Emancipation Celebration Program 1954

The Emancipation Celebrations were held on Saturday, July 31, 1954, Sunday, August 1, 1954, Monday, August 2, 1954, and Tuesday, August 3, 1954.https://scholar.uwindsor.ca/windsoremancipationcelebrationprograms/1014/thumbnail.jp

Twenty Years of Experience With the University of Arkansas Planetarium

The Model A-1 Spitz planetarium was placed in operation at the University of Arkansas in 1954. It was moved to its present location in 1972 and has continued to have a much expanded use. More than 8,000 persons attended demonstrations between 1 August 1972 and 31 March 1974. Approximately one third of these were University students in classes and laboratories; the remaining two thirds were accounted for by school and other youth groups and the public demonstrations

Flamingo, Fall, 1954, Vol. 31, No. 1

Monthly magazine of creative and other writings from undergraduates and faculty of Rollins College, sponsored by the Rollins English Department.https://scholarship.rollins.edu/flamingo/1134/thumbnail.jp

A Comparison of the Variability of the Symbiotic X-ray Binaries GX 1+4, 4U 1954+31, and 4U 1700+24 from Swift/BAT and RXTE/ASM Observations

We present an analysis of the X-ray variability of three symbiotic X-ray binaries, GX 1+4, 4U 1700+24, and 4U 1954+31, using observations made with the Swift Burst Alert Telescope (BAT) and the Rossi X-ray Timing Explorer (RXTE) All-Sky Monitor (ASM). Observations of 4U 1954+31 with the Swift BAT show modulation at a period near 5 hours. Models to explain this modulation are discussed including the presence of an exceptionally slow X-ray pulsar in the system and accretion instabilities. We conclude that the most likely interpretation is that 4U 1954+31 contains one of the slowest known X-ray pulsars. Unlike 4U 1954+31, neither GX 1+4 nor 4U 1700+24 show any evidence for modulation on a timescale of hours. An analysis of the RXTE ASM light curves of GX 1+4, 4U 1700+24, and 4U 1954+31 does not show the presence of periodic modulation in any source, although there is considerable variability on long timescales for all three sources. There is no modulation in GX 1+4 on either the optical 1161 day orbital period or a previously reported 304 day X-ray period. For 4U 1700+24 we do not confirm the 404 day X-ray period previously proposed for this source from a shorter duration ASM light curve. We conclude that all three sources have substantial low-frequency noise in their power spectra that may give the appearance of periodic modulation if this noise is not properly accounted for, particularly if short duration light curves are examined.Comment: Accepted for publication in The Astrophysical Journa

Your Radio Station, ABC In Central Maine, WTVL

Station photographs and the program schedule for Radio Station WTVL in Waterville, Maine, for August 1 - 31, [1954?].https://digitalcommons.library.umaine.edu/wlbz_station_records/1195/thumbnail.jp

Balanced Farm and Home Planning Program Calhoun Progress Report

Condensed progress report for the Balanced Farm and Home Planning Program in Calhoun County (Miss.), from August 1, 1954 to July 31, 1955.https://scholarsjunction.msstate.edu/mss-stevens-papers/1040/thumbnail.jp

Bulletin No. 1, The Dallas Seismological Observatory, January 1-March 31, 1954

Since this station is comparatively new and the personnel relatively untrained, the following system was used in preparing these data. The USCGS H times and deltas, measured on a large, inaccurate globe, were used in conjunction with Gutenberg time-charts to identify each phase. The identifications were made by Edward L. Hazelwood and are as accurate as this method will permit

Slicing Sets and Measures, and the Dimension of Exceptional Parameters

We consider the problem of slicing a compact metric space \Omega with sets of the form \pi_{\lambda}^{-1}\{t\}, where the mappings \pi_{\lambda} \colon \Omega \to \R, \lambda \in \R, are \emph{generalized projections}, introduced by Yuval Peres and Wilhelm Schlag in 2000. The basic question is: assuming that \Omega has Hausdorff dimension strictly greater than one, what is the dimension of the 'typical' slice \pi_{\lambda}^{-1}{t}, as the parameters \lambda and t vary. In the special case of the mappings \pi_{\lambda} being orthogonal projections restricted to a compact set \Omega \subset \R^{2}, the problem dates back to a 1954 paper by Marstrand: he proved that for almost every \lambda there exist positively many $t \in \R$ such that \dim \pi_{\lambda}^{-1}{t} = \dim \Omega - 1. For generalized projections, the same result was obtained 50 years later by J\"arvenp\"a\"a, J\"arvenp\"a\"a and Niemel\"a. In this paper, we improve the previously existing estimates by replacing the phrase 'almost all \lambda' with a sharp bound for the dimension of the exceptional parameters.Comment: 31 pages, three figures; several typos corrected and large parts of the third section rewritten in v3; to appear in J. Geom. Ana

Um Bronze de arte. Escultura romana encontrada em Alvarelhos, Santo Tirso.

64 (1-2) Jan.-Jun. 1954, p. 31-39