Intense radio outburst from the supermassive star Eta Carinae

1995 ◽  
Vol 441 ◽  
pp. L73 ◽  
Author(s):  
R. A. Duncan ◽  
S. M. White ◽  
J. Lim ◽  
G. J. Nelson ◽  
S. A. Drake ◽  
...  



1986 ◽  
Vol 64 (4) ◽  
pp. 520-522 ◽  
Author(s):  
E. R. Seaquist ◽  
A. R. Taylor

We present observations that show that the symbiotic star CH Cygni recently underwent a strong radio outburst that produced a radio-emitting thermal jet. The jet is two-sided and is expanding lengthwise at an observed rate (end to end) of 1 arcsec/year, corresponding to a transverse velocity of 1100 km∙s−1 in each direction. The electron density on January 22, 1985 exceeded 2 × 106 cm−3, and the mass of the (ionized) gas exceeded [Formula: see text]. The emergence of the jet coincided with a decline in the visual luminosity of [Formula: see text].The data are consistent with a jet produced by supercritical accretion in a binary containing a red giant and a [Formula: see text] white dwarf. The discovery of a jet in such a system provides confirming evidence of the role played by accretion in determining the optical and radio properties of this system. It is also the first expanding jet found to be associated with an evolved stellar object.



2010 ◽  
Vol 6 (S272) ◽  
pp. 56-61
Author(s):  
Jose H. Groh

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.



Massive Stars ◽  
2010 ◽  
pp. 116-125
Author(s):  
Theodore. R. Gull
Keyword(s):  


2016 ◽  
Vol 464 (1) ◽  
pp. 775-782 ◽  
Author(s):  
Amit Kashi
Keyword(s):  


1998 ◽  
pp. 112-117
Author(s):  
Daniel Fischer ◽  
Hilmar Duerbeck
Keyword(s):  


1976 ◽  
Vol 174 (1) ◽  
pp. 59P-62P
Author(s):  
A. D. Thackeray
Keyword(s):  


2009 ◽  
Vol 698 (2) ◽  
pp. L142-L146 ◽  
Author(s):  
M. Tavani ◽  
S. Sabatini ◽  
E. Pian ◽  
A. Bulgarelli ◽  
P. Caraveo ◽  
...  


2017 ◽  
Author(s):  
Eva Leser ◽  
Stefan Ohm ◽  
Matthias Füßling ◽  
Mathieu de Naurois ◽  
Kathrin Egberts ◽  
...  
Keyword(s):  


1915 ◽  
Vol 8 ◽  
pp. 134-134
Author(s):  
R. F. Sanford
Keyword(s):  


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