Planetesimal fragmentation and giant planet formation II. Dependencies with planetesimal relative velocities and compositions

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dc.contributor.authorSan Sebastian, I. L.
dc.contributor.authorGuilera, O. M.
dc.contributor.authorParisi, M. G.
dc.date.accessioned2025-01-23T21:13:42Z
dc.date.available2025-01-23T21:13:42Z
dc.date.issued2019
dc.description.abstractContext. Most planet formation models that incorporate planetesimal fragmentation consider a catastrophic impact energy threshold for basalts at a constant velocity of 3 km s(-1) throughout the process of the formation of the planets. However, as planets grow, the relative velocities of the surrounding planetesimals increase from velocities of the order of meters per second to a few kilometers per second. In addition, beyond the ice line where giant planets are formed, planetesimals are expected to be composed roughly of 50% ices.
dc.description.abstractAims. We aim to study the role of planetesimal fragmentation on giant planet formation considering the planetesimal catastrophic impact energy threshold as a function of the planetesimal relative velocities and compositions.
dc.description.abstractMethods. We improved our model of planetesimal fragmentation incorporating a functional form of the catastrophic impact energy threshold with the planetesimal relative velocities and compositions. We also improved in our model the accretion of small fragments produced by the fragmentation of planetesimals during the collisional cascade considering specific pebble accretion rates.
dc.description.abstractResults. We find that a more accurate and realistic model for the calculation of the catastrophic impact energy threshold tends to slow down the formation of massive cores. Only for reduced grain opacity values at the envelope of the planet is the cross-over mass achieved before the disk timescale dissipation.
dc.description.abstractConclusions. While planetesimal fragmentation favors the quick formation of massive cores of 5-10 M-circle plus the cross-over mass could be inhibited by planetesimal fragmentation. However, grain opacity reduction or pollution by the accreted planetesimals together with planetesimal fragmentation could explain the formation of giant planets with low-mass cores.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201834168
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201834168
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101007
dc.identifier.wosidWOS:000469212300006
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectplanets and satellites: formation
dc.subjectplanets and satellites: gaseous planets
dc.subjectmethods: numerical
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titlePlanetesimal fragmentation and giant planet formation II. Dependencies with planetesimal relative velocities and compositions
dc.typeartículo
dc.volumen625
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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