The Propagation of Magnetocentrifugally Launched Jets. I.

Frank, Adam; Lery, Thibaut; Gardiner, Thomas A.; Jones, T. W.; Ryu, Dongsu

doi:10.1086/309298

Cited by 33 publications

(27 citation statements)

References 36 publications

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“…These effects were attributed to the hoop stresses imposed upon the flow by the toroidal field. In subsequent work, Frank et al (2000) added greater realism by using analytical models of MCL launching to specify the cross-sectional distributions of the jet's state variables. The resulting radial stratification of density and magnetic field led to new propagation behavior manifested principally by the development of an inner jet core within a lower density collar.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Nested-Wind Scenarios for Bipolar Outflows: Preplanetary and Yso Nebular Shaping

Dennis

Frank

Blackman

et al. 2009

ApJ

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We present results of a series of magnetohydrodynamic (MHD) and hydrodynamic (HD) 2.5 dimensional simulations of the morphology of outflows driven by nested wide-angle winds, i.e., winds that emanate from a central star as well as from an orbiting accretion disk. While our results are broadly relevant to nested-wind systems, we have tuned the parameters of the simulations to touch on issues in both young stellar objects and planetary nebula (PN) studies. In particular, our studies connect to open issues in the early evolution of PNs. We find that nested MHD winds exhibit marked morphological differences from the single MHD wind case along both dimensions of the flow. Nested HD winds, on the other hand, give rise mainly to geometric distortions of an outflow that is topologically similar to the flow arising from a single stellar HD wind. Our MHD results are insensitive to changes in ambient temperature between ionized and un-ionized circumstellar environments. The results are sensitive to the relative mass-loss rates and the relative speeds of the stellar and disk winds. We also present synthetic emission maps of both nested MHD and HD simulations. We find that nested MHD winds show knots of emission appearing on-axis that do not appear in the HD case.

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Section: Introductionmentioning

confidence: 99%

Magnetic Nested-Wind Scenarios for Bipolar Outflows: Preplanetary and Yso Nebular Shaping

Dennis

Frank

Blackman

et al. 2009

ApJ

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“…Can jets be ejected in the same manner in the axisymmetric cases? The stability of propagating jets has been studied by taking the accretion disk as the fixed boundary condition in twodimensional MHD (e.g., Ustyugova et al 1995;Ouyed & Pudritz 1997a, 1999Romanova et al 1998;Hardee & Rosen 1999Frank et al 2000), three-dimensional MHD ( Nakamura et al 2001;Ouyed et al 2003;Nakamura & Meier 2004), and three-dimensional SPMHD (smoothed particle MHD) simulations (Cerqueira & de Gouveia Dal Pino 2001). The three-dimensional treatment is necessary for investigating the stability of the jet against the nonaxisymmetric modes.…”

Section: Introductionmentioning

confidence: 99%

Three‐dimensional Magnetohydrodynamic Simulations of Jets from Accretion Disks

Kigure

Shibata

2005

ApJ

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We report the results of three-dimensional magnetohydrodynamic ( MHD) simulations of a jet formation by the interaction between an accretion disk and a large-scale magnetic field. The disk is not treated as a boundary condition but is solved self-consistently. To investigate the stability of the MHD jet, the accretion disk is perturbed with a nonaxisymmetric sinusoidal or random fluctuation of the rotational velocity. The dependences of the jet velocity (v z ), mass outflow rate (Ṁ w ), and mass accretion rate (Ṁ a ) on the initial magnetic field strength in both nonaxisymmetric cases are similar to those in the axisymmetric case. That is, v z / B 1 = 3 0 ,Ṁ w / B 0 , anḋ M a / B 1:4 0 , where B 0 is the initial magnetic field strength. The former two relations are consistent with Michel's steady solution, v z / (B 2 0 /Ṁ w ) 1 = 3 , although the jet and accretion do not reach the steady state. In both perturbation cases, a nonaxisymmetric structure with m ¼ 2 appears in the jet, where m is the azimuthal wavenumber. This structure cannot be explained by Kelvin-Helmholtz instability and seems to originate in the accretion disk. Nonaxisymmetric modes in the jet reach almost constant levels after about 1.5 orbital periods of the accretion disk, while all modes in the accretion disk grow with oscillation. As for the angular momentum transport by Maxwell stress, the vertical component, hB B z /4 i, is comparable to the radial component, hB B r /4 i, in the wide range of initial magnetic field strength.

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“…In a search for possible signatures of magnetic fields on the large scales of the YSO outflows, several MHD investigations of overdense, radiative cooling jets, have been carried out with the help of multidimensional numerical simulations both in twodimensions (2-D) [22,[25][26][27][28]35,44,[61][62][63] and in three-dimensions (3-D) ( [7][8][9][10][11], see also [18,19] for reviews). [7]).…”

Section: Effects Of Magnetic Fields On the Jet Structutre And Propagamentioning

confidence: 99%

The Role of Magnetic Fields on Astrophysical Jets

Pino¹,

Elisabete²

2005

AIP Conference Proceedings

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Abstract. Highly collimated supersonic jets and less collimated outflows are observed to emerge from a wide variety of astrophysical objects. They are seen in young stellar objects (YSOs), proto-planetary nebulae, compact objects (such as galactic black holes or microquasars, and X-ray binary stars), and in the nuclei of active galaxies (AGNs). Despite their different physical scales (in size, velocity, and amount of energy transported), they have strong morphological similarities. What is the universal mechanism that can explain their origin? In this lecture, I briefly review the role that magnetic fields seem to play on the formation, structure, and propagation of these jets.

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The Propagation of Magnetocentrifugally Launched Jets. I.

Cited by 33 publications

References 36 publications

Magnetic Nested-Wind Scenarios for Bipolar Outflows: Preplanetary and Yso Nebular Shaping

Magnetic Nested-Wind Scenarios for Bipolar Outflows: Preplanetary and Yso Nebular Shaping

Three‐dimensional Magnetohydrodynamic Simulations of Jets from Accretion Disks

The Role of Magnetic Fields on Astrophysical Jets

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