  In the internal shock model of gamma ray bursts ultrahigh energy muons,
pions, neutrons and kaons are likely to be produced in the interactions of
shock accelerated relativistic protons with low energy photons (KeV-MeV). These
particles subsequently decay to high energy neutrinos/antineutrinos and other
secondaries.
  In the high internal magnetic fields of gamma ray bursts, the ultrahigh
energy charged particles ($\mu^+$, $\pi^+$, $K^+$) lose energy significantly
due to synchrotron radiations before decaying into secondary high energy
neutrinos and antineutrinos. The relativistic neutrons decay to high energy
antineutrinos, protons and electrons. We have calculated the total neutrino
flux (neutrino and antineutrino) considering the decay channels of ultrahigh
energy muons, pions, neutrons and kaons. We have shown that the total neutrino
flux generated in neutron decay can be higher than that produced in $\mu^+$ and
$\pi^+$ decay. The charged kaons being heavier than pions, lose energy slowly
and their secondary total neutrino flux is more than that from muons and pions
at very high energy. Our detailed calculations on secondary particle production
in $p\gamma$ interactions give the total neutrino fluxes and their flavour
ratios expected on earth. Depending on the values of the parameters
(luminosity, Lorentz factor, variability time, spectral indices and break
energy in the photon spectrum) of a gamma ray burst the contributions to the
total neutrino flux from the decay of different particles (muon, pion, neutron
and kaon) may vary and they would also be reflected on the neutrino flavour
ratios.
