Gas and dust in the star-forming regionρOph A

2017/09/01 by Bengt Larsson, R. Liseau, Rene Liseau · 18 citations
Chemistry · Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Atomic physics #Chemical physics #Chemistry #Core (optical fiber) #Geometry #Hydrogen #Hyperfine structure #Line (geometry) #Molecular Spectroscopy and Structure #Outflow #Physics #Radiative transfer #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR

paper · pdf · doi:10.1051/0004-6361/201731466

published in Astronomy and Astrophysics 608, A133 (EDP Sciences) · accepted for publication in Astronomy & Astrophysics (25/08/2017) 20 pages, 17 figures

arxiv created 2017/09/01 · openalex publication_date 2017/09/05 · arxiv updated 2017/12/20 · openalex created_date 2022/10/01 · openalex updated_date 2026/07/31

Abstract

Context. The evolution of interstellar clouds of gas and dust establishes the prerequisites for star formation. The pathway to the formation of stars can be studied in regions that have formed stars, but which at the same time also display the earliest phases of stellar evolution, i.e. pre-collapse/collapsing cores (Class -1), protostars (Class 0), and young stellar objects (Class I, II, III).

Citations

• Odin observations of H2O in the Galactic Centre
• Molecular oxygen in the ρ Ophiuchi cloud
• Circumstellar water vapour in M-type AGB stars: radiative transfer models, abundances, and predictions for HIFI
• ISOCAM observations of the ρ Ophiuchi cloud: Luminosity and mass functions of the pre-main sequence embedded cluster
• The Chemical Composition of the Sun