Results 11 to 20 of about 4,653,928 (371)
The Molecular Cloud Lifecycle. [PDF]
Space Sci Rev, 2020 Giant molecular clouds (GMCs) and their stellar offspring are the building blocks of galaxies. The physical characteristics of GMCs and their evolution are tightly connected to galaxy evolution.
Chevance M +8 more
europepmc +8 more sources
Compression and ablation of the photo-irradiated molecular cloud the Orion Bar. [PDF]
Nature, 2016 The Orion Bar is the archetypal edge-on molecular cloud surface illuminated by strong ultraviolet radiation from nearby massive stars. Our relative closeness to the Orion nebula (about 1,350 light years away from Earth) means that we can study the ...
Goicoechea JR +9 more
europepmc +3 more sources
[Cii] emission from L1630 in the Orion B molecular cloud. [PDF]
Astron Astrophys, 2017 CONTEXT L1630 in the Orion B molecular cloud, which includes the iconic Horsehead Nebula, illuminated by the star system σ Ori, is an example of a photodissociation region (PDR). In PDRs, stellar radiation impinges on the surface of dense material, often
Pabst CHM +13 more
europepmc +3 more sources
Molecular clouds in the Galaxy [PDF]
The Astrophysical Journal, 1975 The J = 1 → 0 emission of CO has been surveyed in the galactic plane between ℓ = -10° and +90° with a U beam sampling every degree. Molecular clouds emitting in the CO line are plentiful over the inner region of the Galaxy. Their greatest number occurs in the galactic nucleus and at a radius of 5.5 kpc—a distribution similar to radio H II regions and ...
N. Z. Scoville, P. M. Solomon
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Filament L1482 in the California molecular cloud [PDF]
, 2014 Aims. The process of gravitational fragmentation in the L1482 molecular filament of the California molecular cloud is studied by combining several complementary observations and physical estimates.
Dalei Li +6 more
semanticscholar +3 more sources
Evolving molecular cloud structure and the column density probability distribution function [PDF]
, 2014 The structure of molecular clouds can be characterized with the probability distribution function (PDF) of the mass surface density. In particular, the properties of the distribution can reveal the nature of the turbulence and star formation present ...
R. L. Ward, J. Wadsley, A. Sills
semanticscholar +4 more sources
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
semanticscholar +3 more sources
Biogenic, urban, and wildfire influences on the molecular composition of dissolved organic compounds in cloud water [PDF]
Atmospheric Chemistry and Physics, 2017 Organic aerosol formation and transformation occurs within aqueous aerosol and cloud droplets, yet little is known about the composition of high molecular weight organic compounds in cloud water.
R. D. Cook +19 more
doaj +2 more sources
Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites. [PDF]
Proc Natl Acad Sci U S A, 2016 Van Kooten EM +9 more
europepmc +2 more sources
Molecular Clouds in Spiral Galaxies [PDF]
Symposium - International Astronomical Union, 1983 A large observational program investigating the 2.6 mm CO line in spiral galaxies is being conducted by myself and Nick Scoville using the 14 m telescope of the Five College Radio Astronomy Observatory (HPBW = 50″). Thus far we have observed 46 galaxies of types Sa, Sb, Sc and Irr, detected 31, and mapped 16.
Judith S. Young
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