4.3. Probes of new physics beyond the electroweak scale
It is intriguing - and at the same time suggestive - that the
observed flux of CRs beyond the GZK-energy is well matched by the
flux predicted for cosmogenic neutrinos
[511,
512].
Of course, this is not a simple coincidence: any proton flux beyond
EpCMBth is degraded in energy by
photoproducing
0
and
±, with
the latter in turn decaying to produce
cosmogenic neutrinos. The number of neutrinos produced in the GZK
chain reaction compensates for their lesser energy, with the
result that the cosmogenic flux matches well the observed CR flux
beyond 1020 eV. Recently, the prospect of an enhanced
neutrino cross section has been explored in the context of
theories with large compact dimensions.
(49)
In these theories, the extra
spatial dimensions are responsible for the extraordinary weakness
of the gravitational force, or, in other words, the extreme size
of the Planck mass
[514,
515].
For example, if spacetime is taken as a direct product of a
non-compact 4-dimensional manifold and a flat spatial n-torus
Tn (of common linear size
2
rc), one
obtains a definite representation of this picture in which the effective
4-dimensional Planck scale, MPl ~ 1019 GeV, is
related to the fundamental scale of gravity, MD,
according to M2Pl =
8
MD2+n
rcn. Within this
framework, virtual graviton exchange would disturb high energy
neutrino interactions, and in principle, could increase the
neutrino interaction cross section in the atmosphere by orders of
magnitude beyond the SM value; namely
~ [E
/
(1010 GeV] mb
[516,
517,
518].
However, it is important to stress that a cross section of ~ 100 mb
would be necessary to obtain consistency with observed
showers which start within the first 50 g / cm2 of the
atmosphere. This is because Kaluza-Klein modes couple to neutral
currents and the scattered neutrino carries away 90% of the
incident energy per interaction
[519].
Moreover, models which postulate strong neutrino interactions at
super-GZK energies also predict that moderately penetrating
showers should be produced at lower energies, where the
neutrino-nucleon cross section reaches a sub-hadronic size. Within
TeV scale gravity is likely to be sub-hadronic
near the energy at which the cosmogenic neutrino flux peaks, and
so moderately penetrating showers should be copiously produced
[520].
Certainly, the absence of
moderately penetrating showers in the CR data sample should be
understood as a serious objection to the hypothesis of neutrino
progenitors of the super-GZK events.
Large extra dimensions still may lead to significant increases in
the neutrino cross section. If this scenario is true, we might
hope to observe black hole (BH) production (somewhat more masive
than MD) in elementary particle collisions with
center-of-mass energies
TeV
[521,
522,
523].
In particular, BHs occurring very deep in the atmosphere (revealed as
intermediate states of ultrahigh energy neutrino interactions)
could trigger quasi-horizontal showers and be detected by cosmic ray
observatories
[524,
525,
526,
527,
528].
Additionally, neutrinos that traverse the atmosphere unscathed may
produce BHs through interactions in the ice or water and be
detected by neutrino telescopes
[529,
530].
Interestingly,
N
BH
MD(-4+2n) / (1+n).
Therefore, the non-observation of the almost
guaranteed flux of cosmogenic neutrinos can be translated into
bounds on the fundamental Planck scale. For n
5 extra spatial
dimensions compactified on Tn, recent null results from CR
detectors lead to MD > 1.0 - 1.4 TeV
[531,
532].
These bounds are among the most stringent and conservative to date. In
the near future, PAO will provide more sensitive probes of
TeV-scale gravity and extra dimensions
[533].
Certainly, the lack of observed deeply-penetrating showers can be
used to place more general, model-independent, bounds on
N
[492,
534,
535,
536].
Up to now we have only discussed how to set bounds on physics beyond the SM. An actual discovery of new physics in cosmic rays is a tall order because of large uncertainties associated with the depth of the first interaction in the atmosphere, and the experimental challenges of reconstructing cosmic air showers from partial information. However, a similar technique to that employed in discriminating between photon and hadron showers can be applied to search for signatures of extra-dimensions. Specifically, if an anomalously large quasi-horizontal deep shower rate is found, it may be ascribed to either an enhancement of the incoming neutrino flux, or an enhancement in the neutrino-nucleon cross section. However, these two possibilities may be distinguished by separately binning events which arrive at very small angles to the horizontal, the so-called "Earth-skimming" events [537, 538]. An enhanced flux will increase both quasi-horizontal and Earth-skimming event rates, whereas a large BH cross section suppresses the latter, because the hadronic decay products of BH evaporation do not escape the Earth's crust [539]. For a more detailed discussion of neutrino interactions in the Earth atmosphere within TeV scale gravity scenarios see e.g. [1].
49 A point worth
noting at this juncture: the neutrino-nucleon cross section can
also be significantly enhanced at center-of-mass energies
100 TeV (within
the SM) via electroweak instanton-induced processes
[513].
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