Abstract
THE triple star system β Persei (Algol) is an erratic radio source1 which has occasional periods of activity lasting for several days. Jones and Woolf2 suggest that the emission results from mass transfer between Algol A and B, the components of the 2.8 d eclipsing binary. Hjellming3 has discussed the parameters of possible models for the emission region.
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References
Hjellming, R. M., Webster, E., and Balick, B., Astrophys. J. Lett., 178, L139 (1972).
Jones, T. W., and Woolf, N. J., Astrophys. J., 179, 859 (1973).
Hjellming, R. M., Nature, 238, 52 (1972).
Ryle, M., Nature, 239, 435 (1972).
Frieboes-Conde, H., Herczeg, T., and Høg, E., Astr. Astrophys., 4, 78 (1970).
Hill, G., Barnes, J. V., Hutchings, J. B., and Pearce, J. A., Astrophys. J., 168, 443 (1971).
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POOLEY, G., RYLE, M. 5 GHz Emission from ß Persei. Nature 244, 270–272 (1973). https://doi.org/10.1038/244270a0
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DOI: https://doi.org/10.1038/244270a0
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