查看“︁磁普兰特数”︁的源代码

'''磁普兰特数'''（'''Pr<sub>m</sub>'''）是在[[磁流体力学]]中的[[無量綱]]，大約是動量擴散率（[[黏度]]）及磁擴散率的比例<ref>{{cite journal | last1=Schekochihin | first1=Alexander A. | last2=Cowley | first2=Steven C. | last3=Maron | first3=Jason L. | last4=McWilliams | first4=James C. | title=Critical Magnetic Prandtl Number for Small-Scale Dynamo | journal=Physical Review Letters | volume=92 | issue=5 | date=2004-02-03 | issn=0031-9007 | doi=10.1103/physrevlett.92.054502 | page=054502| pmid=14995310 | arxiv=astro-ph/0308336 | bibcode=2004PhRvL..92e4502S | s2cid=119389465 }}</ref>，定義為：

:<math>\mathrm{Pr}_\mathrm{m} = \frac{\mathrm{Re_m}}{\mathrm{Re}} = \frac{\nu}{\eta} = \frac{\mbox{viscous diffusion rate}}{\mbox{magnetic diffusion rate}}</math>

其中
* Re<sub>m</sub>為[[磁雷諾數]]
* Re為[[雷諾數]]
* ''&nu;'' 為動量擴散率（[[動黏度]]）
* ''&eta;'' 為[[磁擴散率]]

在[[太陽]][[對流層 (恆星)|對流層]]中磁普兰特数約為10<sup>−2</sup><ref>{{cite journal |last1=Schumacher |first1=Jörg |last2=Sreenivasan |first2=Katepalli R. |title=Colloquium: Unusual dynamics of convection in the Sun |journal=Reviews of Modern Physics |date=7 October 2020 |volume=92 |issue=4 |pages=041001 |doi=10.1103/RevModPhys.92.041001 |bibcode=2020RvMP...92d1001S |s2cid=225111979 |url=https://journals.aps.org/rmp/abstract/10.1103/RevModPhys.92.041001 |access-date=17 April 2021 |archive-date=2024-09-27 |archive-url=https://web.archive.org/web/20240927093626/https://journals.aps.org/rmp/abstract/10.1103/RevModPhys.92.041001 |dead-url=no }}</ref>，在行星內部及實際室的液态金属发电机中，磁普兰特数約為10<sup>−5</sup>。

==相關條目==
*[[普兰特数]]

==參考資料==
{{reflist}}
*''[http://prola.aps.org/abstract/PRL/v92/i5/e054502 Critical Magnetic Prandtl Number for Small Scale Dynamo]'', Schekochihin, A.A., ''et al.'' 2004, Physical Review Letters, 92, 5

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{{流體動力學小作品}}
[[Category:流體力學中的無因次量]]
[[Category:流体动力学]]
[[Category:磁流体力学]]