The Multiple System SK—67°18 in the LMC

Niemelä, Virpi Sinikka; Seggewiss, W.; Moffat, A. F. J.

doi:10.1007/978-94-011-0205-6_59

Cited by 2 publications

(2 citation statements)

References 3 publications

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“…The sources, in chronological order, are codified as follows: 60: Feast et al (1960) 68: Smith (1968b) 76: Fehrenbach et al (1976) 77: Walborn (1977 78: Melnick (1978) 81: Breysacher (1981) 82a: Conti (1982) 82b: Phillips (1982) 82c: Walborn (1982a) 83a: Massey & Conti (1983a) 83b: 83c: Conti & Garmany (1983) 83d: Mathewson et al (1983) 84: Cowley et al (1984) 85a: Azzopardi & Breysacher (1985) 85b: Morgan & Good (1985) 85c: Melnick (1985) 86a: Walborn (1986) 86b: Moffat & Seggewiss (1986) 87a: Moffat et al (1987) 87b: Morgan & Good (1987) 88a : Breysacher (1988) 88b: Torres-Dodgen & Massey (1988) 89a: Conti & Massey (1989) 89b: Bohannan & Walborn (1989) 89c: Moffat (1989) 90a: Moffat et al (1990) 90b: Smith et al (1990a) 90c: Morgan & Good (1990) 90d: Heydari-Malayeri et al (1990) 90e: Testor & Schild (1990) 91a: Niemela (1991) 91b: Pakull (1991 92a: Schild & Testor (1992) 92b: Heydari-Malayeri & Melnick (1992) 93a: Heydari-Malayeri et al (1993) 93b: Testor et al (1993) 94 : Heap et al (1994) 95a: Bartzakos et al (1995) 95b: Niemela (1995) 95c: Niemela et al (1995) 95d: 95e: …”

Section: The Cataloguementioning

confidence: 99%

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The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud

Breysacher

Azzopardi²,

Testor

1999

Astron. Astrophys. Suppl. Ser.

153

184

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Abstract. The catalogue provides for each of the 134 W-R stars of Population I presently known in the Large Magellanic Cloud, accurate equatorial coordinates, photometric data, spectral classification, binary status, correlation with OB associations and HII regions. The miscellaneous designations of the stars are also listed. Although completeness is not pretended, results published during the last decade are highlighted in the notes given for each individual star. A uniform set of finding charts is presented.

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Section: The Cataloguementioning

confidence: 99%

“…According to Niemela et al (1995), the object appears to be a high-mass (∼80 M ) multiple system containing an eclipsing binary (P 2 days) which primary component is not of spectral type WN but probably of type O3f * .…”

Section: Bat99-5 (Brey 4)mentioning

confidence: 99%

The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud

Breysacher

Azzopardi²,

Testor

1999

Astron. Astrophys. Suppl. Ser.

153

184

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The Wolf-Rayet stars in the Large Magellanic Cloud

Hainich

Rühling

Todt

et al. 2014

A&A

201

310

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Context. Massive stars, although being important building blocks of galaxies, are still not fully understood. This especially holds true for Wolf-Rayet (WR) stars with their strong mass loss, whose spectral analysis requires adequate model atmospheres. Aims. Following our comprehensive studies of the WR stars in the Milky Way, we now present spectroscopic analyses of almost all known WN stars in the LMC. Methods. For the quantitative analysis of the wind-dominated emission-line spectra, we employ the Potsdam Wolf-Rayet (PoWR) model atmosphere code. By fitting synthetic spectra to the observed spectral energy distribution and the available spectra (ultraviolet and optical), we obtain the physical properties of 107 stars. Results. We present the fundamental stellar and wind parameters for an almost complete sample of WN stars in the LMC. Among those stars that are putatively single, two different groups can be clearly distinguished. While 12% of our sample are more luminous than 10 6 L and contain a significant amount of hydrogen, 88% of the WN stars, with little or no hydrogen, populate the luminosity range between log (L/L ) = 5.3 ... 5.8. Conclusions. While the few extremely luminous stars (log (L/L ) > 6), if indeed single stars, descended directly from the main sequence at very high initial masses, the bulk of WN stars have gone through the red-supergiant phase. According to their luminosities in the range of log (L/L ) = 5.3 ... 5.8, these stars originate from initial masses between 20 and 40 M . This mass range is similar to the one found in the Galaxy, i.e. the expected metallicity dependence of the evolution is not seen. Current stellar evolution tracks, even when accounting for rotationally induced mixing, still partly fail to reproduce the observed ranges of luminosities and initial masses. Moreover, stellar radii are generally larger and effective temperatures correspondingly lower than predicted from stellar evolution models, probably due to subphotospheric inflation.

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The Multiple System SK—67°18 in the LMC

Cited by 2 publications

References 3 publications

The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud

The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud

The Wolf-Rayet stars in the Large Magellanic Cloud

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