Observation of Muon Neutrino Disappearance with the MINOS Detectors in the NuMI Neutrino Beam

This Letter reports results from the MINOS experiment based on its initial exposure to neutrinos from the Fermilab NuMI beam. The rates and energy spectra of charged current ν_μ interactions are compared in two detectors located along the beam axis at distances of 1 and 735 km. With 1.27×10^(20) 120 GeV protons incident on the NuMI target, 215 events with energies below 30 GeV are observed at the Far Detector, compared to an expectation of 336±14 events. The data are consistent with ν_μ disappearance via oscillations with Δm_(32)^2|=2.74_(-0.26)^(+0.44)×10^(-3)  eV^2 and sin^2(2θ_(23))>0.87 (68% C.L.)

First observations of separated atmospheric ν_μ and ν̅ _μ events in the MINOS detector

The complete 5.4 kton MINOS far detector has been taking data since the beginning of August 2003 at a depth of 2070 meters water-equivalent in the Soudan mine, Minnesota. This paper presents the first MINOS observations of ν_μ and ν̅ _μ charged-current atmospheric neutrino interactions based on an exposure of 418 days. The ratio of upward- to downward-going events in the data is compared to the Monte Carlo expectation in the absence of neutrino oscillations, giving R^(data)_(up/down/R^(MC)_(up/down) = 0:62^(+0.19)_(0:14)(stat.) ± 0.02(sys.). An extended maximum likelihood analysis of the observed L/E distributions excludes the null hypothesis of no neutrino oscillations at the 98% confidence level. Using the curvature of the observed muons in the 1.3 T MINOS magnetic field ν_μ and ν̅ _μ interactions are separated. The ratio of ν̅ _μ to ν_μ events in the data is compared to the Monte Carlo expectation assuming neutrinos and antineutrinos oscillate in the same manner, giving R^(data)_(ν_μ/ν̅ _μ) / R^(MC)_(ν_μ/ν̅ _μ) = 0.96^(+0:38)_(0.27)(stat.) ± 0.15(sys.), where the errors are the statistical and systematic uncertainties. Although the statistics are limited, this is the first direct observation of atmospheric neutrino interactions separately for ν_μ and ν̅ _μ

P3_6 Cavorite Pt 2: the Gravity of the Situation

We continue to explore the gravitational and atmospheric effects of Cavorite, a fictional material that is “opaque to gravitation”, by attempting to form a simplified gravitational model of the situation. This gravitational model was found to define the range at which gravitational acceleration will return to near normal as between 0.02 and 12 m. Further research is required to truly model the gravitational acceleration due to Cavorite

P3_3 On the Atmospheric Effects of Cavorite

We estimate the gravitational and atmospheric effects of a fictional substance known as Cavorite, a material proposed by H.G. Wells that is “opaque to gravitation”. We conclude that for a Cavorite sheet of radius 1 m the impact on the gravitational acceleration is only meaningful at less than 12 m above the plate, and is insignificant at heights greater than this. Therefore, the atmosphere is unlikely to vent away as claimed

P3_4 Elysium: Where'd the Atmosphere Go?

This paper determines whether the Elysium space station, from the 2013 film Elysium[1], could maintain an atmosphere. We found that Elysium, with a radius of 20 km[2], would not hold onto its atmosphere unless high wind speeds (183 ms^-1, 324 ms^-1, and 443 ms^-1; for the atmospheric rotations tested) are to be endured by its inhabitants

P3_5 On the minimum mass for a Death Star's power system

We examine the minimum mass necessary to build the power system for a "Death Star", as shown in the "Star Wars" series of films, using current technology. Considering its powerplant as a Carnot engine we are able to find a balance between the necessary mass of reactor and heat radiators so as to reduce the overall mass of the Death Star's power system to 6.8 x 10^25 kg, approximately 930 times the mass of Earth's moon (to 2 significant figures)

P3_9 Scooby and Shaggy: Metabolic Miracles

In the cartoon `What's New Scooby-Doo?' the characters Shaggy and Scooby are seen to eat large volumesof food without gaining any weight. Their effective temperatures in order to radiate away the excess energywere calculated to be T_Sh ~ 97 ± 033 °C for Shaggy, and T_Sc ~ 140 ± 43 °C for Scooby. It was concludedthat under normal circumstances, the subjects would perish of extreme hyperthermia. It was also notedthat Shaggy could survive if he was able to sweat continuously at the maximum rate for a human

P3_1 On the feasibility of neutrino sails

In this paper we consider whether a neutrino sail, a sheet of material absorbing neutrinos and gaining thrust from their momentum change, is a viable method of spacecraft propulsion. We calculate the thrust that could be achieved per unit area and compare this to that possible using a photon solar sail. We also calculate the thickness of sail necessary assuming that there are no special conditions under which the cross section for neutrino interactions with nuclei can be increased. We find that a thickness of 34000 light years would be necessary if a sheet of osmium were used, whereas neutron star matter could achieve this at 189 km thickness. We conclude that a neutrino sail is not a practical method of propulsion