Bulge formation through disc instability — I. (arXiv:2011.11629v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Devergne_T/0/1/0/all/0/1">Timothée Devergne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cattaneo_A/0/1/0/all/0/1">Andrea Cattaneo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bournaud_F/0/1/0/all/0/1">Frédéric Bournaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koutsouridou_I/0/1/0/all/0/1">Ioanna Koutsouridou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winter_A/0/1/0/all/0/1">Audrey Winter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dimauro_P/0/1/0/all/0/1">Paola Dimauro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mamon_G/0/1/0/all/0/1">Gary A. Mamon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wacher_W/0/1/0/all/0/1">William Wacher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varin_M/0/1/0/all/0/1">Margot Varin</a>
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 S’ersic-exponential
surface-density distribution. The final $B/T$ is strongly related to the disc’s
fractional contribution $f_{rm d}$ to the total gravitational acceleration at
the optical radius. The formula $B/T=0.5,f_{rm }^{1.8}$ fits the simulations
to an accuracy of $30%$, is consistent with observational measurements of B/T
and f_d 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.
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 S’ersic-exponential
surface-density distribution. The final $B/T$ is strongly related to the disc’s
fractional contribution $f_{rm d}$ to the total gravitational acceleration at
the optical radius. The formula $B/T=0.5,f_{rm }^{1.8}$ fits the simulations
to an accuracy of $30%$, is consistent with observational measurements of B/T
and f_d 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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