Industrial preparation of granulated charge

Boldyrev, R. A.; Geroimenkova, L. G.; Zorin, Yu. A.; Mintsyuk, E. M.; Pritula, V. I.

doi:10.1007/bf00700848

Cited by 3 publications

(2 citation statements)

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“…This suggests that the initial mass function (IMF) could be explained from the basic properties of turbulent fragmentation, without tunable parameters. The fact that supersonic MHD turbulence leads to sustaining of shock turbulence, to shock fragmentation, and to establishing a certain universal density distribution has also been recently demonstrated by Boldyrev & Brandenburg (2001) in a one-dimensional solvable Burgers model.…”

Section: Introductionmentioning

confidence: 79%

Kolmogorov‐Burgers Model for Star‐forming Turbulence

Boldyrev

2002

ApJ

140

189

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The process of star formation in interstellar molecular clouds is believed to be controlled by driven supersonic magnetohydrodynamic turbulence. We suggest that in the inertial range such turbulence obeys the Kolmogorov law, while in the dissipative range it behaves as Burgers turbulence developing shock singularities. On the base of the She-Lévêque analytical model we then predict the velocity power spectrum in the inertial range to be E k ∼ k −1.74 . This result reproduces the observational Larson law, u 2 l ∼ l 0.74···0.76 , [Larson, MNRAS 194 (1981) 809] and agrees well with recent numerical findings by Padoan and Nordlund [astro-ph/0011465]. The application of the model to more general dissipative structures, with higher fractal dimensionality, leads to better agreement with recent observational results.

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Section: Introductionmentioning

confidence: 79%

Kolmogorov‐Burgers Model for Star‐forming Turbulence

Boldyrev

2002

ApJ

140

189

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“…Also, the relation of the density distribution to the statistics of the velocity field requires a better understanding. Such a relation may be derived analytically in a simplified one-dimensional case (Boldyrev 1998;Boldyrev & Brandenburg 2001), although in the three-dimensional case the question is still open. However, in the derivation of formula (7) we explicitly constructed the multifractal distribution of the energy dissipation ǫ, which can possibly be related to the multifractal distribution of the density, since the energy dissipates in shocks where the density is accumulated.…”

Section: Discussionmentioning

confidence: 99%

Scaling Relations of Supersonic Turbulence in Star‐forming Molecular Clouds

Boldyrev¹,

Nordlund²,

Padoan

2002

ApJ

121

120

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We present a direct numerical and analytical study of driven supersonic MHD turbulence that is believed to govern the dynamics of star-forming molecular clouds. We describe statistical properties of the turbulence by measuring the velocity difference structure functions up to the fifth order. In particular, the velocity power spectrum in the inertial range is found to be close to E k ∼ k −1.74 , and the velocity difference scales as |∆u| ∼ L 0.42 . The results agree well with the Kolmogorov-Burgers analytical model suggested for supersonic turbulence in [astro-ph/0108300]. We then generalize the model to more realistic, fractal structure of molecular clouds, and show that depending on the fractal dimension of a given molecular cloud, the theoretical value for the velocity spectrum spans the interval [−1.74 · · · − 1.89], while the corresponding window for the velocity difference scaling exponent is [0.42 · · · 0.78].

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