1987
DOI: 10.1086/165480
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Angular momentum from tidal torques

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Cited by 543 publications
(588 citation statements)
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“…The median and dispersion (in ln j) are found to j med p j depend remarkably weakly on the cosmology, halo mass, or initial spectrum of density Ñuctuations (e.g., Barnes & Efstathiou 1987 ;Warren et al 1992 ;Cole & Lacey 1996), with typical values and j med B 0.04 p j B 0.5È0.6. With some simplifying assumptions, we can now relate the halo parameters in deÐnition (4) to the disk radius and luminosity.…”
Section: Derivation Of Functional Formmentioning
confidence: 95%
See 1 more Smart Citation
“…The median and dispersion (in ln j) are found to j med p j depend remarkably weakly on the cosmology, halo mass, or initial spectrum of density Ñuctuations (e.g., Barnes & Efstathiou 1987 ;Warren et al 1992 ;Cole & Lacey 1996), with typical values and j med B 0.04 p j B 0.5È0.6. With some simplifying assumptions, we can now relate the halo parameters in deÐnition (4) to the disk radius and luminosity.…”
Section: Derivation Of Functional Formmentioning
confidence: 95%
“…N-body simulations (e.g., Barnes & Efstathiou 1987 ;Warren et al 1992) show that the distribution of j values of DM halos acquired from tidal torques in hierarchical clustering cosmologies can be well be approximated by a log-normal distribution…”
Section: Derivation Of Functional Formmentioning
confidence: 99%
“…The required halo angular momentum is very large, however. If all of the halo angular momentum arises from tidal torques in the early universe, the required value of j would be reached only rarely (Barnes & Efstathiou 1987 ;Steinmetz & Bartelmann 1995). Since of Z50% all high surface brightness (HSB) disks contain strong bars (Eskridge et al 2000), the vast majority cannot have j large enough to avoid bar slowdown.…”
Section: Implications For Barred Galaxiesmentioning
confidence: 99%
“…η is related to the ratio of the rotational to gravitational energy of the cloud core, β = Erot/|Eg|, with β = 0.9η. Finally, β relates to the so-called "spin parameter," λ = √ β, that is most often used to characterize the angular momentum of dark matter halos (and their associated gas) formed from cosmological initial conditions (e.g., Barnes & Efstathiou 1987;Ryden 1988 Each model is run on a polar coordinate grid with 512 × 512 spatial grid zones in r and φ. The inner and outer boundary conditions allow for free outflow from the computational domain.…”
Section: Initial Conditionsmentioning
confidence: 99%