42,573 research outputs found
Monotone Volume Formulas for Geometric Flows
We consider a closed manifold M with a Riemannian metric g(t) evolving in
direction -2S(t) where S(t) is a symmetric two-tensor on (M,g(t)). We prove
that if S satisfies a certain tensor inequality, then one can construct a
forwards and a backwards reduced volume quantity, the former being
non-increasing, the latter being non-decreasing along the flow. In the case
where S=Ric is the Ricci curvature of M, the result corresponds to Perelman's
well-known reduced volume monotonicity for the Ricci flow. Some other examples
are given in the second section of this article, the main examples and
motivation for this work being List's extended Ricci flow system, the Ricci
flow coupled with harmonic map heat flow and the mean curvature flow in
Lorentzian manifolds with nonnegative sectional curvatures. With our approach,
we find new monotonicity formulas for these flows.Comment: v2: final version (as published
Top down, bottom up structured programming and program structuring
New design and programming techniques for shuttle software. Based on previous Apollo experience, recommendations are made to apply top-down structured programming techniques to shuttle software. New software verification techniques for large software systems are recommended. HAL, the higher order language selected for the shuttle flight code, is discussed and found to be adequate for implementing these techniques. Recommendations are made to apply the workable combination of top-down, bottom-up methods in the management of shuttle software. Program structuring is discussed relevant to both programming and management techniques
Spherical Redshift Distortions
Peculiar velocities induce apparent line of sight displacements of galaxies
in redshift space, distorting the pattern of clustering in the radial versus
transverse directions. On large scales, the amplitude of the distortion yields
a measure of the dimensionless linear growth rate , where is the cosmological density and the linear
bias factor. To make the maximum statistical use of the data in a wide angle
redshift survey, and for the greatest accuracy, the spherical character of the
distortion needs to be treated properly, rather than in the simpler plane
parallel approximation. In the linear regime, the redshift space correlation
function is described by a spherical distortion operator acting on the true
correlation function. It is pointed out here that there exists an operator,
which is essentially the logarithmic derivative with respect to pair
separation, which both commutes with the spherical distortion operator, and at
the same time defines a characteristic scale of separation. The correlation
function can be expanded in eigenfunctions of this operator, and these
eigenfunctions are eigenfunctions of the distortion operator. Ratios of the
observed amplitudes of the eigenfunctions yield measures of the linear growth
rate in a manner independent of the shape of the correlation function.
More generally, the logarithmic derivative with
respect to depth , along with the square and component of the
angular momentum operator, form a complete set of commuting operators for the
spherical distortion operator acting on the density. The eigenfunctions of this
complete set of operators are spherical waves about the observer, with radial
part lying in logarithmic real or Fourier space.Comment: 15 pages, with 1 embedded EPS figur
The interior structure of rotating black holes 1. Concise derivation
This paper presents a concise derivation of a new set of solutions for the
interior structure of accreting, rotating black holes. The solutions are
conformally stationary, axisymmetric, and conformally separable.
Hyper-relativistic counter-streaming between freely-falling collisionless
ingoing and outgoing streams leads to mass inflation at the inner horizon,
followed by collapse. The solutions fail at an exponentially tiny radius, where
the rotational motion of the streams becomes comparable to their radial motion.
The papers provide a fully nonlinear, dynamical solution for the interior
structure of a rotating black hole from just above the inner horizon inward,
down to a tiny scale.Comment: Version 1: 8 pages, 3 figures. Version 2: Extensively revised to
emphasize the derivation of the solution rather than the solution itself. 11
pages, 4 figures. Version 3: Minor changes to match published version.
Mathematica notebook available at
http://jila.colorado.edu/~ajsh/rotatinginflationary/rotatinginflationary.n
The power spectrum of galaxies in the 2dF 100k redshift survey
We compute the real-space power spectrum and the redshift-space distortions
of galaxies in the 2dF 100k galaxy redshift survey using pseudo-Karhunen-Loeve
eigenmodes and the stochastic bias formalism. Our results agree well with those
published by the 2dFGRS team, and have the added advantage of producing
easy-to-interpret uncorrelated minimum-variance measurements of the
galaxy-galaxy, galaxy-velocity and velocity-velocity power spectra in 27
k-bands, with narrow and well-behaved window functions in the range 0.01h/Mpc <
k < 0.8h/Mpc. We find no significant detection of baryonic wiggles, although
our results are consistent with a standard flat Omega_Lambda=0.7
``concordance'' model and previous tantalizing hints of baryonic oscillations.
