5,490 research outputs found
The economics of garbage collection
This paper argues that economic theory can improve our understanding of memory management. We introduce the allocation curve, as an analogue of the demand curve from microeconomics. An allocation curve for a program characterises how the amount of garbage collection activity required during its execution varies in relation to the heap size associated with that program. The standard treatment of microeconomic demand curves (shifts and elasticity) can be applied directly and intuitively to our new allocation curves. As an application of this new theory, we show how allocation elasticity can be used to control the heap growth rate for variable sized heaps in Jikes RVM
The Neutrino mass matrix after Kamland and SNO salt enhanced results
An updated analysis of all available neutrino oscillation evidence in Solar
experiments including the latest SNO ES,CC and NC data (254d live time, NaCL
enhanced efficiency) is presented. We obtain, for the fraction of active
oscillating neutrinos:
sin^2alpha=(\Phi_{NC}-\Phi_{CC})/(\Phi_{SSM}-\Phi_{CC})=0.94^{+0.0.065}_{-0.060}
nearly 20\sigma from the pure sterile oscillation case. The fraction of
oscillating sterile neutrinos cos^2\alpha \lsim 0.12 (1 sigma CL). At face
value, these results might slightly favour the existence of a small sterile
oscillating sector. In the framework of two active neutrino oscillations we
determine individual neutrino mixing parameters and their errors we obtain
Delta m^2= 7.01\pm 0.08 \times 10^{-5} eV^2, tan^2 theta=0.42^{+0.12}_{-0.07}.
The main difference with previous analysis is a better resolution in parameter
space. In particular the secondary region at larger mass differences (LMAII) is
now excluded at 95% CL. The combined analysis of solar and Kamland data
concludes that maximal mixing is not favoured at 4-5 sigma. This is not
supported by the antineutrino reactor results alone. We estimate the individual
elements of the two neutrino mass matrix, writing M^2=m^2 I+M_0^2, we obtain (1
sigma errors):
M_0^2=10^{-5} eV^2\pmatrix{
2.06^{+0.29}_{-0.31} & 3.15^{+0.29}_{-0.35} \cr
3.15^{+0.29}_{-0.35} & 4.60^{+0.56}_{-0.44} }
Hamevol1.0: a C++ code for differential equations based on Runge-Kutta algorithm. An application to matter enhanced neutrino oscillation
We present a C++ implementation of a fifth order semi-implicit Runge-Kutta
algorithm for solving Ordinary Differential Equations. This algorithm can be
used for studying many different problems and in particular it can be applied
for computing the evolution of any system whose Hamiltonian is known. We
consider in particular the problem of calculating the neutrino oscillation
probabilities in presence of matter interactions. The time performance and the
accuracy of this implementation is competitive with respect to the other
analytical and numerical techniques used in literature. The algorithm design
and the salient features of the code are presented and discussed and some
explicit examples of code application are given.Comment: 18 pages, Late
Finite volume study of electric polarizabilities from lattice QCD
Knowledge of the electric polarizability is crucial to understanding the
interactions of hadrons with electromagnetic fields. The neutron polarizability
is very sensitive to the quark mass and is expected to diverge in the chiral
limit. Here we present results for the electric polarizability of the neutron,
neutral pion, and neutral kaon on eight ensembles with nHYP-smeared clover
dynamical fermions with two different pion masses (227 and 306 MeV). These are
currently the lightest pion masses used in polarizability studies. For each
pion mass we compute the polarizability at four different volumes and perform
an infinite volume extrapolation for the three hadrons. Along with the infinite
volume extrapolation we conduct a chiral extrapolation for the kaon
polarizability to the physical point. We compare our results for the neutron
polarizability to predictions from chiral perturbation theory.Comment: 7 pages, 11 figure
Solar neutrino experiments and Borexino perspectives
We present an updated analysis of all the data available about solar
neutrinos, including the charged current SNO results. The best fit of the data
is obtained in the Large Mixing Angle region, but different solutions are still
possible. We also study the perspectives of Borexino and conclude that this
experiment, with a parallel analysis of total rate and day-night asymmmetry,
should be able to discriminate between the different possible solutions.Comment: 3 pages, Latex, talk given by V. Antonelli at TAUP 2001 Conferenc
KamLAND Bounds on Solar Antineutrinos and neutrino transition magnetic moments
We investigate the possibility of detecting solar electron antineutrinos with
the KamLAND experiment. These electron antineutrinos are predicted by
spin-flavor oscillations at a significant rate even if this mechanism is not
the leading solution to the SNP. KamLAND is sensitive to antineutrinos
originated from solar B neutrinos. From KamLAND negative results after
145 days of data taking, we obtain model independent limits on the total flux
of solar electron antineutrinos $\Phi({}^8 B)< 1.1-3.5\times 10^4 cm^{-2}\
s^{-1}P<0.15%\mu B< 2.3\times 10^{-21}(\Delta m^2, \tan^2\theta)\mu\lsim 3.9\times 10^{-12} \mu_BB= 50\mu\lsim 9.0\times 10^{-13} \mu_BB= 200\mu\lsim 2.0\times 10^{-13} \mu_BB= 1000$ kG at the same
statistical significance.Comment: 13 pages, 2 figure
Solving the solar neutrino problem with kamLAND and BOREXINO
We analyze the expected signals of two future neutrino experiments, kamLAND
and BOREXINO. We show that with just these experiments, we will hopefully be
able to determine which of the existing solutions to the solar neutrino problem
is the real solution. We also analyze existing solar neutrino data and
determine the best-fit points in the oscillation-parameter space finding that
with the inclusion of SNO-charged current, the global-rates analysis gives a
favored LMA solution with a goodness of fit (g.o.f) of just 32.63%, whereas the
g.o.f of the SMA solution is 9.83%. Nonetheless, maximal and quasi-maximal
mixing is not favored. If we include the Superkamiokande spectrum in our \chi^2
analysis, we obtain a LMA solution with a g.o.f. of 84.38%.Comment: 4 pages, 5 figures, Talk given at 37th Rencontres de Moriond on
Electroweak Interactions and Unified Theories, Les Arcs, France, 9-16 Mar
200
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