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 [when?] 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
- ^ 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
- ^ 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
{{citation}}: CS1 maint: unflagged free DOI (link)
 | This article about stellar astronomy is a stub. You can help Wikipedia by expanding it. |