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dc.contributor.authorNarayan, R.
dc.contributor.authorMcKinney, J. C.
dc.contributor.authorFarmer, A. J.
dc.date.accessioned2019-09-22T14:23:54Z
dc.date.issued2007
dc.identifier.citationNarayan, R., J. C. McKinney, and A. J. Farmer. 2007. “Self-Similar Force-Free Wind from an Accretion Disc.” Monthly Notices of the Royal Astronomical Society 375 (2): 548–66. https://doi.org/10.1111/j.1365-2966.2006.11272.x.
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384883*
dc.description.abstractWe consider a self-similar force-free wind flowing out of an infinitely thin disc located in the equatorial plane. On the disc plane, we assume that the magnetic stream function P scales as P proportional to R(nu), where R is the cylindrical radius. We also assume that the azimuthal velocity in the disc is constant: v(phi) = Mc, where M < 1 is a constant. For each choice of the parameters nu and M, we find an infinite number of solutions that are physically well-behaved and have fluid velocity <= c throughout the domain of interest. Among these solutions, we show via physical arguments and time-dependent numerical simulations that the minimum-torque solution, i.e. the solution with the smallest amount of toroidal field, is the one picked by a real system. For nu >= 1, the Lorentz factor of the outflow increases along a field line as gamma approximate to M(z/R(fp))((2-nu)/2) approximate to R/R(A), where R(fp) is the radius of the foot-point of the field line on the disc and R(A) = R(fp)/M is the cylindrical radius at which the field line crosses the Alfven surface or the light cylinder. For nu < 1, the Lorentz factor follows the same scaling for z/R(fp) < M(-1/(1-nu)), but at larger distances it grows more slowly: gamma (z/R(fp))(nu/2). For either regime of nu, the dependence of gamma on M shows that the rotation of the disc plays a strong role in jet acceleration. On the other hand, the poloidal shape of a field line is given by z/R(fp) approximate to (R/R(fp))(2/(2-nu)) and is independent of M. Thus rotation has neither a collimating nor a decollimating effect on field lines, suggesting that relativistic astrophysical jets are not collimated by the rotational winding up of the magnetic field.
dc.language.isoen_US
dc.publisherOxford University Press
dash.licenseLAA
dc.titleSelf-similar force-free wind from an accretion disc
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalMonthly Notices of the Royal Astronomical Society
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:23:54Z
dash.workflow.comments1Science Serial ID 66200
dc.identifier.doi10.1111/j.1365-2966.2006.11272.x
dash.source.volume375;2
dash.source.page548-566


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