Two Micron All Sky Survey,<i>Infrared Astronomical Satellite</i>, and<i>Midcourse Space Experiment</i>Color Properties of Intrinsic and Extrinsic S Stars

Yang, Xiaohong; Chen, Peisheng; Wang, Jiancheng; He, Jianhua

doi:10.1086/506965

Cited by 16 publications

(19 citation statements)

References 13 publications

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“…These indications come from Paper II, where we describe how they were obtained. (originally, they derive from Van Eck et al 2000;Yang et al 2006). Apart from a few uncertain cases, the sources considered in this case are all intrinsic AGB stars.…”

Section: The Samplementioning

confidence: 99%

Infrared photometry and evolution of mass-losing AGB stars

Guandalini¹

2010

A&A

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Context. The asymptotic giant branch (AGB) phase marks the end of the evolution for low-and intermediate-mass stars, which are fundamental contributors to the mass return to the interstellar medium and to the chemical evolution of galaxies. The detailed understanding of mass loss processes is hampered by the poor knowledge of the luminosities and distances of AGB stars. Aims. In a series of papers we are trying to establish criteria permitting a more quantitative determination of luminosities for the various types of AGB stars, using the infrared (IR) fluxes as a basis. An updated compilation of the mass loss rates is also required, as it is crucial in our studies of the evolutionary properties of these stars. In this paper we concentrate our analysis on the study of the mass loss rates for a sample of galactic S stars. Methods. We reanalyze the properties of the stellar winds for a sample of galactic MS, S, SC stars with reliable estimates of the distance on the basis of criteria previously determined. We then compare the resulting mass loss rates with those previously obtained for a sample of C-rich AGB stars. Results. Stellar winds in S stars are on average less efficient than those of C-rich AGB stars of the same luminosity. Near-to-mid infrared colors appear to be crucial in our analysis. They show a good correlation with mass loss rates in particular for the Mira stars. We suggest that the relations between the rates of the stellar winds and both the near-to-mid infrared colors and the periods of variability improve the understanding of the late evolutionary stages of low mass stars and could be the origin of the relation between the rates of the stellar winds and the bolometric magnitudes.

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Section: The Samplementioning

confidence: 99%

Infrared photometry and evolution of mass-losing AGB stars

Guandalini¹

2010

A&A

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“…Extrinsic S stars are not AGB stars. Several methods have been used to separate extrinsic and intrinsic S stars (e.g., Yang et al 2006). S stars tend to have low mass-loss rate, implying less efficient dust formation.…”

Section: (C) S Starsmentioning

confidence: 99%

A Catalog of Agb Stars in Iras PSC

Suh

Kwon²

2009

Journal of The Korean Astronomical Society

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We make a new catalog of AGB stars in our Galaxy from the sources listed in the Infrared Astronomical Satellite (IRAS) point source catalog (PSC) compiling the lists of previous works with verifying processes. We verify the class identification of AGB stars into oxygen-rich and carbon-rich stars using the information from recent investigations. For the large sample of AGB stars, we present infrared two-color diagrams from the observations at near infrared bands and IRAS PSC. On the two-color diagrams, we plot the tracks of theoretical radiative transfer model results with increasing dust shell optical depths. Comparing the observations with the theoretical tracks, we discuss the meaning of the infrared two-color diagrams.

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“…Of the 17 S stars, 15 stars are intrinsic S stars (Jorissen et al 1993) or candidate intrinsic S stars (Yang et al 2006). Of the two remaining stars, one is an extrinsic S star (Jorissen et al 1993) and the other is a candidate extrinsic S star (Yang et al 2006) (hereafter, the objects with known type and candidates are not distinguished).…”

Section: The Iso Sws01 Observations Of S Starsmentioning

confidence: 99%

“…In the calculation of S star magnitudes, we have considered measurement errors and interstellar extinction correction. If the measured errors of 2MASS JHK magnitudes are larger than the interstellar extinction correction, the latter correction can be ignored, otherwise the JHK magnitudes must be dereddened (Yang et al 2006). The IRAS fluxes are converted to magnitudes using 12, 25, and 60 µm bands zero-magnitude fluxes of 28.3, 6.73, and 1.19 Jy, respectively (IRAS Explanatory Supplement 1988).…”

Section: The Classification Of 17 S Starsmentioning

confidence: 99%

“…(6) and (7) lists the classifications of the IRAS LRS spectra (Kwok et al 1997) and the spectral type (Keenan 1954;Keenan & Boeshaar 1980;Little-Marenin & Little 1988), respectively; Cols. (8) to (10) give the 2MASS JHK magnitudes (Yang et al 2006), respectively; Cols. (11) to (13) give the IRAS 12, 25, and 60 µm magnitudes, respectively.…”

Section: The Classification Of 17 S Starsmentioning

confidence: 99%

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Analysis of ISO SWS01 spectra of S stars

PS(陈培生)

2006

A&A

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The Infrared Space Observatory (ISO) Short-Wavelength Spectrometer (SWS01) plays an important role in studying properties of S stars. We reduce and analyze the SWS01 spectra of 17 S stars, and identify the candidate carriers of molecular absorption features. The ISO Spectral Analysis Package (ISAP) developed by the LWS and SWS Instrument Teams and Data Centers is used to process and analyze the SWS01 spectra of 17 S stars. The ISO archives of 17 S stars are obtained from the ISO database. Of 17 S stars, two stars are extrinsic S stars, the others are intrinsic S stars. The 15 intrinsic S stars can be divided into three groups (6 stars for Group I, 7 stars for Group II, and 2 stars for Group III) according to their Infrared Astronomical Satellite (IRAS) low-resolution spectra (LRS) and dust mass-loss rateṀ dust , whereṀ dust increases from Group I to II and III gradually. 17 S stars show the following properties: 1. two extrinsic S stars and 15 intrinsic S stars among different groups have different infrared properties; 2. two extrinsic S stars and 6 intrinsic S stars in Group I have similar ISO SWS01 spectra and their continua can be approximately described by a single blackbody representing the stellar photosphere, while some intrinsic S stars in Group I have 60 µm infrared excess; 3. for intrinsic S stars in Groups I, II, and III, their continua peak shifts toward longer wavelength from Groups I to II to III; 4. S stars in Groups II and III show obvious dust emission features in which the ∼10 µm dust features seem to display two different shapes. Moreover, two S stars (IRAS 00192-2020 & IRAS 15492+4837) present the 13 µm feature; 5. molecules H 2 O, CO, and CO 2 greatly affect the ISO SWS01 spectra of S stars. It is noted that the absorption features of molecules CS and HCN usually thought to exist only in C stars may appear in the S stars.

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Two Micron All Sky Survey,Infrared Astronomical Satellite, andMidcourse Space ExperimentColor Properties of Intrinsic and Extrinsic S Stars

Cited by 16 publications

References 13 publications

Infrared photometry and evolution of mass-losing AGB stars

Infrared photometry and evolution of mass-losing AGB stars

A Catalog of Agb Stars in Iras PSC

Analysis of ISO SWS01 spectra of S stars

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