Bibcode
Schneider, F. R. N.; Sana, H.; Evans, C. J.; Bestenlehner, J. M.; Castro, N.; Fossati, L.; Gräfener, G.; Langer, N.; Ramírez-Agudelo, O. H.; Sabín-Sanjulián, C.; Simón-Díaz, S.; Tramper, F.; Crowther, P. A.; de Koter, A.; de Mink, S. E.; Dufton, P. L.; Garcia, M.; Gieles, M.; Hénault-Brunet, V.; Herrero, A.; Izzard, R. G.; Kalari, V.; Lennon, D. J.; Maíz Apellániz, J.; Markova, N.; Najarro, F.; Podsiadlowski, Ph.; Puls, J.; Taylor, W. D.; van Loon, J. Th.; Vink, J. S.; Norman, C.
Bibliographical reference
Science, Volume 359, Issue 6371, pp. 69-71 (2018).
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1
2018
Journal
Citations
185
Refereed citations
166
Description
The 30 Doradus star-forming region in the Large Magellanic Cloud is a
nearby analog of large star-formation events in the distant universe. We
determined the recent formation history and the initial mass function
(IMF) of massive stars in 30 Doradus on the basis of spectroscopic
observations of 247 stars more massive than 15 solar masses (M☉).
The main episode of massive star formation began about 8 million years
(My) ago, and the star-formation rate seems to have declined in the last
1 My. The IMF is densely sampled up to 200 M☉ and contains 32
± 12% more stars above 30 M☉ than predicted by a standard
Salpeter IMF. In the mass range of 15 to 200 M☉, the IMF power-law
exponent is 1.90‑0.26+0.37, shallower than the Salpeter value of
2.35.
Related projects
Physical properties and evolution of Massive Stars
This project aims at the searching, observation and analysis of massive stars in nearby galaxies to provide a solid empirical ground to understand their physical properties as a function of those key parameters that gobern their evolution (i.e. mass, spin, metallicity, mass loss, and binary interaction). Massive stars are central objects to
Sergio
Simón Díaz