We measure the galaxy-matter correlation coefficient r > 0.4 and the
redshift-distortion parameter beta=0.49+/-0.16 for r=1 (beta=0.47+/- 0.16
without finger-of-god compression). Since this is an apparent-magnitude limited
sample, luminosity-dependent bias may cause a slight red-tilt in the power
spectum. A battery of systematic error tests indicate that the survey is not
only impressive in size, but also unusually clean, free of systematic errors at
the level to which our tests are sensitive. Our measurements and window
functions are available at http://www.hep.upenn.edu/~max/2df.html together with
the survey mask, radial selection function and uniform subsample of the survey
that we have constructed.Comment: Replaced to match accepted MNRAS version, with new radial/angular
systematics plot and sigma8 typo corrected. High-res figures, power spectra,
windows and our uniform galaxy subsample with mask at
http://www.hep.upenn.edu/~max/2df.html or from [email protected]. 26
journal pages, 28 fig
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Nonlinear Torsional Wave Beams
An evolution equation with cubic nonlinearity is presented for a torsional wave beam in an isotropic elastic solid. Analytical solutions are presented for the fundamental and third harmonic in the far field of a uniform circular source. Numerical results are presented for harmonic beam patterns at an intermediate distance between the near and far fields, and for a torsional waveform with shocks.Applied Research Laboratorie
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How Does Wind Project Performance Change with Age in the United States?
Wind-plant performance declines with age, and the rate of decline varies between regions. The rate of performance decline is important when determining wind-plant financial viability and expected lifetime generation. We determine the rate of age-related performance decline in the United States wind fleet by evaluating generation records from 917 plants. We find the rate of performance decline to be 0.53%/year for older vintages of plants and 0.17%/year for newer vintages of plants on an energy basis for the first 10 years of operation, which is on the lower end of prior estimates in Europe. Unique to the United States, we find a significant drop in performance by 3.6% after 10 years, as plants lose eligibility for the production tax credit. Certain plant characteristics, such as the ratio of blade length to nameplate capacity, influence the rate of performance decline. These results indicate that the performance decline rate can be partially managed and influenced by policy
Quantum walk with a four-dimensional coin
We examine the physical implementation of a discrete time quantum walk with a four-dimensional coin. Our quantum walker is a photon moving repeatedly through a time delay loop, with time being our position space. The quantum coin is implemented using the internal states of the photon: the polarization and two of the orbital angular momentum states. We demonstrate how to implement this physically and what components would be needed. We then illustrate some of the results that could be obtained by performing the experiment
HST Images and Spectra of the Remnant of SN 1885 in M31
Near UV HST images of the remnant of SN 1885 (S And) in M31 show a 0"70 +-
0"05 diameter absorption disk silhouetted against M31's central bulge, at SN
1885's historically reported position. The disk's size corresponds to a linear
diameter of 2.5 +- 0.4 pc at a distance of 725 +- 70 kpc, implying an average
expansion velocity of 11000 +- 2000 km/s over 110 years. Low-dispersion FOS
spectra over 3200-4800 A; reveal that the absorption arises principally from Ca
II H & K (equivalent width ~215 A;) with weaker absorption features of Ca I
4227 A; and Fe I 3720 A;. The flux at Ca II line center indicates a foreground
starlight fraction of 0.21, which places SNR 1885 some 64 pc to the near side
of the midpoint of the M31 bulge, comparable to its projected 55 pc distance
from the nucleus. The absorption line profiles suggest an approximately
spherically symmetric, bell-shaped density distribution of supernova ejecta
freely expanding at up to 13100 +- 1500 km/s. We estimate Ca I, Ca II, and Fe I
masses of 2.9(+2.4,-0.6) x 10^-4 M_o, 0.005(+0.016,-0.002) M_o, and
0.013(+0.010,-0.005) M_o respectively. If the ionization state of iron is
similar to the observed ionization state of calcium, M_CaII/M_CaI = 16(+42,-5),
then the mass of Fe II is 0.21(+0.74,-0.08) M_o, consistent with that expected
for either normal or subluminous SN Ia.Comment: 8 pages, including 4 embedded EPS figures, emulateapj.sty style file.
Color image at http://casa.colorado.edu/~mcl/sand.shtml . Submitted to Ap
Gas Absorption in the KH 15D System: Further Evidence for Dust Settling in the Circumbinary Disk
Na I D lines in the spectrum of the young binary KH 15D have been analyzed in
detail. We find an excess absorption component that may be attributed to
foreground interstellar absorption, and to gas possibly associated with the
solids in the circumbinary disk. The derived column density is log N_NaI = 12.5
cm^-2, centered on a radial velocity that is consistent with the systemic
velocity. Subtracting the likely contribution of the ISM leaves log N_NaI ~
12.3 cm^-2. There is no detectable change in the gas column density across the
"knife edge" formed by the opaque grain disk, indicating that the gas and
solids have very different scale heights, with the solids being highly settled.
Our data support a picture of this circumbinary disk as being composed of a
very thin particulate grain layer composed of millimeter-sized or larger
objects that are settled within whatever remaining gas may be present. This
phase of disk evolution has been hypothesized to exist as a prelude to the
formation of planetesimals through gravitational fragmentation, and is expected
to be short-lived if much gas were still present in such a disk. Our analysis
also reveals the presence of excess Na I emission relative to the comparison
spectrum at the radial velocity of the currently visible star that plausibly
arises within the magnetosphere of this still-accreting young star.Comment: Accepted for publication in ApJ, 23 pages, 6 figure
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