Microturbulence is a form of turbulence that varies over small distance scales. (Large-scale turbulence is called macroturbulence.)


Microturbulence is one of several mechanisms that can cause broadening of the absorption lines in the stellar spectrum.[1] Stellar microturbulence varies with the effective temperature and the surface gravity.[2]

The microturbulent velocity is defined as the microscale non-thermal component of the gas velocity in the region of spectral line formation.[3] Convection is the mechanism believed to be responsible for the observed turbulent velocity field, both in low mass stars and massive stars. When examined by a spectroscope, the velocity of the convective gas along the line of sight produces Doppler shifts in the absorption bands. It is the distribution of these velocities along the line of sight that produces the microturbulence broadening of the absorption lines in low mass stars that have convective envelopes. In massive stars convection can be present only in small regions below the surface; these sub-surface convection zones can excite turbulence at the stellar surface through the emission of acoustic and gravity waves.[4] The strength of the microturbulence (symbolized by ξ, in units of km s−1) can be determined by comparing the broadening of strong lines versus weak lines.[5]

Magnetic nuclear fusion

Microturbulence plays a critical role in energy transport during magnetic nuclear fusion experiments, such as the Tokamak.[6]


  1. ^ De Jager, C. (1954). "High-energy Microturbulence in the Solar Photosphere". Nature. 173 (4406): 680–1. Bibcode:1954Natur.173..680D. doi:10.1038/173680b0. Retrieved 2007-05-21.
  2. ^ Montalban, J.; Nendwich, J.; Heiter, U.; Kupka, F.; et al. (1999). "The Effect of the microturbulence parameter on the Color-Magnitude Diagram". Reports on Progress in Physics. 61 (S239): 77–115. Bibcode:2007IAUS..239..166M. doi:10.1017/S1743921307000361.
  3. ^ Cantiello, M. et al. (2008). "On the origin of Microturbulence in hot stars" (PDF).
  4. ^ Cantiello, M. et al. (2009); Langer, N.; Brott, I.; De Koter, A.; Shore, S. N.; Vink, J. S.; Voegler, A.; Lennon, D. J.; Yoon, S.-C. (2009). "Sub-surface convection zones in hot massive stars and their observable consequences". Astronomy and Astrophysics. 499 (1): 279. arXiv:0903.2049. Bibcode:2009A&A...499..279C. doi:10.1051/0004-6361/200911643.
  5. ^ Briley, Michael (July 13, 2006). "Stellar Properties from Spectral Lines: Introduction". University of Wisconsin. Archived from the original on November 23, 2007. Retrieved 2007-05-21.
  6. ^ Nevins, W.M. (August 21, 2006). "The Plasma Microturbulence Project". Lawrence Livermore National Laboratory. Retrieved 2007-05-21.

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Bright giant

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CN star

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Frozen star (hypothetical star)

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HD 197027

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HD 59612

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Helium-weak star

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Lambda Boötis star

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Lead star

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Model photosphere

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As computers have evolved, the complexity of the models has deepened, becoming more realistic in including more physical data and excluding more of the simplifying assumptions. This evolution of the models has also made them applicable to different kinds of stars.

Photometric-standard star

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Q star

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Stellar atmosphere

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Stellar mass

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Star systems
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