![]() A few very luminous O stars are found close to the main sequence, while all other, slightly evolved stars obey a strict luminosity limit. The upper Hertzsprung–Russell diagram (HRD) is well populated by the stars of our sample from a specific field in the SMC Wing. The stellar rotation rates show broad, tentatively bimodal distributions. We find that the stellar winds of our sample stars are generally much weaker than theoretically expected. The spectra, which we obtained with the ESO Very Large Telescope, were analyzed using state-of-the-art stellar atmosphere models, and the stellar parameters were determined. Here we report a spectroscopic study of 320 massive stars of spectral types O (23 stars) and B (297 stars) in the Wing of the Small Magellanic Cloud (SMC). At low metallicities, the properties of massive stars and their evolution are not yet fully explored. These massive stars are the primary sources of stellar feedback in star-forming galaxies. Stars that start their lives with spectral types O and early B are the progenitors of core-collapse supernovae, long gamma-ray bursts, neutron stars, and black holes. University of Washington, Physics-Astronomy Bldg. National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ 85719, USA Institute of Astrophysics, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, BelgiumĪrmagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK 18, Kazan, Russiaĭepartment of Astronomy, University of Wisconsin, Madison, WI, USA 24/25, 14476 Potsdam, GermanyĮ-mail: Federal University, Kremlevskaya Ul. Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. Astronomical objects: linking to databases.Including author names using non-Roman alphabets. ![]() Suggested resources for more tips on language editing in the sciences ![]() Punctuation and style concerns regarding equations, figures, tables, and footnotes ![]()
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