Magnetohydrodynamic jets from different magnetic field configurations Export

@article{citeulike:3649546, abstract = {Using axisymmetric MHD simulations we investigate how the overall jet formation is affected by a variation in the disk magnetic flux profile and/or the existence of a central stellar magnetosphere. Our simulations evolve from an initial, hydrostatic equilibrium state in a force-free magnetic field configuration. We find a unique relation between the collimation degree and the disk wind magnetization power law exponent. The collimation degree decreases for steeper disk magnetic field profiles. Highly collimated outflows resulting from a flat profile tend to be unsteady. We further consider a magnetic field superposed of a stellar dipole and a disk field in parallel or anti-parallel alignment. Both stellar and disk wind may evolve in a pair of outflows, however, a reasonably strong disk wind component is essential for jet collimation. Strong flares may lead to a sudden change in mass flux by a factor two. We hypothesize that such flares may eventually trigger jet knots.}, archivePrefix = {arXiv}, author = {Fendt, Christian}, citeulike-article-id = {3649546}, citeulike-linkout-0 = {http://arxiv.org/abs/0811.3416}, citeulike-linkout-1 = {http://arxiv.org/pdf/0811.3416}, day = {20}, eprint = {0811.3416}, keywords = {jet, magnetohydrodynamics, mhd, simulations}, month = {Nov}, posted-at = {2008-11-21 15:05:17}, priority = {2}, title = {Magnetohydrodynamic jets from different magnetic field configurations}, url = {http://arxiv.org/abs/0811.3416}, year = {2008} }

TY - JOUR ID - citeulike:3649546 L3 - citeulike-article-id:3649546 N2 - Using axisymmetric MHD simulations we investigate how the overall jet formation is affected by a variation in the disk magnetic flux profile and/or the existence of a central stellar magnetosphere. Our simulations evolve from an initial, hydrostatic equilibrium state in a force-free magnetic field configuration. We find a unique relation between the collimation degree and the disk wind magnetization power law exponent. The collimation degree decreases for steeper disk magnetic field profiles. Highly collimated outflows resulting from a flat profile tend to be unsteady. We further consider a magnetic field superposed of a stellar dipole and a disk field in parallel or anti-parallel alignment. Both stellar and disk wind may evolve in a pair of outflows, however, a reasonably strong disk wind component is essential for jet collimation. Strong flares may lead to a sudden change in mass flux by a factor two. We hypothesize that such flares may eventually trigger jet knots. TI - Magnetohydrodynamic jets from different magnetic field configurations KW - jet KW - magnetohydrodynamics KW - mhd KW - simulations AU - Fendt, Christian PY - 2008/Nov/20/ UR - http://arxiv.org/abs/0811.3416 ER -