Abstract
Following the first announcement of the discovery of a new type of pulsating radio source1, details of three further objects of this type have been published2, one of these, CP 0950, having an appreciably shorter period than the others. In the original article1 Hewish et al. suggested that the radio emission from these sources might arise from the oscillations of a neutron star. More recently, alternative explanations in terms of a binary neutron star system3 and also a rapidly rotating white dwarf4 have been proposed. The present communication describes further observations to investigate these possibilities and also to examine the frequency structure of individual pulses; further differences between CP 0950 and the other sources have been found.
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References
Hewish, A., Bell, S. .T., Pilkington, J. D. H., Scott, P. F., and Collins, R. A., Nature, 217, 709 (1968), (Paper 1).
Pilkington J. P. H., Hewish, A., Bell, S. J., and Cole, T. W., Nature, 218, 126 (1968), (Paper 2).
Saslaw, W. C., Faulkner, J., and Strittmatter, P. A., Nature, 217, 1222 (1968), (Paper 42).
Ostriker, J., Nature, 217, 1227 (1968), (Paper 39).
Ryle, M., J. Inst. Elect. Eng., 6, 14 (1960).
Davies, J. G., Horton, P. W., Lyne, A. G., Rickett, B. J., and Smith, F. G., Nature, 217, 910 (1968), (Paper 6).
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Scott, P.F., Collins, R.A. (1968). Further Observations of Pulsating Radio Sources. In: Pulsating Stars. Springer, Boston, MA. https://doi.org/10.1007/978-1-4899-6387-1_8
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DOI: https://doi.org/10.1007/978-1-4899-6387-1_8
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