Modelling the dust around Sakurai's Object

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

doi:10.1023/A:1014672712630

Modelling the dust around Sakurai's Object

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

^*Corresponding author for this work

Faculty of Computing, Engineering and Science

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

1 Citation (Scopus)

Abstract

We follow the evolution of the infrared excess and the dust shell of Sakurai's Object by modelling the dust emission. The optical depth, dust temperature, and shell thickness parameters from the models are presented. Fits of DUSTY models to infrared spectra between 1997 May and 1999 September illustrate the development of the dust from small grains to a range of grain sizes with an almost constant 60% graphite - 40% amorphous carbon mixture. The size of the infrared emitting region continues to grow and may now be big enough to resolve. This may help to answer questions such as the morphology of the dust shell, and whether the dust shell is 'blobby' or smooth.

Original language	English
Pages (from-to)	139-147
Number of pages	9
Journal	Astrophysics and Space Science
Volume	279
Issue number	1-2
DOIs	https://doi.org/10.1023/A:1014672712630
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

Dust development
Infrared emission
IR spectra
Stars: individual (Sakurai's Object)

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10.1023/A:1014672712630Licence: CC BY-NC-ND

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@article{93aaf5fb702740be87e2283f14632385,

title = "Modelling the dust around Sakurai's Object",

abstract = "We follow the evolution of the infrared excess and the dust shell of Sakurai's Object by modelling the dust emission. The optical depth, dust temperature, and shell thickness parameters from the models are presented. Fits of DUSTY models to infrared spectra between 1997 May and 1999 September illustrate the development of the dust from small grains to a range of grain sizes with an almost constant 60% graphite - 40% amorphous carbon mixture. The size of the infrared emitting region continues to grow and may now be big enough to resolve. This may help to answer questions such as the morphology of the dust shell, and whether the dust shell is 'blobby' or smooth.",

keywords = "Dust development, Infrared emission, IR spectra, Stars: individual (Sakurai's Object)",

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

year = "2002",

doi = "10.1023/A:1014672712630",

language = "English",

volume = "279",

pages = "139--147",

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 - Modelling the dust around Sakurai's Object

AU - Tyne, V. H.

AU - Smalley, B.

AU - Geballe, T. R.

AU - Eyres, S. P S

AU - Evans, A.

PY - 2002

Y1 - 2002

N2 - We follow the evolution of the infrared excess and the dust shell of Sakurai's Object by modelling the dust emission. The optical depth, dust temperature, and shell thickness parameters from the models are presented. Fits of DUSTY models to infrared spectra between 1997 May and 1999 September illustrate the development of the dust from small grains to a range of grain sizes with an almost constant 60% graphite - 40% amorphous carbon mixture. The size of the infrared emitting region continues to grow and may now be big enough to resolve. This may help to answer questions such as the morphology of the dust shell, and whether the dust shell is 'blobby' or smooth.

AB - We follow the evolution of the infrared excess and the dust shell of Sakurai's Object by modelling the dust emission. The optical depth, dust temperature, and shell thickness parameters from the models are presented. Fits of DUSTY models to infrared spectra between 1997 May and 1999 September illustrate the development of the dust from small grains to a range of grain sizes with an almost constant 60% graphite - 40% amorphous carbon mixture. The size of the infrared emitting region continues to grow and may now be big enough to resolve. This may help to answer questions such as the morphology of the dust shell, and whether the dust shell is 'blobby' or smooth.

KW - Dust development

KW - Infrared emission

KW - IR spectra

KW - Stars: individual (Sakurai's Object)

U2 - 10.1023/A:1014672712630

DO - 10.1023/A:1014672712630

M3 - Article

AN - SCOPUS:0141457577

VL - 279

SP - 139

EP - 147

JO - Astrophysics and Space Science

JF - Astrophysics and Space Science

SN - 0004-640X

IS - 1-2

T2 - Sakurai's Object

Y2 - 3 August 2000 through 4 August 2000

ER -

Modelling the dust around Sakurai's Object

Abstract

Keywords

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