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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2020

Bulge formation through disc instability

Résumé

We use simulations to study the growth of a pseudobulge in an isolated thin exponential stellar disc embedded in a static spherical halo. We observe a transition from later to earlier morphological types and an increase in bar prominence for higher disc-to-halo mass ratios, for lower disc-to-halo size ratios, and for lower halo concentrations. We compute bulge-to-total stellar mass ratios B/T by fitting a two-component Sérsic-exponential surface-density distribution. The final B/T is strongly related to the disc’s fractional contribution fd to the total gravitational acceleration at the optical radius. The formula B/T = 0.5 fd1.8 fits the simulations to an accuracy of 30%, is consistent with observational measurements of B/T and fd as a function of luminosity, and reproduces the observed relation between B/T and stellar mass when incorporated into the GALICS 2.0 semi-analytic model of galaxy formation.
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Dates et versions

hal-03037163 , version 1 (03-12-2020)

Identifiants

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T. Devergne, A. Cattaneo, F. Bournaud, I. Koutsouridou, A. Winter, et al.. Bulge formation through disc instability: I. Stellar discs. Astronomy and Astrophysics - A&A, 2020, 644, pp.A56. ⟨10.1051/0004-6361/201936439⟩. ⟨hal-03037163⟩
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