Matches in SemOpenAlex for { <https://semopenalex.org/work/W2100580327> ?p ?o ?g. }
- W2100580327 endingPage "1978" @default.
- W2100580327 startingPage "1961" @default.
- W2100580327 abstract "We present a Spitzer Space Telescope spectroscopic survey of mass-losing carbon stars (and one oxygen-rich star) in the Large Magellanic Cloud (LMC). The stars represent the superwind phase on the asymptotic giant branch (AGB), which forms a major source of dust for the interstellar medium (ISM) in galaxies. Bolometric magnitudes indicate progenitor masses of 1.5–2.5 M⊙. The spectra cover the wavelength range 5–38 μm. They show varying combinations of dust continuum, dust emission features (SiC, MgS) and molecular absorption bands (C2H2, HCN). A 10-μm absorption feature is attributed to C3. A weak band at 5.8 μm is suggestive of carbonyl. The circumstellar 7.5-μm C2H2 band is found to be stronger at lower metallicity, explained by higher C/O ratios at low metallicity. The J−K versus K−A colours, used to select the sample, are shown to be relatively insensitive in separating carbon versus oxygen-rich AGB stars. The predominance of carbon stars therefore indicates that in the range 1.5–2.5 M⊙, LMC AGB stars become carbon-rich before onset of the superwind. A set of four narrow bands, dubbed the Manchester system, is used to define the infrared continuum for dusty carbon stars. We investigate the strength and central wavelength of the SiC and MgS dust bands as a function of colour and metallicity. The line-to-continuum ratio of these bands shows some indication of being lower at low metallicity. The MgS band is only seen at dust temperatures below 600 K. Metal-poor carbon stars can form amorphous carbon dust from self-produced carbon. The formation efficiency of oxygen-rich dust depends more strongly on metallicity. In lower-metallicity environments, the dust input into the ISM by AGB stars may be strongly biased towards carbonaceous dust." @default.
- W2100580327 created "2016-06-24" @default.
- W2100580327 creator A5002739725 @default.
- W2100580327 creator A5006775177 @default.
- W2100580327 creator A5008721221 @default.
- W2100580327 creator A5009865434 @default.
- W2100580327 creator A5010603271 @default.
- W2100580327 creator A5014266201 @default.
- W2100580327 creator A5024793349 @default.
- W2100580327 creator A5037517484 @default.
- W2100580327 creator A5046253050 @default.
- W2100580327 creator A5047686813 @default.
- W2100580327 creator A5053319490 @default.
- W2100580327 creator A5071008791 @default.
- W2100580327 creator A5071551115 @default.
- W2100580327 creator A5077701450 @default.
- W2100580327 creator A5088644422 @default.
- W2100580327 creator A5091219628 @default.
- W2100580327 date "2006-07-10" @default.
- W2100580327 modified "2023-10-17" @default.
- W2100580327 title "A Spitzer mid-infrared spectral survey of mass-losing carbon stars in the Large Magellanic Cloud" @default.
- W2100580327 cites W1505467319 @default.
- W2100580327 cites W1507274015 @default.
- W2100580327 cites W1539581072 @default.
- W2100580327 cites W1611442573 @default.
- W2100580327 cites W1632903569 @default.
- W2100580327 cites W1925822734 @default.
- W2100580327 cites W1944419244 @default.
- W2100580327 cites W1964902417 @default.
- W2100580327 cites W1983475934 @default.
- W2100580327 cites W1988928004 @default.
- W2100580327 cites W1993198210 @default.
- W2100580327 cites W1995350130 @default.
- W2100580327 cites W1997416041 @default.
- W2100580327 cites W1998366461 @default.
- W2100580327 cites W1998749206 @default.
- W2100580327 cites W2000003859 @default.
- W2100580327 cites W2000826532 @default.
- W2100580327 cites W2001066902 @default.
- W2100580327 cites W2010638118 @default.
- W2100580327 cites W2015241906 @default.
- W2100580327 cites W2018858432 @default.
- W2100580327 cites W2020124438 @default.
- W2100580327 cites W2021821595 @default.
- W2100580327 cites W2025921570 @default.
- W2100580327 cites W2026992256 @default.
- W2100580327 cites W2031304246 @default.
- W2100580327 cites W2032944511 @default.
- W2100580327 cites W2033058438 @default.
- W2100580327 cites W2053950905 @default.
- W2100580327 cites W2054023954 @default.
- W2100580327 cites W2055045249 @default.
- W2100580327 cites W2057099245 @default.
- W2100580327 cites W2063018817 @default.
- W2100580327 cites W2066049120 @default.
- W2100580327 cites W2078611869 @default.
- W2100580327 cites W2083698116 @default.
- W2100580327 cites W2087069688 @default.
- W2100580327 cites W2094204948 @default.
- W2100580327 cites W2096865198 @default.
- W2100580327 cites W2097882773 @default.
- W2100580327 cites W2099582083 @default.
- W2100580327 cites W2101176118 @default.
- W2100580327 cites W2102082889 @default.
- W2100580327 cites W2104584484 @default.
- W2100580327 cites W2112265517 @default.
- W2100580327 cites W2118908971 @default.
- W2100580327 cites W2125120917 @default.
- W2100580327 cites W2128737399 @default.
- W2100580327 cites W2134830549 @default.
- W2100580327 cites W2136929298 @default.
- W2100580327 cites W2141690498 @default.
- W2100580327 cites W2148341398 @default.
- W2100580327 cites W2155141611 @default.
- W2100580327 cites W2158710097 @default.
- W2100580327 cites W2158987644 @default.
- W2100580327 cites W2160540079 @default.
- W2100580327 cites W2160952939 @default.
- W2100580327 cites W2162623014 @default.
- W2100580327 cites W2167812666 @default.
- W2100580327 cites W2167878877 @default.
- W2100580327 cites W2168023905 @default.
- W2100580327 cites W2168076848 @default.
- W2100580327 cites W3003952632 @default.
- W2100580327 cites W3097994407 @default.
- W2100580327 cites W3098613545 @default.
- W2100580327 cites W3099206180 @default.
- W2100580327 cites W3099270657 @default.
- W2100580327 cites W3100599857 @default.
- W2100580327 cites W3106356347 @default.
- W2100580327 cites W3123997635 @default.
- W2100580327 cites W4240733135 @default.
- W2100580327 cites W4296765245 @default.
- W2100580327 cites W4300680226 @default.
- W2100580327 cites W4301438637 @default.
- W2100580327 cites W4302406267 @default.
- W2100580327 doi "https://doi.org/10.1111/j.1365-2966.2006.10623.x" @default.
- W2100580327 hasPublicationYear "2006" @default.