We ﬁnd only three types of pulses S (t) are needed for the deﬁnition of the three time correlation function, these pulses are presented in Table 1 together with the corresponding C3 (τ1 , τ2 , τ3 ).
Photon Counting Statistics for Single Molecule Spectroscopy
The correlation coeﬃcients and ﬁts to the following relationships are detailed in Table 11.
The SCUBA Local Universe Galaxy Survey II. 450 micron data - evidence for cold dust in bright IRAS Galaxies
TABLE I: The position of the maximum of the funcion (37) and the value of stick-slip length Eq. (43) for different types of the surface correlation function.
Surface Roughness and Effective Stick-Slip Motion
In this limit for Gaussian and power-law correlators with the exponential power spectra (types 1 and 2 in the Table I), the contribution from large t to the integral (37) is exponentially small.
Surface Roughness and Effective Stick-Slip Motion
On the other hand, our calculations with correlations produce a much better value of the static dielectric constant as seen from Table 1.
Linear Response Calculations of Lattice Dynamics in Strongly Correlated Systems
Furthermore, as shown in Table 1, the magnetic ﬁeld at the light cylinder of this pulsar, the strength of which seems to be correlated with giant-pulse emission, is ﬁfth among known radio pulsars.
Searches for Giant Pulses from Extragalactic Pulsars
TABLE I: Results of ﬁts of the functional form (18) to the correlator Gqq (R) for dynamical triangulations with N = 500 000 triangles and with various restrictions.
The Harris-Luck criterion for random lattices
TABLE IX: Λc baryon mass and wave functions at the origin (see Eq. (39)) as a function of the number of gaussians included in the light–light correlation function.
Charmed and Bottom Baryons: a Variational Approach based on Heavy Quark Symmetry
In Table IX and for the Λc baryon with an AL1 inter-quark interaction, we present the dependence of the mass and the value of the wave function at the origin on the number of gaussians used to build up the correlation function.
Charmed and Bottom Baryons: a Variational Approach based on Heavy Quark Symmetry
Table 1 also presents the correlation length critical exponent ν and the magnetic susceptibility critical exponent γ calculated for at the FPs.
Critical properties of random anisotropy magnets
The uncorrelated limit may also be described by an average of the appropriate correlation operator, as indicated in Table I.
How Time Works in Quantum Systems: Overview of time ordering and time correlation in weakly perturbed atomic collisions and in strongly perturbed qubits
TABLE I: Comparison of correlation in space and time.
How Time Works in Quantum Systems: Overview of time ordering and time correlation in weakly perturbed atomic collisions and in strongly perturbed qubits
There are also notable differences between temporal and spacial correlation, as detailed in Table I.
How Time Works in Quantum Systems: Overview of time ordering and time correlation in weakly perturbed atomic collisions and in strongly perturbed qubits
The v sin i measurements for the 30 stars with reliable cross-correlation results are given in Table 3.
The Variability and Rotation of Pre-main Sequence Stars in IC 348: Does Intracluster Environment Influence Stellar Rotation?
In spite of these limitations we include here a few comments on the correlation coefﬁcients as presented in Table 2.
Statistical analysis of BATSE gamma-ray bursts: Self-similarity and the Amati-relation
***