Novae in M31 in 1999–2005

Alksnis, A.; Smirnova, O. B.; Zharova, A. V.

doi:10.1134/s1063773708080082

Cited by 8 publications

(10 citation statements)

References 11 publications

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“…It is clear from these references that the dust ejection cannot be in the form of a spherically symmetric shell. A similar phenomenon has been noted in the photographic red magnitudes of northern C stars, measured over a period of 30 yr (Alksnis 2003).…”

Section: Long‐term Trends Obscuration Events and The Rcb Phenomenonsupporting

confidence: 81%

Near-infrared photometry of carbon stars

Whitelock

Feast

Marang

et al. 2006

Monthly Notices of the Royal Astronomical Society

180

344

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Near‐infrared, JHKL, photometry of 239 Galactic C‐rich variable stars is presented and discussed. From these and published data, the stars were classified as Mira or non‐Mira variables, and amplitudes and pulsation periods, ranging from 222 to 948 d for the Miras, were determined for most of them. A comparison of the colour and period relations with those of similar stars in the Large Magellanic Cloud indicates minor differences, which may be the consequence of sample selection effects. Apparent bolometric magnitudes were determined by combining the mean JHKL fluxes with mid‐infrared photometry from IRAS and MSX. Then, using the Mira period luminosity relation to set the absolute magnitudes, distances were determined – to greater accuracy than has hitherto been possible for this type of star. Bolometric corrections to the K magnitude were calculated and prescriptions derived for calculating these from various colours. Mass‐loss rates were also calculated and compared to values in the literature. Approximately one‐third of the C‐rich Miras and an unknown fraction of the non‐Miras exhibit apparently random obscuration events that are reminiscent of the phenomena exhibited by the hydrogen‐deficient R Coronae Borealis stars. The underlying cause of this is unclear, but it may be that mass loss, and consequently dust formation, is very easily triggered from these very extended atmospheres.

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Section: Long‐term Trends Obscuration Events and The Rcb Phenomenonsupporting

confidence: 81%

Near-infrared photometry of carbon stars

Whitelock

Feast

Marang

et al. 2006

Monthly Notices of the Royal Astronomical Society

180

344

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“…CIT 6 (RW LMi, GL 1403, IRC+30219, IRAS 10131+3049) was first discovered during the Caltech 2-µm sky survey and was among the 14 very red infrared-bright optical-faint sources found (Ulrich et al 1966). CIT 6 is characterized by its very low color temperature, implying that the star is surrounded by a very thick dust envelope and has been identified as a long-period variable with a period of about 628 days (Alksnis 1995). From the periodluminosity relation, Cohen & Hitchon (1996) estimated the distance of CIT 6 to be 400 ± 50 pc, which is slightly more distant than IRC+10216, which has a distance of between ∼ 120 pc (Groenewegen et al 1998) and ∼ 150 pc (Lucas & Guélin 1999).…”

Section: Introductionmentioning

confidence: 99%

A Molecular Line Survey of the Highly Evolved Carbon Star Cit 6

Zhang

Kwok

Dinh-V-Trung

2009

ApJ

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We present a spectral line survey of the C-rich envelope CIT 6 in the λ 2 mm and 1.3 mm bands carried out with the Arizona Radio Observatory (ARO) 12 m telescope and the Heinrich Hertz Submillimeter Telescope (SMT). The observations cover the frequency ranges of 131-160 GHz, 219-244 GHz, and 252-268 GHz with typical sensitivity limit of T R < 10 mK. A total of 74 individual emission features are detected, of which 69 are identified to arise from 21 molecular species and isotopologues, with 5 faint lines remaining unidentified. Two new molecules (C 4 H and CH 3 CN) and seven new isotopologues (C 17 O, 29 SiC 2 , 29 SiO, 30 SiO, 13 CS, C 33 S, and C 34 S) are detected in this object for the first time. The column densities, excitation temperatures, and fractional abundances of the detected molecules are determined using rotation diagram analysis. Comparison of the spectra of CIT 6 to that of IRC+10216 suggests that the spectral properties of CIT 6 are generally consistent with those of IRC+10216. For most of the molecular species, the intensity ratios of the lines detected in the two objects are in good agreement with each other. Nevertheless, there is evidence suggesting enhanced emission from CN and HC 3 N and depleted emission from HCN, SiS, and C 4 H in CIT 6. Based on their far-IR spectra, we find that CIT 6 probably has a lower dust-to-molecular gas ratio than IRC+10216. To investigate the chemical evolution of evolved stars, we compare the molecular abundances in the AGB envelopes CIT 6 and IRC+10216 and those in the bright proto-planetary nebula CRL 618. The implication on the circumstellar chemistry is discussed.

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“…Up to now, a series of surveys have been conducted for searching the Galactic carbon stars such as the Automatic Plate Measuring (APM) survey (Totten & Irwin 1998;Ibata et al 2001), the First Byurakan Spectral Sky Survey (Gigoyan et al 1998) and infrared objective-prism surveys (Alksnis et al 2001, and references therein). In particular, Alksnis et al (2001) published a catalogue containing 6 891 carbon stars, which is the revised version of the General Catalogue of Cool Carbon Stars maintained by B. C. Stephenson of the Warner and Swasey Observatory (Stephenson , 1989.…”

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confidence: 99%

Carbon Stars From Lamost Dr2 Data

Cui

Liu

et al. 2016

ApJS

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In this work, we present the new catalog of carbon stars from the LAMOST DR2 catalog. In total, 894 carbon stars are identified from multiple line indices measured from the stellar spectra. Combining the CN bands in the red end with C 2 and other lines, we are able to identify the carbon stars. Moreover, we also classify the carbon stars into spectral sub-types of C-H, C-R, and C-N. These sub-types approximately show distinct features in the multi-dimensional line indices, implying that in the future we can use them to identify carbon stars from larger spectroscopic datasets. Meanwhile, from the line indices space, while the C-N stars are clearly separated from the others, we find no clear separation between C-R and C-H sub-types. The C-R and C-H stars seem to smoothly transition from one to another. This may hint that the C-R and C-H 2 Ji et al.stars may not be different in their origins but look different in their spectra because of different metallicity. Due to the relatively low spectral resolution and lower signalto-noise ratio, the ratio of 12 C/ 13 C is not measured and thus the C-J stars are not identified.

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Novae in M31 in 1999–2005

Cited by 8 publications

References 11 publications

Near-infrared photometry of carbon stars

Near-infrared photometry of carbon stars

A Molecular Line Survey of the Highly Evolved Carbon Star Cit 6

Carbon Stars From Lamost Dr2 Data

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