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- H II region - Wikipedia
An H II region is a region of interstellar atomic hydrogen that is ionized [1] It is typically in a molecular cloud of partially ionized gas in which star formation has recently taken place, with a size ranging from one to hundreds of light years, and density from a few to about a million particles per cubic centimetre
- What Is an H II Region? - CosmoBC AstroBlog
H II regions (also spelled as HII regions), formally known as ionized atomic hydrogen regions, represent distinct cosmic zones characterized by the prevalence of ionized atomic hydrogen (H II)
- HII Region Basics - Harvard University
In this module, we’ll go through a simplified mathematical formulation for the dynamical evolution of a pure hydrogen HII region Our framework won’t explain the intricate features observed in images, but it will give us an idea of the basic underlying physics
- HII Regions - Astronomy Online
HII regions are remarkably tightly correlated with the spiral and ring like structures in the galaxies The red filter is more sensitive to the general distribution of old stars, while the H a filter highlights the sites of young stars in star forming regions
- The Cosmic Crucibles: H II Regions in Stellar Evolution
H II regions are vast, interstellar clouds of ionized gas that play a pivotal role in the evolution of galaxies and the formation of stars These cosmic crucibles are the birthplaces of new stars and planetary systems, shaping the universe as we know it
- H II region | Astronomy, Star Formation Nebulae | Britannica
H II region, interstellar matter consisting of ionized hydrogen atoms The energy that is responsible for ionizing and heating the hydrogen in an emission nebula comes from a central star that has a surface temperature in excess of 20,000 K
- The Optical Depth of H II Regions in the Magellanic Clouds
We exploit ionization-parameter mapping as a powerful tool to measure the optical depth of star-forming HII regions Our simulations using the photoionization code CLOUDY and our new, SURFBRIGHT surface brightness simulator demonstrate that this technique can directly diagnose most density-bounded, optically thin nebulae using spatially
- THE STRUCTURE AND EVOLUTION OF EARLY COSMOLOGICAL H ii REGIONS - IOPscience
pe fraction is achieved for different masses and redshifts In the present paper, we study the evolution of H ii regions around Population III stars for a wide range of halo mass, redshift, and gas density profile Specifically, we consider an ‘‘inside-out’’ situation, where the central source ionizes t
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