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Unidentified Species in Envelopes around Carbon Stars

Published online by Cambridge University Press:  21 February 2014

B. W. Jiang ,
A. Li ,
K. Zhang ,
J. M. Liu ,
J. Gao  and
A. Mishra
B. W. Jiang
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing 100875, China email: [email protected]
A. Li
Affiliation:
Department of Physics and Astronomy, University of Missouri, Columbia, MO 65211, USA
K. Zhang
Affiliation:
Department of Physics, California Institute of Technology, Pasadena, CA 91125, USA
J. M. Liu
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing 100875, China email: [email protected]
J. Gao
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing 100875, China email: [email protected]
A. Mishra
Affiliation:
Department of Physics and Astronomy, University of Missouri, Columbia, MO 65211, USA
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Abstract

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The infrared (IR) spectra of many evolved carbon-rich stars exhibit two prominent dust emission features peaking around 21μm and 30μm, with the former exclusively seen in proto-planetary nebulae (PPNe), while the latter seen in a much wider range of objects, including AGB stars, PPNe and planetary nebulae (PNe). The 30μm feature is seen in all the 21μm sources, but no correlation is found between these two features. Over a dozen carrier candidates have been proposed for the 21μm feature, but none of them has been widely accepted and the nature of the 21μm feature remains a mystery. The carrier of the 30μm feature also remains unidentified. MgS dust, once widely accepted as a valid carrier, was ruled out because of the sulfur budget problem. In this work we examine nano-sized FeO dust as a carrier for the 21μm feature. We calculate the IR emission spectrum of FeO nanodust which undergoes single-photon heating in PPNe. It is found that the 21μm feature emitted by FeO nanodust is too broad to explain the observed feature. For the 30μm feature, we argue that graphite could be a viable carrier. Graphite, provided its d.c. conductivity σd.c. exceeds ~100ohm−1cm−1, exhibits a pronounced band at 30μm.

Keywords

stars: carbon(stars:) circumstellar matterdustinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S297: The Diffuse Interstellar Bands , May 2013 , pp. 219 - 222
Copyright
Copyright © International Astronomical Union 2014 

References

Allamandola, L. J., Tielens, A. G. G. M., & Barker, J. R. 1985, ApJ, 290, L25CrossRefGoogle Scholar
Begemann, B., et al. 1994, ApJ, 423, L71Google Scholar
Cerrigone, L., Hora, J. L., Umana, G., Trigilio, C., Hart, A., & Fazio, G. 2011, ApJ, 738, 121CrossRefGoogle Scholar
Draine, B. T. & Lee, H. M. 1984, ApJ, 285, 89Google Scholar
Henning, T. & Mutschke, H. 1995, A&AS, 112, 143Google Scholar
Henning, T. & Mutschke, H. 1997, A&A, 327, 743Google Scholar
Hony, S., et al. 2003, A&A, 402, 211Google Scholar
Kwok, S., Volk, K. M., & Hrivnak, B. J. 1989, ApJ, 345, L51Google Scholar
Léger, A. & Puget, J. 1984, A&A, 137, L5Google Scholar
Lombaert, R., de Vries, B. L., de Koter, A., et al. 2012, A&A, 544, L18Google Scholar
Messenger, S., Speck, A., & Volk, K. 2013, ApJ, 764, 142Google Scholar
Posch, Th., Mutschke, H., & Andersen, A. 2004, ApJ, 616, 1167Google Scholar
Primak, W. 1956, Phys. Rev., 103, 544Google Scholar
Volk, K., Hrivnak, B. J., Matsuura, M., et al. 2011, ApJ, 735, 127Google Scholar
Zhang, K., Jiang, B. W., & Li, A. 2009a, MNRAS, 396, 1247Google Scholar
Zhang, K., Jiang, B. W., & Li, A. 2009b, ApJ, 702, 680Google Scholar