Early Evolution of Disk Galaxies: Formation of Bulges in Clumpy Young Galactic Disks

@article{Noguchi1999EarlyEO,
  title={Early Evolution of Disk Galaxies: Formation of Bulges in Clumpy Young Galactic Disks},
  author={Masafumi Noguchi},
  journal={The Astrophysical Journal},
  year={1999},
  volume={514},
  pages={77-95}
}
  • M. Noguchi
  • Published 26 June 1998
  • Physics
  • The Astrophysical Journal
A new idea is proposed for the origin of bulges in spiral galaxies. Numerical simulations of protogalactic collapse suggest strongly that galactic bulges have been assembled from massive clumps formed in galactic disks in their early evolutionary phase. These clumps result from the gravitational instability of the gas-rich disks of young galaxies. Owing to dynamical frictions, those massive clumps, individual masses of which can be as large as ~109 M?, are able to spiral toward the galactic… 

Tables from this paper

FORMATION OF LATE-TYPE SPIRAL GALAXIES: GAS RETURN FROM STELLAR POPULATIONS REGULATES DISK DESTRUCTION AND BULGE GROWTH
Spiral galaxies have most of their stellar mass in a large rotating disk, and only a modest fraction in a central spheroidal bulge. This challenges present models of galaxy formation: galaxies form
Rapid Formation of Exponential Disks and Bulges at High Redshift from the Dynamical Evolution of Clump-Cluster and Chain Galaxies
Many galaxies at high redshift have peculiar morphologies dominated by 108-109 M☉ kpc-sized clumps. Using numerical simulations, we show that these "clump clusters" can result from fragmentation in
UNSTABLE DISKS AT HIGH REDSHIFT: EVIDENCE FOR SMOOTH ACCRETION IN GALAXY FORMATION
Galaxies above redshift 1 can be very clumpy, with irregular morphologies dominated by star complexes as large as 2 kpc and as massive as a few ×108 or 109 M ☉. Their co-moving densities and rapid
Bulge formation in disk galaxies with MOND
The formation of galaxies and their various components can be stringent tests of dark matter models and of gravity theories. In the standard cold dark matter (CDM) model, spheroids are formed through
Formation of Massive Galaxies at High Redshift: Cold Streams, Clumpy Disks, and Compact Spheroids
We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal
Stellar feedback and bulge formation in clumpy discs
We use numerical simulations of isolated galaxies to study the effects of stellar feedback on the formation and evolution of giant star-forming gas ‘clumps’ in high-redshift, gas-rich galaxies. Such
Bulge Growth Through Disc Instabilities in High-Redshift Galaxies
The role of disc instabilities, such as bars and spiral arms, and the associated resonances, in growing bulges in the inner regions of disc galaxies have long been studied in the low-redshift nearby
Secular evolution of late-type disc galaxies: formation of bulges and the origin of bar dichotomy
Origins of galactic bulges and bars remain elusive, although they constitute fundamental components of disc galaxies. This paper proposes that the secular evolution process driven by the interstellar
THE LONG LIVES OF GIANT CLUMPS AND THE BIRTH OF OUTFLOWS IN GAS-RICH GALAXIES AT HIGH REDSHIFT
Star-forming disk galaxies at high redshift are often subject to violent disk instability, characterized by giant clumps whose fate is yet to be understood. The main question is whether the clumps
Gas physics, disk fragmentation, and bulge formation in young galaxies
We investigate the evolution of star-forming gas-rich disks, using a 3D chemodynamical model including a dark halo, stars, and a two-phase interstellar medium with feedback processes from the stars.
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 89 REFERENCES
Clumpy star-forming regions as the origin of the peculiar morphology of high-redshift galaxies
Many high-redshift galaxies have peculiar morphologies and photometric properties. It is not clear whether these peculiarities originate in galaxy–galaxy interactions (or mergers) or are intrinsic to
The formation of disc galaxies in a cosmological context: structure and kinematics
We present results concerning the internal structure and kinematics of disk galaxies formed in cosmologically motivated simulations. The calculations include dark matter, gas dynamics, radiative
THE FORMATION OF DISK GALAXIES
We present a scenario for the formation of disks that explains not only the properties of normal galaxies but also the properties of the population of low surface brightness galaxies (LSBs) as well.
The origin of the mass, disk-to-halo mass ratio, and L-V relation of spiral galaxies
A model is presented in which spiral galaxies only form when t(c) is roughly equal to t(f) in a hot component of the protogalactic gas. This assumption, along with a disk stability criterion,
Effects of gas on the global stability of galactic disks - Radial flows
We study numerically the effect of gas on the global stability of a two-component self-gravitating galactic disk embedded in a live halo. The stars are evolved by using a 3D collisionless N-body
Simulations of dissipative galaxy formation in hierarchically clustering universes – II. Dynamics of the baryonic component in galactic haloes
We present self-consistent 3D simulations of the formation of virialized systems containing both gas and dark matter. Using a fully Lagrangian code based on the smooth particle hydrodynamics
Chemical evolution of the galactic disk with radial gas flows.
We present a series of models for the chemical evolution of the galactic disk with radial inflows of the gas at a velocity that is constant in time but may vary with galactocentric radius. The models
Nuclei of nearby disk galaxies .1. A Hubble Space Telescope imaging survey
We present deconvolved images of the central regions of 20 nearby disk galaxies, obtained with the original Planetary Camera of the Hubble Space Telescope. The galaxies span a range in Hubble type
The morphological identification of the rapidly evolving population of faint galaxies
The excess numbers of blue galaxies at faint magnitudes are a long-standing cosmological puzzle. We present new number-magnitude counts as a function of galactic morphology from the first deep fields
Spiral Galaxies with WFPC2. II. The Nuclear Properties of 40 Objects
We report the analysis of Hubble Space Telescope Wide Field Planetary Camera 2 F606W images of 40 spiral galaxies belonging to the sample introduced in Paper I, where 35 other targets were discussed.
...
1
2
3
4
5
...