Gamma Radiation from PSR B1055−52
The Astrophysical Journal1999Vol. 516(1), pp. 297–306
Citations Over TimeTop 10% of 1999 papers
D. J. Thompson, M. Bailes, D. L. Bertsch, J. M. Cordes, N. D’Amico, J. A. Esposito, J. P. Finley, R. C. Hartman, W. Hermsen, G. Kanbach, V. M. Kaspi, D. A. Kniffen, L. Kuiper, Y. C. Lin, A. G. Lyne, R. N. Manchester, S. M. Matz, H. A. Mayer‐Hasselwander, P. F. Michelson, P. L. Nolan, H. Öğelman, M. Pohl, P. V. Ramanamurthy, P. Sreekumar, O. Reimer, J. H. Taylor, M. P. Ulmer
Abstract
The telescopes on the Compton Gamma Ray Observatory (CGRO) have observed PSR B1055-52 a number of times between 1991 and 1998. From these data a more detailed picture of the gamma radiation from this source has been developed, showing several characteristics that distinguish this pulsar: the light curve is complex; there is no detectable unpulsed emission; the energy spectrum is hat, with no evidence of a sharp high-energy cutoff up to greater than 4 GeV. Comparisons of the gamma-ray data with observations at longer wavelengths show that no two of the known gamma-ray pulsars have quite the same characteristics; this diversity males interpretation in terms of theoretical models difficult.
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