Sebastian Marino’s scientific contributions

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Publications (2)


Fig. 2. Dust density distribution after 1 Myr of evolution for no traps (left panel), weak traps (middle panel), and strong traps (right panel), for the case of M = 0.1M and α = 10 −3 . Top panels: the disk mass is M disk = 0.05 M . Bottom panels: the disk mass is M disk = 0.05 M .
Fig. 3. Effect of stellar mass on the evolution of dust mass of particles larger than 0.1 mm from the models with no traps (left panel), weak traps (middle panel), and strong traps (right panel). In all cases α = 10 −3 and M disk = 0.05 M .
Fig. 9. Left panel: fit of the disk size-luminosity relation from sub-millimeter observations of protoplanetary disks in different star forming regions (colors) as reported in Hendler et al. (2020) compare to the relation for TDs (open circles) and disks with substructures (full triangles). Right panel: evolution of the radius that encloses 95% of the mass of dust particles larger than 0.1 mm from the models that assume strong pressure bumps, M disk = 0.05 M , and α = 10 −3 .
Hints on the origins of particle traps in protoplanetary disks given by the M_dust-M_* relation
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February 2020

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49 Reads

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75 Citations

Astronomy and Astrophysics

Paola Pinilla

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Ilaria Pascucci

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Sebastian Marino

Context. Demographic surveys of protoplanetary disks, carried out mainly with the Atacama Large Millimeter/submillimete Array, have provided access to a large range of disk dust masses ( Mdust ) around stars with different stellar types and in different star-forming regions. These surveys found a power-law relation between Mdust and M⋆ that steepens in time, but which is also flatter for transition disks (TDs). Aims. We aim to study the effect of dust evolution in the Mdust − M⋆ relation. In particular, we are interested in investigating the effect of particle traps on this relation. Methods. We performed dust evolution models, which included perturbations to the gas surface density with different amplitudes to investigate the effect of particle trapping on the Mdust − M⋆ relation. These perturbations were aimed at mimicking pressure bumps that originated from planets. We focused on the effect caused by different stellar and disk masses based on exoplanet statistics that demonstrate a dependence of planet mass on stellar mass and metallicity. Results. Models of dust evolution can reproduce the observed Mdust − M⋆ relation in different star-forming regions when strong pressure bumps are included and when the disk mass scales with stellar mass (case of Mdisk = 0.05 M⋆ in our models). This result arises from dust trapping and dust growth beyond centimeter-sized grains inside pressure bumps. However, the flatter relation of Mdust − M⋆ for TDs and disks with substructures cannot be reproduced by the models unless the formation of boulders is inhibited inside pressure bumps. Conclusions. In the context of pressure bumps originating from planets, our results agree with current exoplanet statistics on giant planet occurrence increasing with stellar mass, but we cannot draw a conclusion about the type of planets needed in the case of low-mass stars. This is attributed to the fact that for M⋆ < 1 M⊙ , the observed Mdust obtained from models is very low due to the efficient growth of dust particles beyond centimeter-sizes inside pressure bumps.

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M_{\rm{dust}}-M_{\star}$ Relation Hints at the Origin of Particle Traps in Protoplanetary Disks

January 2020

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3 Reads

[abridged] Demographic surveys of protoplanetary disks, mainly with ALMA, have provided access to a large range of disk dust masses (MdustM_{\rm{dust}}) around stars with different stellar types and for different star-forming regions. These surveys found a linear relation in logarithmic scale between MdustM_{\rm{dust}} and MM_{\star} that steepens with time, but that is flatter for transition disks (TDs). We perform dust evolution models and include perturbations to the gas surface density with different amplitudes to investigate the effect of particle trapping on the MdustMM_{\rm{dust}}-M_{\star} relation. These perturbations aim to mimic pressure bumps originated by planets. We focus on the effect caused by different stellar and disk masses because exoplanet statistics show a dependence of planet mass with stellar mass and metallicity. We find that models of dust evolution can reproduced the observed MdustMM_{\rm{dust}}-M_{\star} relation in different star-forming regions when strong pressure bumps are included and when the disk mass scales with stellar mass (case of Mdisk=0.05MM_{\rm{disk}}=0.05\,M_\star in our models). This result arises from dust trapping and dust growth beyond centimeter-size grains inside pressure bumps. However, the flatter relation of MdustMM_{\rm{dust}}-M_{\star} for TDs and disks with substructures cannot be reproduced by the models, unless the formation of boulders is inhibited inside pressure bumps. In the context of planets originating pressure bumps, our results agree with the current exoplanet statistics about giant planet occurrence increasing with stellar mass, but we cannot conclude about the type of planets needed in the case of low mass stars. This is because for M<1MM_\star<1\,M_\odot, the observed MdustM_{\rm{dust}} obtained from models is very low due to the efficient growth of dust particles beyond centimeter sizes (boulders) inside pressure bumps.

Citations (1)


... SR24S is the only disk among the transition disks studied by N. van der Marel et al. (2015) where a drop of at least 1 or 2 orders of magnitude in the gas surface density within the disk cavity is not inferred. P. Pinilla et al. (2020) confirmed that the optically thin molecular emissions of 13 CO and C 18 O peak at the center of the disk cavity, indicating no gas deficit within the inner cavity of the disk, unlike many transition disks. As pointed out by P. Pinilla et al. (2020), a large cavity created by photoevaporation is unlikely due to the high accretion rate, the large dust cavity, and the gas emission within this region. ...

Reference:

Constraints on the Physical Origin of Large Cavities in Transition Disks from Multiwavelength Dust Continuum Emission
Hints on the origins of particle traps in protoplanetary disks given by the M_dust-M_* relation

Astronomy and Astrophysics