Titlebook: Very High Energy Gamma Ray Astronomy; K. E. Turver Book 1987 D. Reidel Publishing Company, Dordrecht, Holland 1987 astronomy.astrophysics.

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Source Mechanisms (Pulsars)erent models of pulsar emission. These new models are able to explain the presence of high energy photons in a natural way, and provide predictions on pulse position, width and energy spectrum which may guide new observations.

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Statistical Analysis in High Energy Gamma Ray Astronomyhop on High Energy Gamma Ray Astronomy held at Durham in August 1986. Topics covered include testing for a D.C. excess, testing for periodic emission at a known period, choice of statistic, searching for an unknown period, Fourier analysis, source variability, and estimating the light curve.

一个姐姐

VHE Gamma Rays from Cygnus X-3erved during the radio flare of early Oct. at a phase of .. = 0.74. No evidence for pulsar periodicity was found during the burst. Searches for periodicity outside the burst have not yet produced positive results.

chandel

Search for a 12.59 ms. Pulsar in Cygnus X-3 at E > 400 GeVa 12.5908 ms. pulsar, as recently reported by Chadwick et al. (1). The results of our period search fail to substantiate the original observation. Reasons why the two results may not be incompatible are discussed.

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Simultaneous Measurements of VHE Gamma Rays from Hercules X-1he Whipple Observatory reported by Gorham (1986). In both observations evidence for emission of VHE gamma rays showing the same periodicity and significant at about the 3 sd level was obtained. This represents the first simultaneous detection of a VHE gamma ray source by two independent telescopes.

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TeV Observations of Her X-l at the Whipple Observatory: 1984–1985uggests that the gamma-ray source is not always coincident with the X-ray source; in particular, the strongest effect was observed after the pulsar entered eclipse. All effects were observed to occur during the active states of the 35 day X-ray cycle.

宇宙你

VHE Gamma Rays from the X-Ray Pulsar 4U0115+63r member of the binary system. The average peak flux above 0.2 TeV for these observations was (2.0 ± 0.4) x 10. cm. sec.. These observations are consistent with previous reports of the sporadic nature of this source.