Modelling the dust around Sakurai's Object

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

*Awdur cyfatebol y gwaith hwn

Allbwn ymchwil: Cyfraniad at gyfnodolynErthygladolygiad gan gymheiriaid

1 Dyfyniad (Scopus)

Crynodeb

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.

Iaith wreiddiolSaesneg
Tudalennau (o-i)139-147
Nifer y tudalennau9
CyfnodolynAstrophysics and Space Science
Cyfrol279
Rhif cyhoeddi1-2
Dynodwyr Gwrthrych Digidol (DOIs)
StatwsCyhoeddwyd - 2002
DigwyddiadSakurai's Object: What have we learned in the first five years? - Keele University, Y Deyrnas Unedig
Hyd: 3 Aug 20004 Aug 2000

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