Fermi acceleration under control: $\eta$ Carinae

Evidence of Fermi Acceleration of Lyα in the Radio Galaxy 1243+036

The Astrophysical Journal ◽

10.1086/306206 ◽

1998 ◽

Vol 505 (2) ◽

pp. 634-638 ◽

Cited By ~ 6

Author(s):

Luc Binette ◽

Benoit Joguet ◽

John C. L. Wang

Keyword(s):

Radio Galaxy ◽

Fermi Acceleration

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Adiabatic Fermi acceleration of energetic particles between converging interplanetary shock waves

Journal of Geophysical Research Atmospheres ◽

10.1029/ja081i001p00051 ◽

1976 ◽

Vol 81 (1) ◽

pp. 51-59 ◽

Cited By ~ 31

Author(s):

E. H. Levy ◽

S. P. Duggal ◽

M. A. Pomerantz

Keyword(s):

Shock Waves ◽

Interplanetary Shock ◽

Energetic Particles ◽

Fermi Acceleration

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Stimulated Amplification under Spatially Nonhomogeneous Conditions: An Astrophysical Fe II Laser in the Vicinity of Eta Carinae

Physica Scripta ◽

10.1088/0031-8949/2005/t120/015 ◽

2005 ◽

Vol T120 ◽

pp. 99-104

Author(s):

S Johansson ◽

V Letokhov

Keyword(s):

Eta Carinae

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Effects of fast rotation on the wind of Luminous Blue Variables

Proceedings of the International Astronomical Union ◽

10.1017/s1743921311009975 ◽

2010 ◽

Vol 6 (S272) ◽

pp. 56-61

Author(s):

Jose H. Groh

Keyword(s):

Near Infrared ◽

Rotational Velocity ◽

Spectral Lines ◽

High Resolution Spectroscopy ◽

Luminous Blue Variables ◽

Eta Carinae ◽

Fast Rotation ◽

Long Baseline ◽

Infrared Interferometry ◽

Fast Rotating

AbstractWhile theoretical studies have long suggested a fast-rotating nature of Luminous Blue Variables (LBVs), observational confirmation of fast rotation was not detected until recently. Here I discuss the diagnostics that have allowed us to constrain the rotational velocity of LBVs: broadening of spectral lines and latitude-dependent variations of the wind density structure. While rotational broadening can be directly detected using high-resolution spectroscopy, long-baseline near-infrared interferometry is needed to directly measure the shape of the latitude-dependent photosphere that forms in a fast-rotating star. In addition, complex 2-D radiative transfer models need to be employed if one's goal is to constrain rotational velocities of LBVs. Here I illustrate how the above methods were able to constrain the rotational velocities of the LBVs AG Carinae, HR Carinae, and Eta Carinae.

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