The Infrared Evolution of Sakurai's Object

Gemini Observatory; Keele University; Liverpool John Moores University
Astrophysics and Space Science (Impact Factor: 2.06). 02/2002; 279(1):39-49. DOI: 10.1023/A:1014683521291
Source: arXiv

ABSTRACT Infrared spectroscopy and photometry have revealed the remarkableevolution of Sakurai''s Object from 1996 to the present. A cooling,carbon-rich photospheric spectrum was observable from 1996 to 1998.Considerable changes occured in 1998 as the continuum reddened due toabsorption and emission by newly formed dust located outside thephotosphere. In addition, a strong and broad helium 1.083 m P Cygniline developed, signifying the acceleration of an outer envelope ofmaterial to speeds as high as 1000 km s-1. At the same time thephotosphere of the central star remained quiescent. By 1999 thephotosphere was virtually completely obscured by the dust and the heliumemission line was the only detectable spectral feature remaining in the1–5 m band. In 2000 emission by dust has become even more dominant,as the envelope continues to expand and cool and the helium line weakens.

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    ABSTRACT: Techniques and results of computations of model atmospheres are discussed for M and C giants and for giants with abundance anomalies. The SAM12 code, a modification of the ATLAS12 code developed by Kurucz, is used. Blanketing effects due to atomic and molecular line absorption are taken into account using the opacity-sampling approach. The computed model atmosphere for the Sun (G2V) is used as a test of the SAM12 code. The model red-giant atmospheres are compared with models reported in other studies. Comparisons between the computed and observed spectral energy distributions are given for the C giant WX Cyg (C-J6) and Sakurai's object (V4334 Sgr).
    Astronomy Reports 12/2002; 47(1):59-67. · 0.76 Impact Factor

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