2011/01/28 by M. H. D. van der Wiel, F. F. S. van der Tak, M. Spaans +4 · 11 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Circumstellar disk #Circumstellar envelope #Envelope (radar) #Molecular cloud #Protostar #Star formation #Stars #Stellar evolution #astro-ph.GA
paper · pdf · doi:10.1051/0004-6361/201016086
published in Astronomy and Astrophysics 532, A88 (EDP Sciences) · 17 pages; accepted for publication in A&A
arxiv created 2011/01/28 · openalex publication_date 2011/02/15 · arxiv updated 2015/03/18 · openalex created_date 2021/02/01 · openalex updated_date 2026/08/05
Context. The understanding of the formation process of massive stars ( ≳ 8 M⊙) is limited by a combination of theoretical complications and observational challenges. The high UV luminosities of massive stars give rise to chemical complexity in their natal molecular clouds and affect the dynamical properties of their circumstellar envelopes.