The New Generation Planetary Population Synthesis (NGPPS). II. Planetary population of solar-like stars and overview of statistical results. (arXiv:2007.05562v2 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Emsenhuber_A/0/1/0/all/0/1">Alexandre Emsenhuber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mordasini_C/0/1/0/all/0/1">Christoph Mordasini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burn_R/0/1/0/all/0/1">Remo Burn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alibert_Y/0/1/0/all/0/1">Yann Alibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benz_W/0/1/0/all/0/1">Willy Benz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asphaug_E/0/1/0/all/0/1">Erik Asphaug</a>

We want to understand global observable consequences of different physical
processes and initial properties on the demographics of the planetary
population. We use the Generation III Bern model to perform planetary
population synthesis. We synthesise five populations with each a different
initial number of Moon-mass embryos per disc: 1, 10, 20, 50, and 100. The last
is our nominal population around 1 Sun-mass stars. The properties of giant
planets do not change much as long as there are at least 10 embryos in each
system. The study of giants can thus be done with simulations requiring less
computational resources. For inner terrestrial planets, only the 100-embryos
population is able to attain the giant-impact stage. In that population, each
planetary system contains on average 8 planets more massive than 1 $M_oplus$.
The fraction of systems with giants planets at all orbital distances is 18%,
but only 1.6% are at > 10 au. Systems with giants contain on average 1.6 such
planets. The frequency of terrestrial and super-Earth planets peaks at a
stellar [Fe/H] of -0.2 and 0.0, respectively, being limited at lower [Fe/H] by
a lack of building blocks, and by (for them) detrimental growth of more massive
dynamically active planets at higher [Fe/H]. The frequency of more massive
planets (Neptunian, giants) increases monotonically with [Fe/H]. The fast
migration of planets in the 5-50 $M_oplus$ range is reduced by the presence of
multiple lower-mass inner planets in the multi-embryos populations. We present
one of the most comprehensive simulations of (exo)planetary system formation
and evolution to date. For theory, they provide the framework to
observationally test the global statistical consequences of theoretical models
for specific physical processes. This is a important ingredient towards the
development of a standard model of planetary formation and evolution.

We want to understand global observable consequences of different physical
processes and initial properties on the demographics of the planetary
population. We use the Generation III Bern model to perform planetary
population synthesis. We synthesise five populations with each a different
initial number of Moon-mass embryos per disc: 1, 10, 20, 50, and 100. The last
is our nominal population around 1 Sun-mass stars. The properties of giant
planets do not change much as long as there are at least 10 embryos in each
system. The study of giants can thus be done with simulations requiring less
computational resources. For inner terrestrial planets, only the 100-embryos
population is able to attain the giant-impact stage. In that population, each
planetary system contains on average 8 planets more massive than 1 $M_oplus$.
The fraction of systems with giants planets at all orbital distances is 18%,
but only 1.6% are at > 10 au. Systems with giants contain on average 1.6 such
planets. The frequency of terrestrial and super-Earth planets peaks at a
stellar [Fe/H] of -0.2 and 0.0, respectively, being limited at lower [Fe/H] by
a lack of building blocks, and by (for them) detrimental growth of more massive
dynamically active planets at higher [Fe/H]. The frequency of more massive
planets (Neptunian, giants) increases monotonically with [Fe/H]. The fast
migration of planets in the 5-50 $M_oplus$ range is reduced by the presence of
multiple lower-mass inner planets in the multi-embryos populations. We present
one of the most comprehensive simulations of (exo)planetary system formation
and evolution to date. For theory, they provide the framework to
observationally test the global statistical consequences of theoretical models
for specific physical processes. This is a important ingredient towards the
development of a standard model of planetary formation and evolution.

http://arxiv.org/icons/sfx.gif