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4 results

  • 21 - Soil slope stabilization

  • Edited by John J. Clague, Simon Fraser University, British Columbia, Douglas Stead, Simon Fraser University, British Columbia
  • Book:
    Landslides
    Published online:
    05 May 2013
    Print publication:
    23 August 2012, pp 252-266

  • Summary

    Abstract

    This chapter contains a discussion of methods for stabilizing potentially unstable slopes and slowly moving landslides. The methods described include the use of earthworks; surface water and deeper drainage; walls, piles and shear keys; pre-tensioned ground anchors; and a variety of geotechnical processes.

    Some of the reasons for underperformance in stabilization works are described. Where possible, simple rules are given, and suggestions are made as to how to analyze the effectiveness of the stabilization measures.

  • Detection of Pulsed X-ray Emission from The Fastest Millisecond Pulsar PSR B1937+21 with ASCA

  • Motoki Takahashi, Shinpei Shibata, Ken’ichi Torii, Yoshitaka Saito, Nobuyuki Kawai, Masaharu Hirayama, Tadayasu Dotani, Shuichi Gunji, Hirohisa Sakurai
  • Journal:
    International Astronomical Union Colloquium / Volume 177 / 2000
    Published online by Cambridge University Press:
    12 April 2016, pp. 353-354
    Print publication:
    2000
    • Article
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  • We report the first detection of the pulsed X-ray emission from the fastest millisecond pulsar known PSR B1937+21 (P =1.558msec) with ASCA. The pulsar is detected as a point source above ∼ 1.7keV, with no nebulosity indicated. The source flux in the energy band 2–10keV is found to be f = 4.3 × 10−13erg s−1 cm−2, which corresponds to the luminosity of Lx = 4πD2f ≈ 6.6 × 1032(D/3.6kpc)2 erg s−1, where D is the distance, and correspond to ≈ 6 × 10−4 of the rotation power of the pulsar. The pulsation is found at the period predicted by the radio ephemerides with very narrow primary peaks, the width of which is about 1/16 phase ≈ 100μs near the time resolution limit (61μs) of the observation. The pulsed luminosity within the primary peak (1/16 phase interval) is found to be fp = 4.0 × 10−12erg s−1 cm−2. Although there may be a secondary peak, its statistical significance is too low to identify. Spectra of the whole source region and the primary peak are fitted by power law models to give photon indices of about unity for both.