Massive star-formation regions in the Magellanic Clouds

Journal Article · Mon Aug 01 00:00:00 EDT 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/166553· OSTI ID:6753236

Hutchings, J B; Thompson, I B

Optical and UV spectroscopy of stars from six compact, luminous groups or clusters in the SMC and LMC is presented. The groups are characterized by high concentrations of nebulosity or starlight confined to areas smaller than 30 arcsec on a side, in which some stars can be resolved. The spectra and fluxes are used to derive luminosities and effective temperatures for the stars. Spectroscopic and stellar wind properties are also noted. It is found that the stars are all of O and B-type, with low extinction. The stars generally have little or no sign of stellar winds, and often have spectral peculiarities, such as weak lines or mixed spectral indicators. Most spectra have strong, broad Ly-alpha absorption, and some have broad Ca II absorption. The stars are placed on the H-R diagram, and it is argued that some of them are massive stars in pre-main-sequence stages of their evolution. 8 references.

• Research Organization: Dominion Astrophysical Observatory, Victoria (Canada); Mount Wilson and Las Campanas Observatories, Pasadena, CA (USA)
• OSTI ID: 6753236
• Journal Information: Astrophys. J.; (United States), Vol. 331
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
MAGELLANIC CLOUDS
STAR EVOLUTION
HERTZSPRUNG-RUSSELL DIAGRAM
LUMINOSITY
MASS
STAR CLUSTERS
STELLAR WINDS
ULTRAVIOLET SPECTRA
VISIBLE SPECTRA
DIAGRAMS
GALAXIES
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
SPECTRA
STELLAR ACTIVITY
640105* - Astrophysics & Cosmology- Galaxies