Abstract
The growing body of observational data on extrasolar planets and protoplanetary disks has stimulated intense research on planet formation and evolution in the past few years. The extremely diverse, sometimes unexpected physical and orbital characteristics of exoplanets lead to frequent updates on the mainstream scenarios for planet formation and evolution, but also to the exploration of alternative avenues. The aim of this review is to bring together classical pictures and new ideas on the formation, orbital and internal evolutions of planets, highlighting the key role of the protoplanetary disk in the various parts of the theory. We begin by briefly reviewing the conventional mechanism of core accretion by the growth of planetesimals, and discuss a relatively recent model of core growth through the accretion of pebbles. We review the basic physics of planet-disk interactions, recent progress in this area, and discuss their role in observed planetary systems. We address the most important effects of planets internal evolution, like cooling and contraction, the mass-luminosity relation, and the bulk composition expressed in the mass-radius and mass-mean density relations.
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Notes
As long as \(M_{c}\) is much smaller than the “thermal mass” \(M_{\mathrm{th}}=c_{\mathrm{s}}^{3}/G\varOmega_{\mathrm{K}}\), which is about the mass scale of Jupiter and is well beyond the mass scale for core growth.
Note this definition given in Lambrechts and Johansen (2012) is different from the conventional definition of the Bondi radius, where \(\Delta v_{\mathrm{K}}\) is replaced by the sound speed.
By integrating individual particle trajectories, \(r_{a}\) is found to be about \(R_{\mathrm{H}}\) for particles with \(\tau_{s}\sim0.1\) (Lambrechts and Johansen 2012), thus \(r_{a}\approx(\tau_{s}/0.1)^{1/3}R_{\mathrm{H}}\) is probably more accurate for \(\tau_{s}\lesssim0.1\), which still agrees with the order-of-magnitude derivation within a factor of order unity.
This is inferred from the sample of planets listed in http://exoplanets.org that have a minimum mass greater than \(0.5 M_{\mathrm{J}}\). Defining as aligned a planet with projected obliquity less than about 40°, we find that, in the range of orbital periods between 1 and 3 days, there are 18 aligned and 7 misaligned planets, while for orbital periods between 3 and 5 days, there are 16 aligned and 8 misaligned planets.
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Acknowledgements
We thank the organizers of the ISSI workshop “The Disk in Relation to the Formation of Planets and their Protoatmospheres”, which was held in Beijing in August 2014. We thank D. Lin, N. Madhusudhan, Z. Sandor and S. Udry for stimulating discussions at the workshop. We thank Gabriel Marleau for interesting discussions and for providing Figure 7, and David Swoboda and Yann Alibert for providing the starting data for Figure 11. We also thank Aurélien Crida and Bertram Bitsch for detailed comments on an earlier draft of this paper, and the referee for a detailed and constructive report. XNB acknowledges support from Hubble and ITC Fellowships. CM acknowledges the support from the Swiss National Science Foundation under grant BSSGI0\(\_\)155816 “PlanetsInTime”.
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Baruteau, C., Bai, X., Mordasini, C. et al. Formation, Orbital and Internal Evolutions of Young Planetary Systems. Space Sci Rev 205, 77–124 (2016). https://doi.org/10.1007/s11214-016-0258-z
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DOI: https://doi.org/10.1007/s11214-016-0258-z