Galactic disks, infall, and the global value of Omega

Tóth, Gábor Fejes; Ostriker, Jeremiah P.

doi:10.1086/171185

Cited by 383 publications

(350 citation statements)

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“…The Tully-Fisher relation applies to a particular morphological class of galaxies, and so one may argue that galaxies which have undergone major mergers since the formation of their stellar disks would not appear as thin spiral galaxies today (T oth & Ostriker 1992). This morphological restriction on merger histories ought to yield a smaller value of = , but because the epoch of star formation is unknown, it cannot be incorporated in a simple way.…”

Section: Discussionmentioning

confidence: 99%

“…At rst glance, it seems unlikely that both the baryonic mass and the velocity dispersion of the halo would remain unchanged as the growth factor increases by a signi cant factor and the corresponding accretion occurs. However, detailed consideration of these conditions raises di cult questions concerning the maximum mass of galaxies (Thoul & Weinberg 1995), the accretion of satellite galaxies (T oth & Ostriker 1992;Navarro, Frenk, & White 1994), and the fate of dark matter cores as they fall into larger objects (Moore, Katz, & Lake 1995). It is important to note that galaxy-sized halos in the universe at z = 0 do not correspond to rare density peaks.…”

Section: Discussionmentioning

confidence: 99%

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Can the Tully-Fisher Relation Be the Result of Initial Conditions?

Eisenstein

Loeb

1997

Galaxy Scaling Relations: Origins, Evolution and Applications

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Can the Tully-Fisher Relation Be the Result of Initial Conditions?

Eisenstein

Loeb

1997

Galaxy Scaling Relations: Origins, Evolution and Applications

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“…The majority of the external gas cannot come from companions, since galaxy interactions heat the disks (Toth & Ostriker 1992). What is required instead is a source of continuous cold gas accretion from the filaments in the near environment of galaxies.…”

Section: Bar Frequency and Gas Accretionmentioning

confidence: 99%

Secular Evolution of Galaxies

Falcón-Barroso¹,

Knapen²

2013

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Abstract. New observations in favour of a significant role of secular evolution are reviewed: central star formation boosted in pseudo-bulge barred galaxies, relations between bulge and disk, evidence for rejuvenated bulges. Numerical simulations have shown that secular evolution can occur through a cycle of bar formation and destruction, in which the gas plays a major role. Since bars are weakened or destroyed in gaseous disks, the high frequency of bars observed today requires external cold gas accretion, to replenish the disk and allow a new bar formation. The rate of gas accretion from external filaments is compatible with what is observed in cosmological simulations.Keywords. galaxies: general, galaxies: spiral, galaxies: bulges, galaxies: evolution, galaxies: formation, galaxies: starburst, galaxies: structure Role of secular evolutionSecular evolution is one of the three scenarios for galaxy formation and evolution. In a first one, monolithic collapse, gas clouds in free fall form stars so quickly that the resulting system is ellipsoidal. Disks then form afterward, through gas accretion around these bulges. In a second scenario, hierarchical formation, gas clouds have time to settle in rotating disks through dissipation, and form stars in thin spiral disks, which after several minor mergers, or a major merger, can also result in an ellipsoidal system. The secular evolution scenario also considers that spiral disks form first, then non-axisymmetric waves (bars and spirals) with their associated gravity torques and resonances, drive internal evolution, and in particular mass concentration towards the centre, and formation of bulges from the stellar disk. Spiral disks are continuously replenished through external gas accretion.

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“…• Its coldness has been used to constrain the amount of recent merger events (Toth & Ostriker 1992). Small dark satellites, which are so abundant in CDM simulations (Springel et al 2008), do not induce much heating (Font et al 2001), but mergers of 10-20% mass ratio can significantly increase the velocity dispersion of the stars.…”

Section: Dynamics Of the Disk(s)mentioning

confidence: 99%