Editing Planetary system (section)

====Planet capture====
[[Rogue planet|Free-floating planet]]s in open clusters have similar velocities to the stars and so can be recaptured. They are typically captured into wide orbits between 100 and <!--abstract seems to have a typo 10^6: rest of paper uses 10^5-->10<sup>5</sup> AU<!--see preceding comment-->. The capture efficiency decreases with increasing cluster size, and for a given cluster size it increases with the host/primary{{Clarify|reason=Please reword to avoid the use of a slash; this is ambiguous.|date=August 2021}} mass. It is almost independent of the planetary mass. Single and multiple planets could be captured into arbitrary unaligned orbits, non-coplanar with each other or with the stellar host spin, or pre-existing planetary system. Some planet–host metallicity correlation may still exist due to the common origin of the stars from the same cluster. Planets would be unlikely to be captured around [[neutron star]]s because these are likely to be ejected from the cluster by a [[pulsar kick]] when they form. Planets could even be captured around other planets to form free-floating planet binaries. After the cluster has dispersed some of the captured planets with orbits larger than 10<sup>6</sup> AU would be slowly disrupted by the [[galactic tide]] and likely become free-floating again through encounters with other field stars or giant [[molecular cloud]]s.<ref name="WideRecapture">{{cite journal |last1=Perets |first1=Hagai B. |title=On the Origin of Planets at Very Wide Orbits from the Recapture of Free Floating Planets |date=2012-03-13 |last2=Kouwenhoven |first2=M. B. N.|journal=The Astrophysical Journal |volume=750 |issue=1 |page=83 |doi=10.1088/0004-637X/750/1/83 |arxiv=1202.2362 |bibcode=2012ApJ...750...83P }}</ref>