Dynamics and Planet Formation in/Around Binaries

  • Francesco Marzari
  • Philippe Thébault
  • Steve Kortenkamp
  • Hans Scholl
Part of the Astrophysics and Space Science Library book series (ASSL, volume 366)


The extent to which planetesimal accretion is affected by the perturbing presence of a companion star is an important issue in the formation of planets in and around binary systems. In this chapter, we review this issue by concentrating on one crucial parameter: the distribution of encounter velocities within the planetesimal swarm. The evolution of this parameter is numerically explored accounting for the secular perturbations of the binary and the friction due to the very likely presence of gas in the disk. Maps of the average encounter velocity ⟨Δv⟩ between different size planetesimals are presented for a total of 120 stellar dynamical configurations obtained by different combinations of the binary semimajor axis a b and eccentricity e b . According to the different values of ⟨Δv⟩, 3 different planetesimal accumulation modes are identified: 1) in regions where ⟨Δv⟩ is comparable to that derived for planetesimal swarms around single-stars, “standard” accretion is likely, eventually via runaway growth, 2) in regions where ⟨Δv⟩ is larger than v ero , the threshold velocity above which all impacts are eroding, no accretion is possible and planet growth is stopped, 3) in between these two extremes, there is a large fraction of binary configurations where the increase in ⟨Δv⟩ is still below the erosion threshold. Planetesimal accumulation can still occur but it possibly proceeds at a slower rate than in the single-star case, following the so-called type II runaway growth mode.


Semimajor Axis Giant Planet Terrestrial Planet Protoplanetary Disk Companion Star 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.



S. Kortenkamp acknowledges support from NASA for some of this work under grants NNG04GP56G and NNG04GI14G.


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© Springer Science+Business Media B.V. 2010

Authors and Affiliations

  1. 1.Dipartimento di FisicaPaduvaItaly
  2. 2.Observatoire de ParisSection de MeudonPrincipal CedexFrance
  3. 3.Planetary Science InstituteTucsonUSA
  4. 4.Observatoire de la Côte d’AzurNice, Cedex 4France

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