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On the origin of planets at very wide orbits from the re-capture of free floating planets
Earth and Planetary Astrophysics · Submitted 10 Feb 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Here we propose a novel scenario for the production of planetary systems at such orbits, through the dynamical recapture of free floating planets (FFPs) in dispersing stellar clusters.
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The abstract, sentence by sentence
In recent years several planets have been discovered at wide orbits (>100 AU) around their host stars. Theoretical studies encounter difficulties in explaining their formation and origin. Here we propose a novel scenario for the production of planetary systems at such orbits, through the dynamical recapture of free floating planets (FFPs) in dispersing stellar clusters. This process is a natural extension of the recently suggested scenario for the formation of wide stellar binaries. We use N-body simulations of dispersing clusters with 10-1000 stars and comparable numbers of FFPs to study this process. We find that planets are captured into wide orbits in the typical range ~100-10^6 AU, and have a wide range of eccentricities (thermal distribution). Typically, 3-6 x (f_FFP/1) % of all stars capture a planetary companion with such properties (where f_FFP is the number of FFP per star). The planetary capture efficiency is comparable to that of capture-formed stellar-binaries, and shows a similar dependence on the cluster size and structure. It is almost independent of the specific planetary mass; planets as well as sub-stellar companions of any mass can be captured. The capture efficiency decreases with increasing cluster size, and for a given cluster size the it increases with the host/primary mass. More than one planet can be captured around the same host and planets can be captured into binary systems. Planets can also be captured into pre-existing planetary and into orbits around black holes and massive white dwarfs, if these formed early enough before the cluster dispersal. In particular, stellar black holes have a high capture efficiency (>50 % and 5-10 x (f_FFP/1) % for capture of stars and planetary companions, respectively) due to their large mass. Finally, although rare, two FFPs or brown dwarfs can become bound and form a FFP-binary system with no stellar host.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In recent years several planets have been discovered at wide orbits (>100 AU) around their host stars. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | Theoretical studies encounter difficulties in explaining their formation and origin. | gap 0.71 | 0.04 | 0.02 | asserted 1.00 |
| s2 | Here we propose a novel scenario for the production of planetary systems at such orbits, through the dynamical recapture of free floating planets (FFPs) in dispersing stellar clusters. | contribution 1.00 | 0.42 | 0.62 | speculative 0.40 |
| s3 | This process is a natural extension of the recently suggested scenario for the formation of wide stellar binaries. | background 0.74 | 0.11 | 0.05 | asserted 0.99 |
| s4 | We use N-body simulations of dispersing clusters with 10-1000 stars and comparable numbers of FFPs to study this process. | method 0.99 | 0.93 | 0.03 | asserted 0.92 |
| s5 | We find that planets are captured into wide orbits in the typical range ~100-10^6 AU, and have a wide range of eccentricities (thermal distribution). | result 1.00 | 0.96 | 0.39 | asserted 1.00 |
| s6 | Typically, 3-6 x (f_FFP/1) % of all stars capture a planetary companion with such properties (where f_FFP is the number of FFP per star). | result 1.00 | 0.93 | 0.17 | asserted 0.99 |
| s7 | The planetary capture efficiency is comparable to that of capture-formed stellar-binaries, and shows a similar dependence on the cluster size and structure. | result 0.87 | 0.88 | 0.10 | asserted 1.00 |
| s8 | It is almost independent of the specific planetary mass; planets as well as sub-stellar companions of any mass can be captured. | result 1.00 | 0.85 | 0.07 | asserted 1.00 |
| s9 | The capture efficiency decreases with increasing cluster size, and for a given cluster size the it increases with the host/primary mass. | result 1.00 | 0.91 | 0.06 | asserted 1.00 |
| s10 | More than one planet can be captured around the same host and planets can be captured into binary systems. | result 1.00 | 0.89 | 0.07 | asserted 0.69 |
| s11 | Planets can also be captured into pre-existing planetary and into orbits around black holes and massive white dwarfs, if these formed early enough before the cluster dispersal. | result 0.97 | 0.67 | 0.04 | hedged possibility 0.80 |
| s12 | In particular, stellar black holes have a high capture efficiency (>50 % and 5-10 x (f_FFP/1) % for capture of stars and planetary companions, respectively) due to their large mass. | result 1.00 | 0.86 | 0.09 | asserted 1.00 |
| s13 | Finally, although rare, two FFPs or brown dwarfs can become bound and form a FFP-binary system with no stellar host. | result 1.00 | 0.75 | 0.03 | asserted 0.60 |
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Original abstract
In recent years several planets have been discovered at wide orbits (>100 AU) around their host stars. Theoretical studies encounter difficulties in explaining their formation and origin. Here we propose a novel scenario for the production of planetary systems at such orbits, through the dynamical recapture of free floating planets (FFPs) in dispersing stellar clusters. This process is a natural extension of the recently suggested scenario for the formation of wide stellar binaries. We use N-body simulations of dispersing clusters with 10-1000 stars and comparable numbers of FFPs to study this process. We find that planets are captured into wide orbits in the typical range ~100-10^6 AU, and have a wide range of eccentricities (thermal distribution). Typically, 3-6 x (f_FFP/1) % of all stars capture a planetary companion with such properties (where f_FFP is the number of FFP per star). The planetary capture efficiency is comparable to that of capture-formed stellar-binaries, and shows a similar dependence on the cluster size and structure. It is almost independent of the specific planetary mass; planets as well as sub-stellar companions of any mass can be captured. The capture efficiency decreases with increasing cluster size, and for a given cluster size the it increases with the host/primary mass. More than one planet can be captured around the same host and planets can be captured into binary systems. Planets can also be captured into pre-existing planetary and into orbits around black holes and massive white dwarfs, if these formed early enough before the cluster dispersal. In particular, stellar black holes have a high capture efficiency (>50 % and 5-10 x (f_FFP/1) % for capture of stars and planetary companions, respectively) due to their large mass. Finally, although rare, two FFPs or brown dwarfs can become bound and form a FFP-binary system with no stellar host.
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