%0 Generic %1 citeulike:13506215 %A Lingam, Manasvi %A Mahajan, Swadesh M. %D 2015 %K imported %T Modeling astrophysical outflows via the unified Dynamo-Reverse Dynamo mechanism %U http://arxiv.org/abs/1501.06509 %X The unified Dynamo-Reverse Dynamo (Dy-RDy) mechanism, capable of simultaneously generating large scale outflows and magnetic fields from an ambient microscopic reservoir, is explored in a broad astrophysical context. The Dy-RDy mechanism is derived via Hall magnetohydrodynamics, which unifies the evolution of magnetic field and fluid vorticity. It also introduces an intrinsic length scale, the ion skin depth, allowing for the proper normalization and categorization of microscopic and macroscopic scales. The large scale Alfvén Mach number \$M\_A\$, defining the relative äbundance" of the flow field to the magnetic field is shown to be tied to a microscopic scale length that reflects the characteristics of the ambient short scale reservoir. The dynamo (Dy), preferentially producing the large scale magnetic field, is the dominant mode when the ambient turbulence is mostly kinetic, while the outflow producing reverse dynamo (RDy) is the principal manifestation of a magnetically dominated turbulent reservoir. It is conjectured that an efficient RDy may be the source of many observed astrophysical outflows that have \$M\_A 1\$.

@misc{citeulike:13506215, abstract = {The unified Dynamo-Reverse Dynamo (Dy-RDy) mechanism, capable of simultaneously generating large scale outflows and magnetic fields from an ambient microscopic reservoir, is explored in a broad astrophysical context. The Dy-RDy mechanism is derived via Hall magnetohydrodynamics, which unifies the evolution of magnetic field and fluid vorticity. It also introduces an intrinsic length scale, the ion skin depth, allowing for the proper normalization and categorization of microscopic and macroscopic scales. The large scale Alfv\'en Mach number \$\mathcal{M}\_{A}\$, defining the relative "abundance" of the flow field to the magnetic field is shown to be tied to a microscopic scale length that reflects the characteristics of the ambient short scale reservoir. The dynamo (Dy), preferentially producing the large scale magnetic field, is the dominant mode when the ambient turbulence is mostly kinetic, while the outflow producing reverse dynamo (RDy) is the principal manifestation of a magnetically dominated turbulent reservoir. It is conjectured that an efficient RDy may be the source of many observed astrophysical outflows that have \$\mathcal{M}\_{A} \gg 1\$.}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Lingam, Manasvi and Mahajan, Swadesh M.}, biburl = {https://www.bibsonomy.org/bibtex/238c377bff75c6f2fac2e19f8ea195ded/ericblackman}, citeulike-article-id = {13506215}, citeulike-linkout-0 = {http://arxiv.org/abs/1501.06509}, citeulike-linkout-1 = {http://arxiv.org/pdf/1501.06509}, day = 26, eprint = {1501.06509}, interhash = {c750cf1ec987a3d4d01345e973a59b66}, intrahash = {38c377bff75c6f2fac2e19f8ea195ded}, keywords = {imported}, month = jan, posted-at = {2015-02-02 08:06:15}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{Modeling astrophysical outflows via the unified Dynamo-Reverse Dynamo mechanism}}, url = {http://arxiv.org/abs/1501.06509}, year = 2015 }