Outward migration of a super-Earth in a disc with outward propagating density waves excited by a giant planet

Authors

  • E. Podlewska-Gaca,

    Corresponding author
    1. Institute of Physics and CASA, University of Szczecin, ul. Wielkopolska 15, 70-451 Szczecin, Poland
    2. Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA
      E-mail: edytap@univ.szczecin.pl (EP-G); J.C.B.Papaloizou@dampt.cam.ac.uk (JCBP); szusz@fermi.fiz.univ.szczecin.pl (ES)
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  • J. C. B. Papaloizou,

    Corresponding author
    1. Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA
      E-mail: edytap@univ.szczecin.pl (EP-G); J.C.B.Papaloizou@dampt.cam.ac.uk (JCBP); szusz@fermi.fiz.univ.szczecin.pl (ES)
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  • E. Szuszkiewicz

    Corresponding author
    1. Institute of Physics and CASA, University of Szczecin, ul. Wielkopolska 15, 70-451 Szczecin, Poland
    2. Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA
      E-mail: edytap@univ.szczecin.pl (EP-G); J.C.B.Papaloizou@dampt.cam.ac.uk (JCBP); szusz@fermi.fiz.univ.szczecin.pl (ES)
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E-mail: edytap@univ.szczecin.pl (EP-G); J.C.B.Papaloizou@dampt.cam.ac.uk (JCBP); szusz@fermi.fiz.univ.szczecin.pl (ES)

ABSTRACT

In this paper, we consider a new mechanism for stopping the inward migration of a low-mass planet embedded in a gaseous protoplanetary disc. It operates when a low-mass planet (for example a super-Earth) encounters outgoing density waves excited by another source in the disc. This source could be a gas giant in an orbit interior to that of the low-mass planet. As the super-Earth passes through the wave field, angular momentum is transferred to the disc material and then communicated to the planet through co-orbital dynamics, with the consequence that its inward migration can be halted or even reversed.

We illustrate how the mechanism we consider works in a variety of different physical conditions employing global two-dimensional hydrodynamical calculations. We confirm our results by performing local shearing box simulations in which the super-Earth interacts with density waves excited by an independent harmonically varying potential. Finally, we discuss the constraints arising from the process considered here, on formation scenarios for systems containing a giant planet and lower mass planet in an outer orbit with a 2:1 commensurability such as GJ 876.

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