahlung: / 1/m2
  • Low energy ( E ¿), stau range is determined by ionization energy loss or stau lifetime, X / E
  • High energy ( E À), stau range is determined by radiative energy loss, X / log (E)
  • Previous estimation (scale stau) underestimate stau range by about a factor of two

stau propagation

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