Star formation in the spiral arms of NGC 4321. I - CO observations

1992 ◽  
Vol 103 ◽  
pp. 429 ◽  
Author(s):  
J. Cepa ◽  
J. E. Beckman ◽  
J. H. Knapen ◽  
N. Nakai ◽  
N. Kuno
Keyword(s):  
Star Formation ◽  
Spiral Arms ◽  
Co Observations

scholarly journals The Galactic Ecosystem

2004 ◽  
Vol 213 ◽  
pp. 123-126
Author(s):  
Michael Burton
Keyword(s):  
Star Formation ◽  
Crucial Role ◽  
Self Regulation ◽  
Spiral Arms ◽  
Carbon Abundance

We discuss how the process of star formation across the spiral arms of galaxies functions as an ecosystem. The carbon abundance plays a crucial role in both its self-regulation and evolution.

scholarly journals [CII] emission and star formation in the spiral arms of M 31

2006 ◽  
Vol 453 (1) ◽  
pp. 77-82 ◽  
Author(s):  
N. J. Rodriguez-Fernandez ◽  
J. Braine ◽  
N. Brouillet ◽  
F. Combes
Keyword(s):  
Star Formation ◽  
Spiral Arms ◽  
M 31

scholarly journals Cloud and Star Formation in Spiral Arms

2014 ◽  
pp. 147-156
Author(s):  
Clare Dobbs ◽  
Alex Pettitt
Keyword(s):  
Star Formation ◽  
Spiral Arms

scholarly journals Large Scale Star Formation: Density Waves, Superassociations and Propagation

1987 ◽  
Vol 115 ◽  
pp. 457-481 ◽  
Author(s):  
Bruce G. Elmegreen
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Density Waves ◽  
Spiral Arms ◽  
Gravitational Instabilities ◽  
Significant Difference ◽  
Star Formation In Galaxies ◽  
The Difference ◽  
The Waves

The hypothesis that density waves trigger star formation is critically examined. Much of the former evidence in favor of the hypothesis is shown to be inconsistent with modern observations. A comparison between galaxies with and without density waves reveals no significant difference in their star formation rates. A new role for density waves in the context of star formation might be based on four principles: 1. density waves are intrinsically strong, 2. the gas is compressed more than the stars in the wave, 3. star formation follows the gas, with no preferential trigger related to the wave itself, and 4. regions of star formation are larger in the spiral arms than they are between the arms. This new role for density waves is primarily one of organization: the waves place most of the gas in the arms, so most of the star formation is in the arms too. The waves also promote the coagulation of small clouds into large cloud complexes, or superclouds, by what appears to be a combination of collisional agglomeration and large-scale gravitational instabilities. Special regions where density waves do trigger a true excess of star formation are discussed, and possible reasons for the difference between these triggering waves and the more common, organizing, waves are mentioned. Other aspects of large-scale star formation, such as the occurrence of kiloparsec-size regions of activity and kiloparsec-range propagation, are illustrated with numerous examples. The importance of these largest scales to the overall mechanism of star formation in galaxies is emphasized.

scholarly journals The Evolution of Giant Molecular Clouds

1980 ◽  
Vol 87 ◽  
pp. 137-149 ◽  
Author(s):  
Colin Norman ◽  
Joseph Silk
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Molecular Clouds ◽  
Supernova Remnants ◽  
Density Wave ◽  
Collective Effects ◽  
Giant Molecular Clouds ◽  
Spiral Density Wave ◽  
External Galaxies ◽  
Co Observations

We discuss the origin, lifetime, destruction, spatial distribution and relation to star formation of giant molecular clouds. A coagulation model including the effects of spiral density wave shocks is described. We explore implications for CO observations of external galaxies. The collective effects of OB star winds and supernova remnants in disrupting clouds are considered.

scholarly journals Supplying Gas for Nuclear Star Formation: The Central Molecular Spiral of IC 342

1994 ◽  
Vol 140 ◽  
pp. 339-340 ◽  
Author(s):  
D. A. Levine ◽  
J. L. Turner ◽  
R. L. Hurt
Keyword(s):  
Star Formation ◽  
Spiral Galaxy ◽  
Density Wave ◽  
Wave Pattern ◽  
Molecular Gas ◽  
Spiral Arms

IC 342 is a large nearby (1.8Mpc) spiral galaxy undergoing a moderate nuclear starburst. Previous maps of the inner arc minute in 13CO (1→0) show that the nuclear molecular gas forms spiral arms approximately 500 pc in extent in a density wave pattern (Turner & Hurt, 1992).

Efficient star formation in the spiral arms of M51

1990 ◽  
Vol 356 ◽  
pp. 135 ◽  
Author(s):  
Steven D. Lord ◽  
Judith S. Young
Keyword(s):  
Star Formation ◽  
Spiral Arms

scholarly journals Constraining star formation timescales with molecular gas and young star clusters

2019 ◽  
Vol 15 (S352) ◽  
pp. 350-352
Author(s):  
Kathryn Grasha ◽  
Daniela Calzetti
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Star Clusters ◽  
Young Star ◽  
Molecular Gas ◽  
Gas Reservoirs ◽  
Multi Wavelength ◽  
Predictive Theory ◽  
Young Star Clusters ◽  
Co Observations

AbstractStar formation provides insight into the physical processes that govern the transformation of gas into stars. A key missing piece in a predictive theory of star formation is the link between scales of individual stars and star clusters up to entire galaxies. LEGUS is now providing the information to test the overall organization and spatial evolution of star formation. We present our latest findings of using star clusters from LEGUS combined with ALMA CO observations to investigate the transition from molecular gas to star formation in local galaxies. This work paves the way for future JWST observations of the embedded phase of star formation, the last missing ingredient to connect young star clusters and their relation with gas reservoirs. Multi-wavelength studies of local galaxies and their stellar and gas components will help shed light on early phases of galaxy evolution and properties of the ISM at high-z.

Star formation in galactic spiral arms

Nature ◽  
1982 ◽  
Vol 297 (5863) ◽  
pp. 179-180
Author(s):  
Gerard Gilmore
Keyword(s):  
Star Formation ◽  
Spiral Arms ◽  
Galactic Spiral
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