On the magnetic acceleration and collimation of astrophysical outflows

Bogovalov, S. V.; Tsinganos, K.

doi:10.1046/j.1365-8711.1999.02413.x

Cited by 106 publications

(130 citation statements)

References 35 publications

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“…The phenomenon does not appear to have been much considered in the astrophysical context in contrast to magnetic collimation or magnetic centrifugal acceleration (e.g. Bogovalov & Tsinganos 1999;Banerjee & Pudritz 2006). The most simple r θ manner to appreciate the phenomenon is through the magnetic pressure, B 2 /2μ 0 (Demichev et al 1965).…”

Section: Magnetic Deflection Of the Ejecta In The Omc-1 Explosionmentioning

confidence: 99%

A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1)

Nissen¹,

Cunningham²,

Gustafsson³

et al. 2012

A&A

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Context. Stars whose mass is an order of magnitude greater than the Sun play a prominent role in the evolution of galaxies, exploding as supernovae, triggering bursts of star formation and spreading heavy elements about their host galaxies. A fundamental aspect of star formation is the creation of an outflow. The fast outflow emerging from a region associated with massive star formation in the Orion Molecular Cloud 1 (OMC-1), located behind the Orion Nebula, appears to have been set in motion by an explosive event. Aims. We study the structure and dynamics of outflows in OMC-1. We combine radial velocity and proper motion data for near-IR emission of molecular hydrogen to obtain the first 3-dimensional (3D) structure of the OMC-1 outflow. Our work illustrates a new diagnostic tool for studies of star formation that will be exploited in the near future with the advent of high spatial resolution spectro-imaging in particular with data from the Atacama Large Millimeter Array (ALMA). Methods. We used published radial and proper motion velocities obtained from the shock-excited vibrational emission in the H 2 v = 1−0 S(1) line at 2.122 μm obtained with the GriF instrument on the Canada-France-Hawaii Telescope, the Apache Point Observatory, the Anglo-Australian Observatory, and the Subaru Telescope. Results. These data give the 3D velocity of ejecta yielding a 3D reconstruction of the outflows. This allows one to view the material from different vantage points in space giving considerable insight into the geometry. Our analysis indicates that the ejection occurred < ∼ 720 years ago from a distorted ring-like structure of ∼15 (6000 AU) in diameter centered on the proposed point of close encounter of the stars BN, source I and maybe also source n. We propose a simple model involving curvature of shock trajectories in magnetic fields through which the origin of the explosion and the center defined by extrapolated proper motions of BN, I and n may be brought into spatial coincidence.

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Section: Magnetic Deflection Of the Ejecta In The Omc-1 Explosionmentioning

confidence: 99%

A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1)

Nissen¹,

Cunningham²,

Gustafsson³

et al. 2012

A&A

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“…In the special relativistic domain, simulations have been presented for coronal winds (Bogovalov & Tsinganos 1999;Tsinganos & Bogovalov 2002), and in the general relativistic domain for disk winds (e.g. Koide et al 1999Koide et al , 2001 to model the formation and collimation of relativistic outflows in the vicinity of black holes.…”

Section: Introductionmentioning

confidence: 99%

Nonradial and nonpolytropic astrophysical outflows

Méliani¹,

Sauty²,

Vlahakis³

et al. 2006

A&A

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Steady axisymmetric outflows originating at the hot coronal magnetosphere of a Schwarzschild black hole and surrounding accretion disk are studied in the framework of general relativistic magnetohydrodynamics (GRMHD). The assumption of meridional self-similarity is adopted for the construction of semi-analytical solutions of the GRMHD equations describing outflows close to the polar axis. In addition, it is assumed that relativistic effects related to the rotation of the black hole and the plasma are negligible compared to the gravitational and other energetic terms. The constructed model allows us to extend previous MHD studies for coronal winds from young stars to spine jets from Active Galactic Nuclei surrounded by disk-driven outflows. The outflows are thermally driven and magnetically or thermally collimated. The collimation depends critically on an energetic integral measuring the efficiency of the magnetic rotator, similarly to the non relativistic case. It is also shown that relativistic effects quantitatively affect the depth of the gravitational well and the coronal temperature distribution in the launching region of the outflow. Similarly to previous analytical and numerical studies, relativistic effects tend to increase the efficiency of the thermal driving but reduce the effect of magnetic self-collimation.

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“…In Bogovalov & Tsinganos (1999) and Tsinganos & Bogovalov (2000) it was found that, for a uniformly rotating base, only a small part of the total massand magnetic flux is collimated cylindrically. This fraction is only about 1% of the corresponding values of an assumed uncollimated outflow, i.e.…”

Section: Introductionmentioning

confidence: 96%

Magnetic collimation of the relativistic jet in M87

Tsinganos¹,

Bogovalov²

2005

AIP Conference Proceedings

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Abstract. We apply a two-zone MHD model to the jet of M87. The model consists of an inner relativistic outflow, which is surrounded by a non-relativistic outer disk-wind. The outer disk-wind collimates very well through magnetic self-collimation and confines the inner relativistic jet into a narrow region around the rotation axis. Further, we show by example, that such models reproduce very accurately the observed opening angle of the M87 jet over a large range from the kiloparsec scale down to the sub-parsec scale.

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On the magnetic acceleration and collimation of astrophysical outflows

Cited by 106 publications

References 35 publications

A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1)

A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1)

Nonradial and nonpolytropic astrophysical outflows

Magnetic collimation of the relativistic jet in M87

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