Pith. sign in

REVIEW 4 cited by

Dissipation in Compressible MHD Turbulence

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv astro-ph/9809357 v1 pith:3F5PCMP4 submitted 1998-09-28 astro-ph

Dissipation in Compressible MHD Turbulence

James M. Stone (1) , Eve C. Ostriker (1) , Charles F. Gammie (2) ((1) University of Maryland , (2) Center for Astrophysics) This is my paper
classification astro-ph
keywords turbulencedissipationfieldscompressiblemagneticstrongtimeamplified
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

We report results of a three dimensional, high resolution (up to 512^3) numerical investigation of supersonic compressible magnetohydrodynamic turbulence. We consider both forced and decaying turbulence. The model parameters are appropriate to conditions found in Galactic molecular clouds. We find that the dissipation time of turbulence is of order the flow crossing time or smaller, even in the presence of strong magnetic fields. About half the dissipation occurs in shocks. Weak magnetic fields are amplified and tangled by the turbulence, while strong fields remain well ordered.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. ALMA observations of Magnetic Fields in the Massive Star-forming Region IRAS 18360-0537

    astro-ph.GA 2026-07 conditional novelty 6.0

    An ordered hourglass B-field in IRAS 18360-0537 lies perpendicular to the outflow/rotation axis and is reshaped by rotation, outflow cavity walls, and accretion rather than pure magnetic regulation.

  2. Jet--ISM Interactions in Gaseous Disks: Simulating Kinetic Feedback in the Radio Galaxy 3C 326 N

    astro-ph.GA 2026-07 conditional novelty 6.0

    Jet–ISM coupling in multi-scale cloudy disks produces asymmetric lobes and kinematics that match the JWST-observed bubble in 3C 326 N for a 10^45 erg s^{-1} jet.

  3. The evolution of the galaxy gas-phase mass-metallicity relation from $z=15$ to $z=0$ in the COLIBRE cosmological simulations

    astro-ph.GA 2026-06 unverdicted novelty 6.0

    COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.

  4. Numerical simulations of shock-driven, supersonic turbulence in colliding three-temperature laboratory plasmas

    physics.plasm-ph 2026-05 unverdicted novelty 5.0

    Three-dimensional three-temperature simulations of colliding supersonic plasma flows from irradiated CH mesh targets produce a persistent shocked turbulent mixing layer that evolves toward an isothermal state with ani...