The Evolution of the Circumstellar Shell of C‐J Stars: New Models Based on Gemini∕T‐ReCS Observations

de Mello, Ana Beatriz; Martins, Silvia Lorenz

doi:doi:10.1063/1.3099252

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The Evolution of the Circumstellar Shell of C‐J Stars: New Models Based on Gemini∕T‐ReCS Observations

AIP Conf. Proc. 1094, pp. 860-863; doi:10.1063/1.3099252 (4 pages)

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun

Date: 21–25 July 2008

Location: St. Andrews (Scotland)

Ana Beatriz de Mello¹ and Silvia Lorenz Martins²

¹Observatório Nacional‐Rua Gen. Jose Cristino 77, Rio de Janeiro, RJ, Brazil
²Observatório do Valongo∕UFRJ‐Lad. Pedro Antônio 43, Rio de Janeiro, RJ, Brazil

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Abstract

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A large number of questions related to the C‐J type carbon stars remain unanswered. The circumstellar shell of these stars is usually carbon‐rich, as one would expect. Nevertheless, there is a peculiar group of C‐J stars which were classified as silicon‐rich C‐J stars, due to their emission at 9.8 μm. This kind of emission is commonly seen in oxygen‐rich stars and is connected to silicon dust grains at the circumstellar shell. Following the most established theories, the occurrence of this peculiar type of circumstellar shell around carbon‐rich stars can only exist if the AGB star in question is in fact part of binary system. In this work we present an analysis of the circumstellar shell of 2 C‐J stars using LRS‐IRAS and T‐ReCS Gemini spectra obtained in 1986 and 2007, respectively. One is a normal C‐J star, namely C∗ 2123, and the other is a silicon‐rich C‐J, MC79 2–11. The joint study of the two kinds of C‐J stars allows a more representative analysis of this class of stars.

KEYWORDS and PACS

Keywords

circumstellar matter, giant stars, Monte Carlo methods

PACS

97.10.Fy

Circumstellar shells, clouds, and expanding envelopes; circumstellar masers
97.20.Li

Giant and subgiant stars
02.70.Uu

Applications of Monte Carlo methods