Browsing by Author "Ronco, M. P."

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    Formation of Solar system analogues - II. Post-gas-phase growth and water accretion in extended discs via N-body simulations
    (2018) Ronco, M. P.; de Elia, G. C.
    This work is the second part of a project that attempts to analyse the formation of Solar system analogues (SSAs) from the gaseous to the post-gas phase, in a self-consistently way. In the first paper (PI) we presented our model of planet formation during the gaseous phase which provided us with embryo distributions, planetesimal surface density, eccentricity, and inclination profiles of SSAs, considering different planetesimal sizes and type I migration rates at the time the gas dissipates. In this second work we focus on the late accretion stage of SSAs using the results obtained in PI as initial conditions to carry out N-body simulations. One of our interests is to analyse the formation of rocky planets and their final water contents within the habitable zone. Our results show that the formation of potentially habitable planets (PHPs) seems to be a common process in this kind of scenarios. However, the efficiency in forming PHPs is directly related to the size of the planetesimals. The smaller the planetesimals, the greater the efficiency in forming PHPs. We also analyse the sensitivity of our results to scenarios with type I migration rates and gap-opening giants, finding that both phenomena act in a similar way. These effects seem to favour the formation of PHPs for small planetesimal scenarios and to be detrimental for scenarios formed from big planetesimals. Finally, another interesting result is that the formation of water-rich PHPs seems to be more common than the formation of dry PHPs.
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    The HD 98800 quadruple pre-main sequence system Towards full orbital characterisation using long-baseline infrared interferometry
    (2021) Zuniga-Fernandez, S.; Olofsson, J.; Bayo, A.; Haubois, X.; Corral-Santana, J. M.; Lopera-Mejia, A.; Ronco, M. P.; Tokovinin, A.; Gallenne, A.; Kennedy, G. M.; Berger, J-P
    Context. HD 98800 is a young (similar to 10 Myr old) and nearby (similar to 45 pc) quadruple system, composed of two spectroscopic binaries orbiting around each other (AaAb and BaBb), with a gas-rich disk in polar configuration around BaBb. While the orbital parameters of BaBb and AB are relatively well constrained, this is not the case for AaAb. A full characterisation of this quadruple system can provide insights on the formation of such a complex system.
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    Thermal torque effects on the migration of growing low-mass planets
    (2019) Guilera, O. M.; Cuello, N.; Montesinos, M.; Bertolami, M. M. M.; Ronco, M. P.; Cuadra Stipetich, Jorge Rodrigo; Masset, F. S.
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    WD 1856 b: a close giant planet around a white dwarf that could have survived a common envelope phase
    (2021) Lagos, F.; Schreiber, M. R.; Zorotovic, M.; Gansicke, B. T.; Ronco, M. P.; Hamers, Adrian S.
    The discovery of a giant planet candidate orbiting the white dwarf WD 1856+534 with an orbital period of 1.4 d poses the questions of how the planet reached its current position. We here reconstruct the evolutionary history of the system assuming common envelope evolution as the main mechanism that brought the planet to its current position. We find that common envelope evolution can explain the present configuration if it was initiated when the host star was on the asymptotic giant branch, the separation of the planet at the onset of mass transfer was in the range 1.69-2.35 au, and if in addition to the orbital energy of the surviving planet either recombination energy stored in the envelope or another source of additional energy contributed to expelling the envelope. We also discuss the evolution of the planet prior to and following common envelope evolution. Finally, we find that if the system formed through common envelope evolution, its total age is in agreement with its membership to the Galactic thin disc. We therefore conclude that common envelope evolution is at least as likely as alternative formation scenarios previously suggested such as planet-planet scattering or Kozai-Lidov oscillations.