Osservatorio Astrofisico di Arcetri

Informazioni sul Premio

Premio per tesi di Laurea Magistrale "Stefano Magini" - DD88/2018


Nomina commissione

Approvazione degli atti


Vincitori 2018

Curriculum Vitae Marco Cilibrasi
Titolo della tesi di Laurea: A semi-analytical model for the formation of Jupiter’s satellites in circumplanetary disks
Abstract: The satellites of Jupiter are thought to form in a circumplanetary disc (CPD), i.e. a small disc forming around a giant planet when a gap is opened in the protoplanetary disc. We study the forma- tion and orbital evolution of moons with a population synthesis approach, by varying the dust-to-gas ratio, the disc dispersal timescale and the dust refilling timescale in such a disc. The CPD initial conditions (density and temperature) are directly drawn from the results of 3D radiative hydrody- namical simulations. The disc evolution is taken into account within the population synthesis, and the satellitesimals were assumed to initially grow via streaming instability, then via dust accretion, while they migrate through the disc.
We find that the moons form fast, often within 104 years, due to the short orbital timescales in the disc. They form in sequence, and many are lost into the planet due to fast type I migration, polluting Jupiter’s envelope with typically 15 Earth-masses of metals. The last generation of surviving moons can form very late in the evolution of the giant planet when the disc has already lost more than 99% of its mass. The late circumplanetary disc is cold enough to sustain water ice, hence not surprisingly 85% of the moon population has icy composition. The distribution of the satellite-masses is peaking slightly above Galilean masses, up until a few Earth-masses, in a regime which is observable with the current instrumentation around Jupiter-analog exoplanets orbiting sufficiently close to their host stars.

Curriculum Vitae
Antonio Pensabene
Titolo della tesi di Laurea The ALMA view of the high redshift relation between supermassive black holes and their host galaxies
Abstract:  The existence of tight correlations between supermassive black holes (BHs) and their host galaxies properties in the local Universe suggests a closely linked evolution. Investigating these relations up to the high redshifts (z > 6) is thus crucial to understand the interplay between star-formation and BH growth across the cosmic time and to set constraints on galaxy formation and evolution models. In this work, I present the relation between black hole mass (MBH) and the host galaxy dynamical mass (Mgal) for a sample of 10 high-z (z ~ 2 – 7) quasars for which we have obtained measurements of the host galaxy kinematics from archival data of the Atacama Large (Sub-)Millimeter Array (ALMA). Thanks to the unparalleled capabilities of ALMA, we are now able to spatially resolve the kinematics of cold gas traced by bright atomic/molecular lines such [CII] or CO and measure the galaxy masses through a full kinematical modelling of galaxy disks even at the highest redshifts, thus avoiding all possible biases and effects introduced by the rough estimates usually adopted so far (photometric measurements of stellar masses, virial estimates, etc.). Up to redshift z ∼ 5, the MBH/Mgal ratio is consistent with the extrapolation of the relation inferred at z < 3. At z > 5 we find a steady decrease of the MBH/Mgal ratio with increasing redshift, possibly witnessing the phase of fast growth of the BHs compared to the host galaxies. I will discuss how these results fit within the coevolution scenario and highlight the constraints that they pose on models of galaxy evolution.


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