Support data for NASA Convair 990 meteorological flight 3, 5 June - 21 June 1968

Support documentation for NASA Convair 990 meteorological flight number

Reminiscence of John Muir by Cole, H.E.

Wis. Hist Soc Mus. Baraboo Daily News Sept. 23, 1919. LITTLE JOURNEY TO THE BOYHOOD HOME OF JOHN MUIR. By H.E. Cole. Excerpts. Mr. Cole made journey with Attorney and Mrs. E.S. Baker of Portage. Mr. Baker was the first white child born in town of Port Winnebago and in early manhood operated a horse-power threshing machine. The last two seasons the Muirs lived on farm, he threshed their grain, and attended the sale when they left the farm, purchasing some of the tools used by John Muir. Mrs. Baker attended a rural school taught by Joanna Muir. It was School #3, the Spicer school, in the town of Winnebago. Ate lunch at Ennis Lake. Blue jays screaming in the trees. Woodpeckers, kingbirds all about us. Daniel Muir helped organize Presbyterian Church (where cemetery is). ?? Mr. Keams says Muir visited the farm about 1898. Told Mr. Kearns the orchard looked more familiar than any other spot. At the auction Merrill Smith cried the sale. After selling one of the old-fashioned hand corn anters, the autioneer shouted that there was another better than the first. To this Daniel Muir cried out with all his Scotch honesty, No, it isn\u27t. The father conducted religious services, but received meager compensation. One day the question of small pay was mentioned to one of the members of the church to which he replied, Oh, well, he likes to preach

Mathematical models for radiation transfer

A radiation transfer model was modified to include semitransparent and opaque layers as well as molecular constituents. An example of the use of the program and an analysis of the mathematical model are included

Wind tunnel wall interference in V/STOL and high lift testing: A selected, annotated bibliography

This bibliography, with abstracts, consists of 260 citations of interest to persons involved in correcting aerodynamic data, from high lift or V/STOL type configurations, for the interference arising from the wind tunnel test section walls. It provides references which may be useful in correcting high lift data from wind tunnel to free air conditions. References are included which deal with the simulation of ground effect, since it could be viewed as having interference from three tunnel walls. The references could be used to design tests from the standpoint of model size and ground effect simulation, or to determine the available testing envelope with consideration of the problem of flow breakdown. The arrangement of the citations is chronological by date of publication in the case of reports or books, and by date of presentation in the case of papers. Included are some documents of historical interest in the development of high lift testing techniques and wall interference correction methods. Subject, corporate source, and author indices, by citation numbers, have been provided to assist the users. The appendix includes citations of some books and documents which may not deal directly with high lift or V/STOL wall interference, but include additional information which may be helpful

The Orbital Structure of Dark Matter Halos with Gas

With the success of the Chandra and XMM missions and the maturation of gravitational lensing techniques, powerful constraints on the orbital structure of cluster dark matter halos are possible. I show that the X-ray emissivity and mass of a galaxy cluster uniquely specify the anisotropy and velocity dispersion profiles of its dark matter halo. I consider hydrostatic as well as cooling flow scenarios, and apply the formalism to the lensing cluster CL0024+16 and the cooling flow cluster Abell 2199. In both cases, the model predicts a parameter-free velocity dispersion profile that is consistent with independent optical redshift surveys of the clusters.Comment: 17 pages, 12 figures; to appear in the Astrophysical Journa

CC267 Dairy Producer Waste Guidelines

Campaign Circular 267: This circular is about dairy producer waste guidelines

CC267 Dairy Producer Waste Guidelines

Campaign Circular 267: This circular is about dairy producer waste guidelines

Spin-exchange Cross Sections For Hydrogen-atomalkali-metal-atom Collisions

The pseudopotential molecular-structure method has been used to calculate the X1 and a3 interaction potentials for the alkali-metal-atom hydrogen-atom systems. These potentials were then used in a quantum-mechanical calculation to determine the spin-exchange cross sections in the energy range from 2.5x10-4 eV to 2.5 eV. The cross sections follow the general form Q1/2=a-b lnv. However, abundant structure on the cross sections is present due to orbiting resonances induced by the deeply bound well of the X1 molecular state. The spin-exchange cross sections range from 17x10-16 to 25x10-16 cm2 at room temperature for H(F=1) transferring to H(F=0) in collision with unpolarized lithium and cesium, respectively. © 1985 The American Physical Society

Dependence of the Inner DM Profile on the Halo Mass

I compare the density profile of dark matter (DM) halos in cold dark matter (CDM) N-body simulations with 1 Mpc, 32 Mpc, 256 Mpc and 1024 Mpc box sizes. In dimensionless units the simulations differ only for the initial power spectrum of density perturbations. I compare the profiles when the most massive halos are composed of about 10^5 DM particles. The DM density profiles of the halos in the 1 Mpc box show systematically shallower cores with respect to the corresponding halos in the 32 Mpc simulation that have masses, M_{dm}, typical of the Milky Way and are fitted by a NFW profile. The DM density profiles of the halos in the 256 Mpc box are consistent with having steeper cores than the corresponding halos in the 32 Mpc simulation, but higher mass resolution simulations are needed to strengthen this result. Combined, these results indicate that the density profile of DM halos is not universal, presenting shallower cores in dwarf galaxies and steeper cores in clusters. Physically the result sustains the hypothesis that the mass function of the accreting satellites determines the inner slope of the DM profile. In comoving coordinates, r, the profile \rho_{dm} \propto 1/(X^\alpha(1+X)^{3-\alpha}), with X=c_\Delta r/r_\Delta, r_\Delta is the virial radius and \alpha =\alpha(M_{dm}), provides a good fit to all the DM halos from dwarf galaxies to clusters at any redshift with the same concentration parameter c_\Delta ~ 7. The slope, \gamma, of the outer parts of the halo appears to depend on the acceleration of the universe: when the scale parameter is a=(1+z)^{-1} < 1, the slope is \gamma ~ 3 as in the NFW profile, but \gamma ~ 4 at a > 1 when \Omega_\Lambda ~ 1 and the universe is inflating.[abridged]Comment: Accepted for publication in MNRAS. 13 pages, including 11 figures and 2 tables. The revised version has an additional discussion section and work on the velocity dispersion anisotrop