RevModPhys.84.1307

Of the inclusive neutrino and antineutrino cc cross

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Unformatted text preview: al data. As can be seen, the CC cross section is measured to a few percent in this region. A linear dependence of the cross section on neutrino energy is also exhibited at these energies, a confirmation of the quark parton model predictions. In addition to such inclusive measurements as a function of neutrino energy, experiments have reported differential cross sections, for example, most recently Tzanov et al. (2006). Also, over the years, exclusive processes such as oppositesign dimuon production have been measured (Dore, 2011). Such dimuon investigations have been performed in counter experiments like CCFR (Foudas et al., 1990; Rabinowitz et al., 1993; Bazarko et al., 1995), CDHS (Abramowicz et al., 1982), CHARM-II (Vilain et al., 1999), E616 (Lang et al., 1987), Harvard-Penn-Wisconsin-Fermilab (HPWF) (Aubert et al., 1974; Benvenuti et al., 1978), NOMAD (Astier et al., 2000), and NuTeV (Goncharov et al., 2001; Mason et al., 2007b), in bubble chambers like Big European Bubble Chamber (BEBC) (Gerbier, 1985), Fermi National Accelerator Laboratory (FNAL) (Ballagh et al., 1981; Baker et al., 1985) and Gargamelle (Haatuft et al., 1983) as well as in nuclear emulsion detectors such as E531 (Ushida et al., 1983) and CERN Hybrid Oscillation Research apparatUS (CHORUS) (Onengut et al., 2004; Kayis-Topaksu et al., 2005, 2008b, 2011; Onengut et al., 2005). This latter class of measurements is particularly important for constraining the strange and antistrange quark content of the nucleon and their momentum dependence. In the near future, high statistics measurements of neutrino and antineutrino DIS are expected from the MINERA Rev. Mod. Phys., Vol. 84, No. 3, July–September 2012 In reaching the ultra-high-energy scale, we find ourselves, remarkably, back to the beginning of our journey at extremely low energies. Neutrinos at this energy scale have yet to manifest themselves as confirmed observations, though our present technology is remarkably close to dispelling that fact. To date, the highest energy neutrino recorded is several hundred TeV (DeYoung, 2011). However, experimentalists and theorists have their aspirations set much higher, to energies above 1015 eV. On the theoretical side, this opens the door for what could be called ‘‘neutrino astrophysics.’’ A variety of astrophysical objects and mechanisms become accessible at these energies, providing information that is complementary to that already obtained from electromagnetic or hadronic observations. In response to the call, the experimental community has forged ahead with a number of observational programs and techniques geared toward the observation of ultra-highenergy neutrinos from astrophysical sources. The range of these techniques include detectors scanning for ultra-highenergy cosmic neutrino-induced events in large volumes of water [Baikal (Antipin et al., 2007; Aynutdinov et al., 2009), Antares (Aslanides et al., 1999)], ice [Antarctic Muon And Neutrino Detector Array (AMAND...
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This document was uploaded on 09/28/2013.

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