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Neutrino oscillations in the neutrino beam from CERN to Gran Sasso
The question whether neutrinos have mass or not is of fundamental
importance, not only for the standard model of particle physics. Neutrinos come
in three different “flavours”: electronic νe , muonic νμ and tauonic ντ.
Besides photons, neutrinos are
the most abundant particles existing in the cosmos. They outnumber the ordinary
baryonic matter by a factor 1010. This factor suggests that
neutrinos, even if their rest mass is extremely small, may represent a
considerable share of the total mass of the universe. Hence, they are
candidates for a part of “dark matter”, which, though not found so far, is
thought to account for 90-95% of the total mass of the universe.
Our sun is a particularly intensive source of
neutrinos, and it has been known for quite a while that a respectable share of
the solar neutrinos mysteriously disappears on the way to our earth. The effect
can be explained by the phenomenon of neutrino oscillation, which means that
the flavour state (νe, νμ, ντ) of a neutrino varies with time along the
distance travelled. Oscillation can however only occur, if neutrinos have a
finite rest mass. The probability for a transition/oscillation from a state 1
into a state 2, W(1 → 2), is obtained from quantum
mechanics:
W(1 → 2) ∝ sin2(Δm2 L /E),
Δm being the mass difference of the two neutrinos, L the path length, and E the kinetic energy. The smaller Δm,
the larger the path length needed to obtain a
measurable effect. In the CERN/Gran Sasso (long baseline neutrino oscillation)
project, a muon neutrino beam νμ is
produced at CERN and directed towards the OPERA neutrino detector located 732
km afar in an underground laboratory in the Gran Sasso highway tunnel.
The OPERA
detector consists of about 13 million lead plates (approx. 2000 metric tons),
which are arranged in a sandwich structure with photo emulsion sheets in
between. The signature of a νμ to ντ oscillation event is the observation of the charged tauon particle from a neutrino-induced reaction in
the detector. The use of nuclear photo emulsion is dictated by the fact that
the tauon has only a short lifetime and thus generates a track as short as 100
µm. The challenge is to locate the proper emulsion sheet after a reaction occurred,
to develop the sheet and to analyze the tracks contained in the sheet by use of
automatic optical scanning microscopes.
Our group is at present building up a facility for the measurement of low radioactivity lead
samples as a quality control for OPERA.
First data taking is scheduled in 2006.
Links
OPERA homepage
CERN
OPERA (INFN)
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