Vaughan–Preston gap

In astronomy, the Vaughan–Preston gap refers to the absence of F-, G- and K-type stars with intermediate levels of magnetic activity. That is, Vaughan and Preston noted two groups of stars with either high or low levels of activity, separated by an apparent gap.[1] There remains no consensus on the cause of the gap.[2]

References
  1. Vaughan, A. H.; Preston, G. W. (1980), "A survey of chromospheric CA II H and K emission in field stars of the solar neighborhood", Publications of the Astronomical Society of the Pacific, 92: 385, Bibcode:1980PASP...92..385V, doi:10.1086/130683
  2. McQuillan, A.; Aigrain, S.; Mazeh, T. (2013), "Measuring the rotation period distribution of field M dwarfs with Kepler", Monthly Notices of the Royal Astronomical Society, 432 (2): 1203–1216, arXiv:1303.6787, Bibcode:2013MNRAS.432.1203M, doi:10.1093/mnras/stt536, S2CID 118468125


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