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diffuse nebula


  • WordNet 3.6
    • n diffuse nebula a cluster of stars within an intricate cloud of gas and dust
    • ***


In literature:

Can we learn whether the luminous matter in such nebulae is more diffused or less diffused, than that of the comet of Encke?
"The Plurality of Worlds" by William Whewell

In poetry:

Light over the laminae of roofs,
Diffusing in shimmering nebulae
About the night's boundaries,
Or billowing in pearly foam
Submerging the low-lying stars…
"Broadway" by Lola Ridge

In science:

In the X-rays, the nebula is composed of a compact nebula of ∼ 1′ and the diffuse nebula with the radius of ∼ 5′ (Safi-Harb et al. 1995).
Gamma-rays from the pulsar wind nebulae
In Table 15 we compare our Orion nebula gas+dust abundances –corrected for depletion onto dust grains– with those of the Sun, young F−G disk stars (ages 62 Gyr), nearby B dwarfs and gas-phase abundances of the local diffuse clouds.
A reappraisal of the chemical composition of the Orion nebula based on VLT echelle spectrophotometry
We have compared the chemical composition of the nebula with that of the Sun and other representative ob jects, as the neutral diffuse ISM, young F and G stars and B dwarfs of the solar vicinity.
A reappraisal of the chemical composition of the Orion nebula based on VLT echelle spectrophotometry
Study of the diffuse band carriers in localised astrophysical environments such as stars and nebulae offers the potential to investigate their spectroscopic transitions under different excitation conditions and potentially to learn something of their formation mechanism.
The Diffuse Interstellar Bands: A Major Problem in Astronomical Spectroscopy
The Red Rectangle displays the UIR bands strongly from both the central star and the nebula and this has led to the idea that PAHs are responsible for the unidentified optical emission bands including those close in wavelength to some diffuse bands.
The Diffuse Interstellar Bands: A Major Problem in Astronomical Spectroscopy
Hubble Space Telescope (HST) images at optical wavelengths and recent Spitzer Space Telescope (Spitzer) images at 3.6–8 µm have resolved the Helix Nebula into thousands of “cometary knots” immersed in diffuse gas, producing strikingly beautiful and well-publicized images (O’Dell et al. 2004; Hora et al. 2006).
A Debris Disk around the Central Star of the Helix Nebula?
The He II image of the Helix Nebula shows a central diffuse emission region similar to that seen at 24 µm, but not a point-like central source.
A Debris Disk around the Central Star of the Helix Nebula?
More extended (∼ 10’s of pc) diffuse X-ray emission traces abundance variations and either shows a large-scale variation in iron abundance across the nebula much larger than the Galactic gradient, possibly indicative of a supernova explosion.
Eta Car and Its Surroundings: the X-ray Diagnosis
We derive bounds of 1013 –10 15 cm on the droplet sizes inside H  regions in order that (1) they should not have already been detected by direct imaging of nearby nebulae, and (2) they should not be too swiftly destroyed by diffusion in the ionized gas.
Enrichment of the ISM by metal-rich droplets and the abundance bias in HII regions
TTs with discs observed in silhouette (i.e., in absorption) against the diffuse background emission in the Orion nebula, and are typically surrounded by characteristic cometary-shaped nebulae (O’Dell et al., 1993; McCaughrean & O’Dell, 1996).
From discs to planetesimals I: evolution of gas and dust discs
Rapid formation of Jupiter by diffuse redistribution of water vapor in the solar nebula.
Forming Planetesimals in Solar and Extrasolar Nebulae
The nebula consists of high gas density knots embedded in a diffuse body.
A pilot study of the radio-continuum emission from MASH planetary nebulae
Thus, for example, in a photoionized H II region such as the great diffuse nebula in Orion, stellar ionizing flux is effectively shielded by Helium to prevent extensive ionization of Fe ions beyond Fe IV.
Atomic data from the Iron Project.LVIII. New radiative transition probabilities for Fe IV including fine structure
The “head” of the nebula is coincident with the radio position of the pulsar, while diffuse emission is seen predominantly to the SE.
Chandra and XMM-Newton Observations of the Vela-like Pulsar B1046-58
The observations thus point to the presence of another component of cold plasma, previously unknown, embedded in the diffuse nebula.
Elemental abundances of Galactic bulge planetary nebulae from optical recombination lines