In astronomy, the Kraft break refers to the abrupt decrease in stars' average rotation rates at surface temperatures below about 6200 kelvin. The so-called break bears the name of astronomer Robert Kraft,[1] though its existence was recognized prior to his publications on the topic.[2] The break is understood to separate stars with deep convective envelopes and efficient magnetic dynamos from those without. The dynamos are thought to maintain magnetic fields that transfer angular momentum to the stellar wind, thus slowing down the star's surface through magnetic braking. In hot stars the process is less efficient (because the convective envelopes are shallow) so the stars continue to rotate quickly.[3]
Referencesedit
^Kraft, R. P. (1967), "Studies of Stellar Rotation. V. The Dependence of Rotation on Age among Solar-Type Stars", Astrophysical Journal, 150: 551, Bibcode:1967ApJ...150..551K, doi:10.1086/149359
^Schatzman, E. (1962), "A theory of the role of magnetic activity during star formation", Annales d'Astrophysique, 25: 18, Bibcode:1962AnAp...25...18S
^Maeder, A. (2009), Physics, Formation and Evolution of Rotating Stars(PDF), Astronomy and Astrophysics Library, Bibcode:2009pfer.book.....M, doi:10.1007/978-3-540-76949-1, ISBN978-3-540-76948-4
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kraft, break, astronomy, refers, abrupt, decrease, stars, average, rotation, rates, surface, temperatures, below, about, 6200, kelvin, called, break, bears, name, astronomer, robert, kraft, though, existence, recognized, prior, publications, topic, break, unde. In astronomy the Kraft break refers to the abrupt decrease in stars average rotation rates at surface temperatures below about 6200 kelvin The so called break bears the name of astronomer Robert Kraft 1 though its existence was recognized prior to his publications on the topic 2 The break is understood to separate stars with deep convective envelopes and efficient magnetic dynamos from those without The dynamos are thought to maintain magnetic fields that transfer angular momentum to the stellar wind thus slowing down the star s surface through magnetic braking In hot stars the process is less efficient because the convective envelopes are shallow so the stars continue to rotate quickly 3 References edit Kraft R P 1967 Studies of Stellar Rotation V The Dependence of Rotation on Age among Solar Type Stars Astrophysical Journal 150 551 Bibcode 1967ApJ 150 551K doi 10 1086 149359 Schatzman E 1962 A theory of the role of magnetic activity during star formation Annales d Astrophysique 25 18 Bibcode 1962AnAp 25 18S Maeder A 2009 Physics Formation and Evolution of Rotating Stars PDF Astronomy and Astrophysics Library Bibcode 2009pfer book M doi 10 1007 978 3 540 76949 1 ISBN 978 3 540 76948 4 nbsp This article about stellar astronomy is a stub You can help Wikipedia by expanding it vte Retrieved from https en wikipedia org w index php title Kraft break amp oldid 1190871184, wikipedia, wiki, book, books, library,
