Show simple item record

Files in this item


Item metadata

dc.contributor.authorRice, Ken
dc.contributor.authorLopez, Eric
dc.contributor.authorForgan, Duncan
dc.contributor.authorBiller, Beth
dc.identifier.citationRice , K , Lopez , E , Forgan , D & Biller , B 2015 , ' Disc fragmentation rarely forms planetary-mass objects ' , Monthly Notices of the Royal Astronomical Society , vol. 454 , no. 2 , pp. 1940-1947 .
dc.identifier.otherPURE: 252129649
dc.identifier.otherPURE UUID: f66247e6-521e-4064-82b7-c8c19d402a70
dc.identifier.otherBibCode: 2015MNRAS.454.1940R
dc.identifier.otherScopus: 84975780144
dc.identifier.otherWOS: 000367997700060
dc.descriptionKR gratefully acknowledges support from STFC grant ST/M001229/1. The research leading to these results also received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). DF grateful acknowledges support from the ECOGAL ERC advanced grant.en
dc.description.abstractIt is now reasonably clear that disc fragmentation can only operate in the outer parts of protostellar discs (r > 50 au). It is also expected that any object that forms via disc fragmentation will have an initial mass greater than that of Jupiter. However, whether or not such a process actually operates, or can play a significant role in the formation of planetary-mass objects, is still unclear. We do have a few examples of directly imaged objects that may have formed in this way, but we have yet to constrain how often disc fragmentation may actually form such objects. What we want to consider here is whether or not we can constrain the likely population of planetary-mass objects formed via disc fragmentation by considering how a population of objects at large radii (a > 50) au - if they do exist - would evolve under perturbations from more distant stellar companions. We find that there is a specific region of parameter space to which such objects would bes cattered and show that the known exoplanets in that region have properties more consistent with that of the bulk exoplanet population, than with having been formed via disc fragmentation at large radii. Along with the scarcity of directly imaged objects at large radii, our results provide a similar, but independent, constraint on the frequency of objects formed via disc fragmentation.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2015, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at
dc.subjectPlanets and satellites: formationen
dc.subjectPlanets and satellites: generalen
dc.subjectBrown dwarfsen
dc.subjectStars: formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleDisc fragmentation rarely forms planetary-mass objectsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Commissionen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

This item appears in the following Collection(s)

Show simple item record