Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-17T15:22:33.526Z Has data issue: false hasContentIssue false
  • English
  • Français

Pulsations and Dust Formation in R Coronae Borealis Stars

Published online by Cambridge University Press:  12 April 2016

Geoffrey C. Clayton ,
Barbara A. Whitney  and
Warrick A. Lawson
Geoffrey C. Clayton
Affiliation:
Center for Astrophysics and Space Astronomy, Campus Box 389, University of Colorado, Boulder, CO 80309
Barbara A. Whitney
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138
Warrick A. Lawson
Affiliation:
Department of Physics, University College, University of New South Wales, Australian Defence Force Academy, Canberra ACT 2600, Australia

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 observed correlation between pulsational phase in RCB stars and the timing of their declines shows empirically that the stellar pulsations and dust formation are intimately connected (e.g., Lawson et al. 1992). However, the nature of this relationship and the process of dust formation itself are not well understood. We have shown that it is likely that dust is forming in close proximity (< 2 stellar radii) to the RCB star photosphere, based on time scales for acceleration of the dust, eclipse of the chromospheric region, and dispersal of the dust (Clayton et al. 1992, 1993; Whitney, Balm & Clayton 1993; Whitney et al. 1993). The temperature at which amorphous carbon forms can be as high as 4000 K, and can occur in conditions far removed from thermodynamic equilibrium, as long as a mechanism exists to contain carbon atoms within a given volume. A likely form of carbon condensate is fullerenes such as C60 (Whitney, Balm & Clayton 1993). Shocks in the stellar atmosphere due to the pulsations may provide such a mechanism for containing the carbon. However, no spectroscopic signature related to the dust formation has been seen. We have searched unsuccessfully for IR emission bands of C60 (Clayton et al. 1995a).

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 155: Astrophysical Applications of Stellar Pulsation , 1995 , pp. 433 - 434
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

Clayton, G.C., Whitney, B.A., Stanford, S.A., & Drilling, J. 1992, ApJ, 397, 652 CrossRefGoogle Scholar
Clayton, G.C., Lawson, W.A., Whitney, B.A., & Pollacco, D.L. 1993, MNRAS, 264, L13 Google Scholar
Clayton, G.C., Lawson, W.A., Cottrell, P.L., Whitney, B.A., Stanford, S.A., & de Ruyter, F. 1994, ApJ, 432, 785 CrossRefGoogle Scholar
Clayton, G.C., Kelly, D.M., Lacy, J.H., Little-Marenin, I.R., Feldman, P.A., & Bernath, P.F. 1995a, AJ, in press (May)Google Scholar
Clayton, G.C., Whitney, B.A., Meade, M.R., Babler, B., Bjorkman, K.S., & Nordsieck, K.H. 1995, PASP, in pressGoogle Scholar
Lawson, W.A., Cottrell, P.L., Gilmore, A.C., & Kilmartin, P.M. 1992, MNRAS, 256, 339 Google Scholar
Whitney, B.A., Clayton, G.C., Schulte-Ladbeck, R.E., Calvet, N., Hartmann, L., & Kenyon, S.J. 1993, ApJ, 417, 687 CrossRefGoogle Scholar
Whitney, B.A, Balm, S.P., & Clayton, G.C. 1993, Luminous High-Latitude Stars, ASP Conference Series No. 45, ed. Sasselov, D., p. 115 Google Scholar