Observations of molecular envelopes of late-type stars: CRL 618, CRL 2688, CRL 3068, and CIT 6

Fukasaku, Sadafumi; Hirahara, Yasuhiro; Masuda, Akimasa; Kawaguchi, Kentarou; Ishikawa, Shinya; Kaifu, Norio; Irvine, William M.

doi:10.1086/175005

Cited by 36 publications

(48 citation statements)

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“…The J = 6-5 and J = 5-4 transitions of SiS in CRL 3068 have been previously observed by Bujarrabal et al (1994), Fukasaku et al (1994), and Woods et al (2003). In this survey, we conclusively detected four SiS transitions with higher J (8-7, 9-8, 13-12, and 14-13) transitions.…”

Section: Sissupporting

confidence: 82%

“…Table 2 also gives a comparison of our results with those derived by Fukasaku et al (1994) and Woods et al (2003). While more molecular species are detected in our survey, for the molecules that are commonly detected (but no necessarily from the same transitions), Table 2 shows that the N and f X values are in agreement within 1 order of magnitude.…”

Section: Column Densities and Abundancessupporting

confidence: 57%

“…HNC has been detected in CRL 3068 (Sopka et al 1989;Fukasaku et al 1994;Woods et al 2003). This species can be produced through a similar way to HCN.…”

Section: Hncmentioning

confidence: 99%

“…Wannier et al (1991) discovered relatively faint emission from C 3 H 2 . Radio observations toward CRL 3068 in the frequency ranges between 39-47 GHz and 85-91 GHz were carried out with the Nobeyama 45 m radio telescope by Fukasaku et al (1994), and the molecular species C 2 H, HC 5 N, C 4 H, and SiS were detected in this object for the first time. Woods et al (2003) reported a molecular line survey made with the SEST 15 m and Onsala 20 m telescopes.…”

Section: Introductionmentioning

confidence: 99%

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A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths

Zhang

Kwok

Nakashima

2009

ApJ

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We present the results of a molecular line survey of the extreme carbon star CRL 3068. The observations were carried out with the Arizona Radio Observatory (ARO) 12 m telescope and the Heinrich Hertz Submillimeter Telescope (SMT) at the λ 2 mm and λ 1.3 mm atmospheric windows. The observations cover the frequency bands from 130 to 162 GHz and 219.5 to 267.5 GHz. The typical sensitivities achieved are T R < 15 mK and T R < 7 mK for the ARO 12 m and SMT, respectively. Seventy-two individual emission features belonging to 23 molecular species and isotopologues were detected. Only three faint lines remain unidentified. SiS, and 30 SiS are detected in this object for the first time. Rotational-diagram analysis is carried out to determine the column densities and excitation temperatures. The isotopic ratios of the elements C, N, O, S, and Si have also been estimated. The results are consistent with stellar CNO processing and suggest that CRL 3068 is more carbon rich than IRC+10216 and CIT 6. It is also shown that the chemical composition in CRL 3068 is somewhat different from that in IRC+10216 with a more extensive synthesis of cyclic and long-chain molecules in CRL 3068. The results will provide valuable clues for better understanding circumstellar chemistry.

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Section: Sissupporting

confidence: 82%

Section: Column Densities and Abundancessupporting

confidence: 57%

“…HNC has been detected in CRL 3068 (Sopka et al 1989;Fukasaku et al 1994;Woods et al 2003). This species can be produced through a similar way to HCN.…”

Section: Hncmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths

Zhang

Kwok

Nakashima

2009

ApJ

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“…To date, these carbon-chain molecules include cyanopolyynes (HC 2nϩ1 N, n ϭ 1-4) and hydrocarbon radicals (C n H, n ϭ 1-8), as well as the cyanoethynyl radical C 3 N. The cyanopolyynes, in particular, appear in a variety of astrophysical environments including cold dark molecular clouds (Benson & Myers 1983), star-forming regions (Turner 1991), the diffuse interstellar clouds (Bell, Feldman, & Matthews 1983), and the circumstellar envelopes (CSEs) surrounding evolved mass-losing red giant stars (Jewell & Snyder 1984;Fukasaku et al 1994). Several different chemical models have been put forward to try to explain the large cyanopolyyne abundances inferred from observations.…”

Section: Introductionmentioning

confidence: 99%

Detection of HCCNC from IRC+10216

Gensheimer

1997

The Astrophysical Journal

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The J ϭ 9 -8 transition of HCCNC has been detected toward IRCϩ10216. The intensity of the line indicates that the column density of HCCNC toward IRCϩ10216 is N ϭ 8.4 ϫ 10 12 cm Ϫ2. The ratio of column densities N(HC 3 N)͞N(HCCNC) in IRCϩ10216 is 1130. This is a factor 2-7 larger than the ratio from TMC-1. The mere presence of HCCNC in IRCϩ10216 suggests that ion-molecule reactions are at least partly responsible for the production of HC 3 N in the circumstellar envelope. On the other hand, the high N(HC 3 N)͞N(HCCNC) ratio from IRCϩ10216, as compared to TMC-1, suggests that other chemical processes, such as fast neutral-neutral reactions, may also make a significant contribution to the production of HC 3 N in IRCϩ10216.

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Infrared study of the extreme carbon stars based on IRAS, 2MASS and ISO data

Chen

Shan

2007

Astrophys Space Sci

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We collected 55 galactic extreme carbon stars from the published literature in this paper. Observational data from IRAS, 2MASS and ISO were analyzed. The results show that the infrared properties of extreme carbon stars are quite different to those for ordinary visual carbon stars. It is shown from IRAS and 2MASS photometric data that extreme carbon stars have much redder infrared colors not only in the far infrared, but also in the near infrared, hence they have much thicker ciucumstellar envelopes and mass loss. It is also indicated from IRAS Low-Resolution Spectra (LRS) and ISO Short Wavelength Spectra (SWS) that they have much redder infrared spectra from 2 µm to 45 µm. The above results are believed to be the signature of undergoing the last stages of AGB evolution for extreme carbon stars.

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Observations of molecular envelopes of late-type stars: CRL 618, CRL 2688, CRL 3068, and CIT 6

Cited by 36 publications

References 0 publications

A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths

A Molecular Line Survey of the Extreme Carbon Star CRL 3068 at Millimeter Wavelengths

Detection of HCCNC from IRC+10216

Infrared study of the extreme carbon stars based on IRAS, 2MASS and ISO data

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