| 词条 | Vaughan–Preston gap |
| 释义 |
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|date=November 2018}} 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] References1. ^{{Citation | last1 = Vaughan | first1 = A. H. | last2 = Preston | first2 = G. W. | title = A survey of chromospheric CA II H and K emission in field stars of the solar neighborhood | year = 1980 | journal = Publications of the Astronomical Society of the Pacific| volume = 92 | pages = 385| bibcode = 1980PASP...92..385V|doi = 10.1086/130683 }} {{DEFAULTSORT:Vaughan-Preston gap}}{{astronomy-stub}}2. ^{{Citation | last1 = McQuillan | first1 = A. | last2 = Aigrain | first2 = S. | last3 = Mazeh | first3 = T. | title = Measuring the rotation period distribution of field M dwarfs with Kepler | year = 2013 | journal = Monthly Notices of the Royal Astronomical Society| volume = 432 | issue = 2 | pages = 1203–1216| arxiv = 1303.6787 | bibcode = 2013MNRAS.432.1203M|doi = 10.1093/mnras/stt536 }} 3 : Stellar astronomy|Magnetism|Stellar physics |
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