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High Mass Star Formation

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Web pages of some of our collaborators
Images of star-forming regions
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Higher resolution Figure
(DSS, ESA/ESO/NASA)

Stars are formed within clouds of molecular gas (mostly molecular hydrogen) and dust. The densest parts of these clouds are very opaque to optical radiation. Therefore, we have to resort to infrared and radio wavelengths to study the youngest stellar objects. Many interesting phenomena take place before a star starts its life in the main sequence (the stage in which our Sun is right now): e.g., gravitational collapse, powerful mass-loss phenomena, or the birth of new planets.

In the Star Formation group at LAEFF, we study these processes related to star formation, as well as the environment in which they take place. Our main observational tool to carry out this research is Radio Astronomy.

There are two other groups at our laboratory whose research line is related to ours: pre-main-sequence stars and brown dwarfs.


The Star Formation Group at LAEFF

(NASA-JPL-MDSCC) (NOAO-KPNO)

 

News


 (NOAO/AURA/NSF)

Some links on Star Formation