The infrared evolution of Sakurai's Object

T. R. Geballe; A. Evans; B. Smalley; V. H. Tyne; S. P S Eyres

doi:10.1023/A:1014683521291

The infrared evolution of Sakurai's Object

T. R. Geballe^*, A. Evans, B. Smalley, V. H. Tyne, S. P S Eyres

^*Corresponding author for this work

Faculty of Computing, Engineering and Science

Research output: Contribution to journal › Article › peer-review

15 Citations (Scopus)

Abstract

Infrared spectroscopy and photometry have revealed the remarkable evolution 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 to absorption and emission by newly formed dust located outside the photosphere. In addition, a strong and broad helium 1.083 μm P Cygni line developed, signifying the acceleration of an outer envelope of material to speeds as high as 1000 km s^-1. At the same time the photosphere of the central star remained quiescent. By 1999 the photosphere was virtually completely obscured by the dust and the helium emission line was the only detectable spectral feature remaining in the 1-5 μm band. In 2000 emission by dust has become even more dominant, as the envelope continues to expand and cool and the helium line weakens.

Original language	English
Pages (from-to)	39-49
Number of pages	11
Journal	Astrophysics and Space Science
Volume	279
Issue number	1-2
DOIs	https://doi.org/10.1023/A:1014683521291
Publication status	Published - 2002
Event	Sakurai's Object: What have we learned in the first five years? - Keele University, United Kingdom Duration: 3 Aug 2000 → 4 Aug 2000

Keywords

Stars: AGB and post-AGB
Stars: evolution
Stars: individual (Sakurai's Object (V4334 Sgr))
Stars: peculiar

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@article{2b99a2d0c2884faba7d365c75ef5da19,

title = "The infrared evolution of Sakurai's Object",

abstract = "Infrared spectroscopy and photometry have revealed the remarkable evolution 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 to absorption and emission by newly formed dust located outside the photosphere. In addition, a strong and broad helium 1.083 μm P Cygni line developed, signifying the acceleration of an outer envelope of material to speeds as high as 1000 km s-1. At the same time the photosphere of the central star remained quiescent. By 1999 the photosphere was virtually completely obscured by the dust and the helium emission line was the only detectable spectral feature remaining in the 1-5 μm band. In 2000 emission by dust has become even more dominant, as the envelope continues to expand and cool and the helium line weakens.",

keywords = "Stars: AGB and post-AGB, Stars: evolution, Stars: individual (Sakurai's Object (V4334 Sgr)), Stars: peculiar",

author = "Geballe, {T. R.} and A. Evans and B. Smalley and Tyne, {V. H.} and Eyres, {S. P S}",

year = "2002",

doi = "10.1023/A:1014683521291",

language = "English",

volume = "279",

pages = "39--49",

journal = "Astrophysics and Space Science",

issn = "0004-640X",

publisher = "Springer",

number = "1-2",

note = "Sakurai's Object : What have we learned in the first five years? ; Conference date: 03-08-2000 Through 04-08-2000",

}

TY - JOUR

T1 - The infrared evolution of Sakurai's Object

AU - Geballe, T. R.

AU - Evans, A.

AU - Smalley, B.

AU - Tyne, V. H.

AU - Eyres, S. P S

PY - 2002

Y1 - 2002

N2 - Infrared spectroscopy and photometry have revealed the remarkable evolution 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 to absorption and emission by newly formed dust located outside the photosphere. In addition, a strong and broad helium 1.083 μm P Cygni line developed, signifying the acceleration of an outer envelope of material to speeds as high as 1000 km s-1. At the same time the photosphere of the central star remained quiescent. By 1999 the photosphere was virtually completely obscured by the dust and the helium emission line was the only detectable spectral feature remaining in the 1-5 μm band. In 2000 emission by dust has become even more dominant, as the envelope continues to expand and cool and the helium line weakens.

AB - Infrared spectroscopy and photometry have revealed the remarkable evolution 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 to absorption and emission by newly formed dust located outside the photosphere. In addition, a strong and broad helium 1.083 μm P Cygni line developed, signifying the acceleration of an outer envelope of material to speeds as high as 1000 km s-1. At the same time the photosphere of the central star remained quiescent. By 1999 the photosphere was virtually completely obscured by the dust and the helium emission line was the only detectable spectral feature remaining in the 1-5 μm band. In 2000 emission by dust has become even more dominant, as the envelope continues to expand and cool and the helium line weakens.

KW - Stars: AGB and post-AGB

KW - Stars: evolution

KW - Stars: individual (Sakurai's Object (V4334 Sgr))

KW - Stars: peculiar

U2 - 10.1023/A:1014683521291

DO - 10.1023/A:1014683521291

M3 - Article

AN - SCOPUS:0013346313

SN - 0004-640X

VL - 279

SP - 39

EP - 49

JO - Astrophysics and Space Science

JF - Astrophysics and Space Science

IS - 1-2

T2 - Sakurai's Object

Y2 - 3 August 2000 through 4 August 2000

ER -

The infrared evolution of Sakurai's Object

Abstract

Keywords

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