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

Research output: Contribution to journalArticlepeer-review

1 Citation (Scopus)


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 languageEnglish
Pages (from-to)139-147
Number of pages9
JournalAstrophysics and Space Science
Issue number1-2
Publication statusPublished - 2002
EventSakurai's Object: What have we learned in the first five years? - Keele University, United Kingdom
Duration: 3 Aug 20004 Aug 2000


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


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