In astronomy, the VaughanâPreston 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): 1203â1216, arXiv: 1303.6787, Bibcode: 2013MNRAS.432.1203M, doi: 10.1093/mnras/stt536, S2CID 118468125
 | This article about stellar astronomy is a stub. You can help Wikipedia by expanding it. |
In astronomy, the VaughanâPreston 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): 1203â1216, arXiv: 1303.6787, Bibcode: 2013MNRAS.432.1203M, doi: 10.1093/mnras/stt536, S2CID 118468125
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| This article about stellar astronomy is a stub. You can help Wikipedia by expanding it. |