Supernova-regulated ISM. V. Space and Time Correlations

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dc.contributor Aalto-yliopisto fi
dc.contributor Aalto University en
dc.contributor.author Hollins, J. F.
dc.contributor.author Sarson, G. R.
dc.contributor.author Shukurov, A.
dc.contributor.author Fletcher, A.
dc.contributor.author Gent, F. A.
dc.date.accessioned 2018-02-09T09:53:37Z
dc.date.available 2018-02-09T09:53:37Z
dc.date.issued 2017-11-20
dc.identifier.citation Hollins , J F , Sarson , G R , Shukurov , A , Fletcher , A & Gent , F A 2017 , ' Supernova-regulated ISM. V. Space and Time Correlations ' Astrophysical Journal , vol 850 , no. 1 , pp. 1-18 . DOI: 10.3847/1538-4357/aa93e7 en
dc.identifier.issn 0004-637X
dc.identifier.issn 1538-4357
dc.identifier.other PURE UUID: 1409cfe1-2265-4eae-bdd0-c433447231d2
dc.identifier.other PURE ITEMURL: https://research.aalto.fi/en/publications/supernovaregulated-ism-v-space-and-time-correlations(1409cfe1-2265-4eae-bdd0-c433447231d2).html
dc.identifier.other PURE LINK: http://www.scopus.com/inward/record.url?scp=85037697496&partnerID=8YFLogxK
dc.identifier.other PURE FILEURL: https://research.aalto.fi/files/16610561/Hollins_2017_ApJ_850_4.pdf
dc.identifier.uri https://aaltodoc.aalto.fi/handle/123456789/29741
dc.description.abstract We apply correlation analysis to random fields in numerical simulations of the supernova-driven interstellar medium (ISM) with the magnetic field produced by dynamo action. We solve the magnetohydrodynamic (MHD) equations in a shearing Cartesian box representing a local region of the ISM, subject to thermal and kinetic energy injection by supernova explosions, and parameterized, optically thin radiative cooling. We consider the cold, warm, and hot phases of the ISM separately; the analysis mostly considers the warm gas, which occupies the bulk of the domain. Various physical variables have different correlation lengths in the warm phase: 40, 50, and 60 pc for the random magnetic field, density, and velocity, respectively, in the midplane. The correlation time of the random velocity is comparable to the eddy turnover time, about 107 year, although it may be shorter in regions with a higher star formation rate. The random magnetic field is anisotropic, with the standard deviations of its components bx by bz having approximate ratios 0.5 0.6 0.6 in the midplane. The anisotropy is attributed to the global velocity shear from galactic differential rotation and locally inhomogeneous outflow to the galactic halo. The correlation length of Faraday depth along the z axis, 120 pc, is greater than for electron density, 60-90 pc, and the vertical magnetic field, 60 pc. Such comparisons may be sensitive to the orientation of the line of sight. Uncertainties of the structure functions of synchrotron intensity rapidly increase with the scale. This feature is hidden in a power spectrum analysis, which can undermine the usefulness of power spectra for detailed studies of interstellar turbulence. en
dc.format.extent 1-18
dc.format.mimetype application/pdf
dc.language.iso en en
dc.relation.ispartofseries Astrophysical Journal en
dc.relation.ispartofseries Volume 850, issue 1 en
dc.rights openAccess en
dc.subject.other Astronomy and Astrophysics en
dc.subject.other Space and Planetary Science en
dc.subject.other 113 Computer and information sciences en
dc.subject.other 115 Astronomy and space science en
dc.title Supernova-regulated ISM. V. Space and Time Correlations en
dc.type A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä fi
dc.description.version Peer reviewed en
dc.contributor.department Newcastle University
dc.contributor.department Centre of Excellence Research on Solar Long-Term Variability and Effects, ReSoLVE
dc.contributor.department Department of Computer Science en
dc.subject.keyword galaxies: ISM
dc.subject.keyword ISM: kinematics and dynamics
dc.subject.keyword ISM: magnetic fields
dc.subject.keyword Turbulence
dc.subject.keyword Astronomy and Astrophysics
dc.subject.keyword Space and Planetary Science
dc.subject.keyword 113 Computer and information sciences
dc.subject.keyword 115 Astronomy and space science
dc.identifier.urn URN:NBN:fi:aalto-201802091237
dc.identifier.doi 10.3847/1538-4357/aa93e7
dc.type.version publishedVersion


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