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The growth of planets by pebble accretion in evolving protoplanetary discs
The formation of planets depends on the underlying protoplanetary disc structure, which in turn influences both the accretion and migration rates of embedded planets. The disc itself evolves on time
The structure of protoplanetary discs around evolving young stars
The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles,
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants
The growth of a planetary core by pebble accretion stops at the so-called pebble isolation mass, when the core generates a pressure bump that traps drifting pebbles outside its orbit. The value of
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores
The basic structure of the Solar System is set by the presence of low-mass terrestrial planets in its inner part and giant planets in its outer part. This is the result of the formation of a system
Stellar irradiated discs and implications on migration of embedded planets. I. Equilibrium discs
The strength and direction of migration of low mass planets depends on the disc's thermodynamics. In discs where the viscous heating is balanced by radiative transport, the migration can be directed
Orbital evolution of eccentric planets in radiative discs
Context. With an average eccentricity of about 0.29, the eccentricity distribution of extrasolar planets is markedly different from the solar system. Among other scenarios considered, it has been
Fossilized condensation lines in the Solar System protoplanetary disk
The terrestrial planets and the asteroids dominant in the inner asteroid belt are water poor. However, in the protoplan-etary disk the temperature should have decreased below water-condensation level
Stellar irradiated discs and implications on migration of embedded planets - II. Accreting-discs
The strength and direction of migration of embedded low mass planets depends on the disc's structure. It has been shown that, in discs with viscous heating and radiative transport, the migration can
Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains
'Hot super-Earths' (or 'mini-Neptunes') between one and four times Earth's size with period shorter than 100 d orbit 30-50 per cent of Sun-like stars. Their orbital configuration - measured as the
Highly inclined and eccentric massive planets - I. Planet-disc interactions
In the Solar System, planets have a small inclination with respect to the equatorial plane of the Sun, but there is evidence that in extrasolar systems the inclination can be very high. This
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