Impact Of Magnetic Fields On Molecular Cloud Formation & Evolution [PDF]
, 2015 We use magnetohydrodynamical simulations of converging flows to investigate the process of molecular cloud formation and evolution out of the magnetised ISM.
B. Kortgen, R. Banerjee
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Chemistry of Molecular Clouds [PDF]
International Astronomical Union Colloquium, 1989 AbstractA discussion is presented of the chemistry of quiescent molecular clouds, and the effects of the presence of polycyclic aromatic hydrocarbon molecules and of cosmic-ray induced ultraviolet photons are examined. A comparison is made with the chemistry occurring in molecular clouds that are subjected to shocks and the differences between ...
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Cloud-cloud Collision in the Galactic Center 50 km s$^{-1}$ Molecular Cloud [PDF]
, 2015 We performed a search of star-forming sites influenced by external factors, such as SNRs, HII regions, and cloud-cloud collisions, to understand the star-forming activity in the Galactic center region using the NRO Galactic Center Survey in SiO $v=0, J=2-
M. Tsuboi, A. Miyazaki, K. Uehara
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SUPERNOVA DRIVING. I. THE ORIGIN OF MOLECULAR CLOUD TURBULENCE [PDF]
, 2015 Turbulence is ubiquitous in molecular clouds (MCs), but its origin is still unclear because MCs are usually assumed to live longer than the turbulence dissipation time.
P. Padoan +3 more
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‘The Brick’ is not abrick: a comprehensive study of the structure and dynamics of the central molecular zone cloud G0.253+0.016 [PDF]
Monthly notices of the Royal Astronomical Society, 2019 In this paper we provide a comprehensive description of the internal dynamics of G0.253+0.016 (a.k.a. 'the Brick'); one of the most massive and dense molecular clouds in the Galaxy to lack signatures of widespread star formation. As a potential host to a
J. Henshaw +22 more
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Molecular Abundances in the Sgr a Molecular Cloud [PDF]
Symposium - International Astronomical Union, 1992 We have obtained column densities for HCO+, HCO, HCS+, C3H2, HC5N, SiO, OCS, HCOOH, CH3CH2 OH, and CH3CCH toward Sgr A. The fractional abundance of SiO relative to molecular hydrogen in Sgr A is comparable to that for the Orion plateau, ~ 10−7 − 10−8, which may be a typical value for hot clouds.
Yc Minh, William M. Irvine, Per Friberg
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SUBMILLIMETER POLARIZATION SPECTRUM IN THE VELA C MOLECULAR CLOUD [PDF]
, 2015 Polarization maps of the Vela C molecular cloud were obtained at 250, 350, and 500 μm during the 2012 flight of the balloon-borne telescope BLASTPol.
N. Gandilo +29 more
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Cloud-scale Molecular Gas Properties in 15 Nearby Galaxies [PDF]
Astrophysical Journal, 2018 We measure the velocity dispersion, σ, and surface density, Σ, of the molecular gas in nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to the size of individual giant molecular clouds. Combining 11 galaxies from the
Jiayi Sun +21 more
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Statistical study of dust properties in LMC molecular clouds [PDF]
, 2010 The objective of this paper is to construct a catalog providing the dust properties and the star formation efficiency (SFE) of the molecular clouds in the Large Magellanic Cloud (LMC).
Akiko Kawamura +36 more
core +2 more sources
CARMA LARGE AREA STAR FORMATION SURVEY: OBSERVATIONAL ANALYSIS OF FILAMENTS IN THE SERPENS SOUTH MOLECULAR CLOUD [PDF]
, 2014 We present the N2H+ (J = 1 → 0) map of the Serpens South molecular cloud obtained as part of the CARMA Large Area Star Formation Survey. The observations cover 250 arcmin2 and fully sample structures from 3000 AU to 3 pc with a velocity resolution of 0 ...
M. Fernández-López +22 more
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