Results 31 to 40 of about 50 (50)
The local galaxy density and the bars of spiral galaxies
The Astrophysical Journal, 1993 23 pages, LaTeX, SISSA Ref.
GIURICIN G +3 more
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Stellar Populations in Spiral Galaxies [PDF]
Proceedings of the International Astronomical Union, 2006 We report preliminary results of the characterization of bulge and inner disk stellar populations for 8 nearby spiral galaxies using Gemini/GMOS. The long-slit spectra extend out to 1-2 disk scale lengths with S/N/Ang > 50. Two different model fitting techniques, absorption-line indices and full spectral synthesis, are found to weigh age ...
J. Jesús González +2 more
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SECULAR EVOLUTION OF SPIRAL GALAXIES [PDF]
Journal of The Korean Astronomical Society, 2003 15 pages, 8 figures, Invited talk presented at the 2nd APCTP workshop on Astrophysics, Pohang, Korea (June 2002)
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THE OPACITY OF SPIRAL GALAXY DISKS [PDF]
, 2007 The opacity of foreground spiral disks can be probed from the number of distant galaxies seen through them. To calibrate this number for effects other than the dust extinction, Gonzalez et al. (1998) developed the "Synthetic Field Method". A synthetic field is an extincted Hubble Deep Field added to the science field.
Holwerda, Benne W. +3 more
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Formation of Spiral Galaxies [PDF]
International Astronomical Union Colloquium, 1977 Conventionally, two major components of spiral galaxies are distinguished: (1) a “spheroidal component”, which includes the central bulge and the surrounding halo, and (2) a “disc component”, which is basically flat and circular but is often warped at the edges. Other structures, such as bars or rings, may also be present, but they are probably of less
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Outskirts of spiral galaxies [PDF]
Proceedings of the International Astronomical Union, 2016 AbstractI present an overview of the recent star formation activity in the outer disks of spiral galaxies, from the observational standpoint, with emphasis on the gas content, the star formation law, the metallicity and the stellar populations.
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, 2022 The most important theory of the spiral arms of galaxies is the density wave theory based on the Lin-Shu dispersion relation. However, the density waves move with the group velocity towards the inner Lindblad resonance and tend to disappear. Various mechanisms to replenish the spiral waves have been proposed.
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The Rotation of Spiral Galaxies [PDF]
Science, 1983 There is accumulating evidence that as much as 90 percent of the mass of the universe is nonluminous and is clumped, halo-like, around individual galaxies. The gravitational force of this dark matter is presumed to be responsible for the high rotational velocities of stars and gas in the disks of spiral galaxies.
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Nature, 1990 The photographic images of a carefully selected sample of about 16,000 galaxies have been digitized, and an extensive set of photometric parameters has been determined. These data allow a reanalysis of the effective transparency using the measured surface brightness profiles for much larger, more strictly defined samples. Several tests provide evidence
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Proceedings of the International Astronomical Union, 2019
AbstractThe venerable problem of what causes the spiral features in disk galaxies is nearing a solution. In previous work, we have shown that transient spirals in simulations result from the superposition of a few coherent waves that have many properties of modes.
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AbstractThe venerable problem of what causes the spiral features in disk galaxies is nearing a solution. In previous work, we have shown that transient spirals in simulations result from the superposition of a few coherent waves that have many properties of modes.
openaire +2 more sources