Testing Relativity Theory With Neutrinos. Brett Altschul University of South Carolina May 15, 2008. Overview. Lorentz invariance is extremely well tested. Yet many candidate theories of quantum gravity “predict” Lorentz violation in certain regimes, especially at very high speeds.
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University of South Carolina
May 15, 2008
Lorentz invariance is extremely well tested.
Yet many candidate theories of quantum gravity “predict” Lorentz violation in certain regimes, especially at very high speeds.
Neutrino physics offers interesting ways to test whether relativity still holds very close to the speed of light.
In the last fifteen years, there has been growing interest in the possibility that Lorentz symmetry may not be exact.
There are two broad reasons for this interest:
Reason One:Many theories that have been put forward as candidates to explain quantum gravity involve LV in some regime.
(For example, string theory, non-commutative geometry, loop quantum gravity…)
Reason Two:Lorentz symmetry is a basic building block of both quantum field theory and the General Theory of Relativity, which together describe all observed phenomena.
Anything this fundamental should be tested. Much of the story of modern theoretical physics is how important symmetries do not hold exactly.
There is no excellent beauty that hath not somestrangeness in the proportion. — Francis Bacon
With those restrictions, the Lagrange density for a free fermion looks like:
A separate set of coefficients will exist for every elementary particle in the theory.
One important effect of these Lorentz-violating terms is to modify the velocity. For example, with c present:
From this expression, we can see when the effective field theory breaks down. The velocity may become superluminal when . If , this is .
More generally, momentum eigenstates may not be eigenstates of velocity.
Most Lorentz-violating effects at high relativistic energies depend on a particle’s maximum achievable velocity (MAV).
The corresponding energy-momentum relation is
Most of these couplings are easy to constrain with astrophysical polarimetry.
However, some will require more complicated measurements (e.g. with Doppler shifts or electromagnetostatics).
The coefficients need not be diagonal in flavor space either. Like neutrino masses, they may mix different species.
In fact, three-parameter Lorentz-violating models can explain all observed neutrino oscillations (including LSND).
However, many possible parameters have not been probed.
The “full” neutrino sector has 102 Lorentz-violating parameters.
It’s well known that SN1987A neutrinos traveled to Earth with a speed that differed from by a fraction .
However, this boundapplies only to electronneutrinos moving in onedirection.
We can get better bounds by looking at energetic constraints.We now feel con-fident that ultra-high-energy cosmicrays are primarilyprotons, with en-ergies up toGeV.
The protons have to live long enough to travel tens of Mpc to reach Earth.
Normally, that would be no problem, but relativity violations might cause fast-moving protons to decay, even if they’re stable at rest.
If the protons has speeds greater than 1, they would emit vacuum Cerenkov radiation.
The primary cosmic rays must also be immune to -decay, .
This is where the neutrinos come in.
This decay is disallowed only if vacuum Cerenkov radiation.
This is only a one-sided bound if the neutrino MAV is isotropic.
However, an anistropic MAV is bounded on both sides at the level.
The bounds are the same for the . Just swap the positron for a .
The constraints on the MAV for are worse by a factor of 3, since in a decay, themass makes a significant contribution.
Most other particles that a proton could decay into are also subject to similar or better bounds.
Lorentz violation is an interesting possibility to be part of the “Theory of Everything.”Lorentz tests for ultrarelativistic particles like neutrinos are parameterized by the MAV.The fact that primary cosmic ray protons don’t decay into neutrons sets stronger limits on the neutrino MAV than time-of-flight measurements.
Thanks to V. A. Kostelecký and E. Altschul. positron for a .
That’s all, folks!