Can One Unscramble an Omelet? China's Economic Reform in by Yuan-li Wu, Richard Y. C. Yin

By Yuan-li Wu, Richard Y. C. Yin

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Lx, where 37 T. 01 X * by assuming a steady flux of 10- 11 cm- 2 8- 1 flux at 1 TeV. B is in gauss. The Crab and Vela pulsars (with an assumed steady VHE emission for the latter) is quite consistent in this relation of X and VHE luminosity. However, for PSR 1706-44, the X-ray luminosity detected by the ROSAT satellite (Becker et al. L gauss. A softer X-ray spectrum within the uncertainty of the ROSAT data may allow TeV emission compatible with the X-ray luminosity of ROSAT (Harding, this workshop).

The energy spectrum would be useful to distinguish whether the SNR and/or pulsar contributes to the VHE gamma ray emission. 7 (Lewis et al. 1993) can be evidence that the VHE energy spectrum from the pulsar (or from pulsar nebula) differs from that expected from SNR. In addition, there must be an enhancement of gamma rays from molecular clouds. The energy spectrum from the clouds can be different from SNR. In fact, the case of p Ophiuchus shows a steeper spectrum at GeV energies (Hunter et al. 1993).

A shift from the pulsar position and/or extended emission may be the case, and the data need a careful analysis. Haines (1993) mentioned the preliminary CANGAROO result on the Vela pulsar. Analysis on data accumulated since then is in progress in the CANGAROO experiment. PSR1706-44: A flux of"" 8 x 10- 12 cm- 2 s-l was detected by the CANGAROO group (Kifune et al. 1995) at 1 TeV energy with a statistical significance at the level of 10 (J. It is unlikely that the total of this observed flux is pulsed.

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