W61 28-5 , the SIMBAD biblio

W61 28-5 , the SIMBAD biblio (10 results) C.D.S. - SIMBAD4 rel 1.8 - 2024.04.24CEST00:08:36


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Title First 3 Authors
1961UppAn...5a...1W 386 0 Population I in the Large Magellanic Cloud WESTERLUND B.
2000AJ....119.2214M viz 654 146 The progenitor masses of Wolf-Rayet stars and luminous blue variables determined from cluster turnoffs. I. Results from 19 OB associations in the Magellanic clouds. MASSEY P., WATERHOUSE E. and DEGIOIA-EASTWOOD K.
2004ApJ...608.1001M 1 27 81 The physical properties and effective temperature scale of O-type stars as a function of metallicity. I. A sample of 20 stars in the Magellanic clouds. MASSEY P., BRESOLIN F., KUDRITZKI R.P., et al.
2005ApJ...627..477M 1 52 168 The physical properties and effective temperature scale of O-type stars as a function of metallicity. II. Analysis of 20 more Magellanic cloud stars and results from the complete sample. MASSEY P., PULS J., PAULDRACH A.W.A., et al.
2007A&A...473..603M 16       D               1 123 294 The empirical metallicity dependence of the mass-loss rate of O- and early B-type stars. MOKIEM M.R., DE KOTER A., VINK J.S., et al.
2009AJ....138.1003B viz 15       D               1 1760 163 Spitzer SAGE infrared photometry of massive stars in the Large Magellanic Cloud. BONANOS A.Z., MASSA D.L., SEWILO M., et al.
2012ApJ...745..173W viz 15       D               1 307 56 Interstellar H I and H2 in the Magellanic Clouds: an expanded sample based on ultraviolet absorption-line data. WELTY D.E., XUE R. and WONG T.
2012A&A...543A..95R 867       D     X C F     21 26 33 Nitrogen line spectroscopy in O-stars. III. The earliest O-stars. RIVERO GONZALEZ J.G., PULS J., MASSEY P., et al.
2015MNRAS.449.1545B 16       D     X     *   2 22 14 No breakdown of the radiatively driven wind theory in low-metallicity environments. BOURET J.-C., LANZ T., HILLIER D.J., et al.
2016MNRAS.458..624C 218       D     X C       5 123 147 The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters. CROWTHER P.A., CABALLERO-NIEVES S.M., BOSTROEM K.A., et al.

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