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Title: On the structure and stability of magnetic tower jets

Abstract

Modern theoretical models of astrophysical jets combine accretion, rotation, and magnetic fields to launch and collimate supersonic flows from a central source. Near the source, magnetic field strengths must be large enough to collimate the jet requiring that the Poynting flux exceeds the kinetic energy flux. The extent to which the Poynting flux dominates kinetic energy flux at large distances from the engine distinguishes two classes of models. In magneto-centrifugal launch models, magnetic fields dominate only at scales <~ 100 engine radii, after which the jets become hydrodynamically dominated (HD). By contrast, in Poynting flux dominated (PFD) magnetic tower models, the field dominates even out to much larger scales. To compare the large distance propagation differences of these two paradigms, we perform three-dimensional ideal magnetohydrodynamic adaptive mesh refinement simulations of both HD and PFD stellar jets formed via the same energy flux. We also compare how thermal energy losses and rotation of the jet base affects the stability in these jets. For the conditions described, we show that PFD and HD exhibit observationally distinguishable features: PFD jets are lighter, slower, and less stable than HD jets. Here, unlike HD jets, PFD jets develop current-driven instabilities that are exacerbated as coolingmore » and rotation increase, resulting in jets that are clumpier than those in the HD limit. Our PFD jet simulations also resemble the magnetic towers that have been recently created in laboratory astrophysical jet experiments.« less

Authors:
 [1];  [1];  [1];  [2];  [3];  [4];  [4]
  1. Univ. of Rochester, Rochester, NY (United States)
  2. Univ. Pierre et Marie Curie, Meudon (France); Ecole Normale Superieure, Paris (France)
  3. Rice Univ., Houston, TX (United States)
  4. Imperial College, London (United Kingdom)
Publication Date:
Research Org.:
Rice Univ., Houston, TX (United States)
Sponsoring Org.:
USDOE National Nuclear Security Administration (NNSA)
OSTI Identifier:
1334725
Grant/Contract Number:  
NA0000904
Resource Type:
Accepted Manuscript
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 757; Journal Issue: 1; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 97 MATHEMATICS AND COMPUTING; ISM: jets and outflows; methods: numerical; stars: magnetic field; stars: winds, outflows

Citation Formats

Huarte-Espinosa, M., Frank, A., Blackman, E. G., Ciardi, A., Hartigan, P., Lebedev, S. V., and Chittenden, J. P. On the structure and stability of magnetic tower jets. United States: N. p., 2012. Web. doi:10.1088/0004-637X/757/1/66.
Huarte-Espinosa, M., Frank, A., Blackman, E. G., Ciardi, A., Hartigan, P., Lebedev, S. V., & Chittenden, J. P. On the structure and stability of magnetic tower jets. United States. doi:10.1088/0004-637X/757/1/66.
Huarte-Espinosa, M., Frank, A., Blackman, E. G., Ciardi, A., Hartigan, P., Lebedev, S. V., and Chittenden, J. P. Wed . "On the structure and stability of magnetic tower jets". United States. doi:10.1088/0004-637X/757/1/66. https://www.osti.gov/servlets/purl/1334725.
@article{osti_1334725,
title = {On the structure and stability of magnetic tower jets},
author = {Huarte-Espinosa, M. and Frank, A. and Blackman, E. G. and Ciardi, A. and Hartigan, P. and Lebedev, S. V. and Chittenden, J. P.},
abstractNote = {Modern theoretical models of astrophysical jets combine accretion, rotation, and magnetic fields to launch and collimate supersonic flows from a central source. Near the source, magnetic field strengths must be large enough to collimate the jet requiring that the Poynting flux exceeds the kinetic energy flux. The extent to which the Poynting flux dominates kinetic energy flux at large distances from the engine distinguishes two classes of models. In magneto-centrifugal launch models, magnetic fields dominate only at scales <~ 100 engine radii, after which the jets become hydrodynamically dominated (HD). By contrast, in Poynting flux dominated (PFD) magnetic tower models, the field dominates even out to much larger scales. To compare the large distance propagation differences of these two paradigms, we perform three-dimensional ideal magnetohydrodynamic adaptive mesh refinement simulations of both HD and PFD stellar jets formed via the same energy flux. We also compare how thermal energy losses and rotation of the jet base affects the stability in these jets. For the conditions described, we show that PFD and HD exhibit observationally distinguishable features: PFD jets are lighter, slower, and less stable than HD jets. Here, unlike HD jets, PFD jets develop current-driven instabilities that are exacerbated as cooling and rotation increase, resulting in jets that are clumpier than those in the HD limit. Our PFD jet simulations also resemble the magnetic towers that have been recently created in laboratory astrophysical jet experiments.},
doi = {10.1088/0004-637X/757/1/66},
journal = {Astrophysical Journal},
number = 1,
volume = 757,
place = {United States},
year = {2012},
month = {9}
}

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