Hostname: page-component-84b7d79bbc-4hvwz Total loading time: 0 Render date: 2024-07-26T05:15:30.951Z Has data issue: false hasContentIssue false
  • English
  • Français

3.0 To 3.5 Micron Spectrum of V348 Sgr and R CrB

Published online by Cambridge University Press:  12 April 2016

K. Nandy ,
N. Kameswara Rao  and
D.H. Morgan
K. Nandy
Affiliation:
1. Royal Observatory, Edinburgh
N. Kameswara Rao
Affiliation:
2. Indian Institute of Astrophysics, Bangalore 560034
D.H. Morgan
Affiliation:
1. Royal Observatory, Edinburgh

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The circumstellar dust in R CrB stars is often thought to be due to graphite, because of the high carbon abundance in the stars. Further, the spectra of these stars in the infrared show feature-less smooth continuum (Forrest 1974, Roche and Aitken 1984) which was also thought to be characteristic of graphite. However, the recent comparison of the ultraviolet spectra obtained at maximum and minimum light of R CrB showed an extinction peak in the region of 2400 to 2500A (Holm, Wu & Doherty 1982, Hecht et al. 1984) which was identified as due to amorphous or glassy carbon particles. According to Duley and Williams (1981,83) amorphous carbon is supposed to show spectral features in the 3.3-3.4 μm region. Further many dust emission features are also supposed to appear in the spectral region 3 to 3.5 μm (Aikten 1981). The previous studies in this spectral region in R CrB (Forrest 1974) and in the hotter star V348 Sgr (Allen et al. 1982) showed smooth continuum. V348 Sgr shows spectroscopically many similarities with other WC 11 stars and was grouped with CPD-56°8032, He 2-113 and M4-18 (Webster and Glass 1974). All these three stars show strong dust emission features at 3.3, 8.6 11.25 μm. With a view to search for weaker dust spectral features we obtained the spectrum of R CrB and V348 Sgr with higher resolution than employed before.

Type
IV Cool Hydrogen Deficient Stars
Information
International Astronomical Union Colloquium , Volume 87: Hydrogen Deficient Stars and Related Objects , 1985 , pp. 203 - 205
Copyright
Copyright © Reidel 1986

References

Allen, D.A., Baines, D.W.T., Blades, J.C., Whittet, D.C.B., 1982: MNRAS 199, 1017.Google Scholar
Aitken, D.K., 1981: IAU Symp. 96, p.207.Google Scholar
Duley, W.W., and Williams, D.A., 1981: MNRAS 196, 269.CrossRefGoogle Scholar
Duley, W.W., and Williams, D.A., 1983: MNRAS, 205, p.67.Google Scholar
Forrest, W.J., 1974: Thesis Univ. Calif. San Diego.Google Scholar
Hecht, J.H., Holm, A.V., Donn, B., and Wu, C.C., 1984: Ap. J. 280, 228.Google Scholar
Holm, A.V., Wu, C.C. and doherty, L.R., 1982: PASP, 94, 548.Google Scholar
Roche, P.F., and Aitken, D.K., 1984: MNRAS, 208, 481.Google Scholar
Wade, R., 1983: UKIRT Users and Operations Manual.Google Scholar
Webster, B.L., and Glass, I.S., 1974: MNRAS, 166, 491.Google Scholar