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dc.contributor.authorScholz, Aleks
dc.contributor.authorMoore, Keavin
dc.contributor.authorJayawardhana, Ray
dc.contributor.authorAigrain, Suzanne
dc.contributor.authorPeterson, Dawn
dc.contributor.authorStelzer, Beate
dc.date.accessioned2018-06-15T16:30:06Z
dc.date.available2018-06-15T16:30:06Z
dc.date.issued2018-06
dc.identifier.citationScholz , A , Moore , K , Jayawardhana , R , Aigrain , S , Peterson , D & Stelzer , B 2018 , ' A universal spin-mass relation for brown dwarfs and planets ' Astrophysical Journal , vol. 859 , no. 2 , 153 . DOI: 10.3847/1538-4357/aabfbeen
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 253378846
dc.identifier.otherPURE UUID: 4b33c132-3094-43c7-bed3-b66c8e5707cf
dc.identifier.otherBibCode: 2018arXiv180407380S
dc.identifier.otherScopus: 85048258408
dc.identifier.otherBibCode: 2018ApJ...859..153S
dc.identifier.urihttp://hdl.handle.net/10023/14136
dc.identifier.urihttp://adsabs.harvard.edu/abs/2018arXiv180407380Sen
dc.descriptionFunding: UK Science and Technology Facilities Council (ST/R000824/1) (AS).en
dc.description.abstractWhile brown dwarfs show similarities to stars early in their lives, their spin evolutions are much more akin to those of planets. We have used light curves from the K2 mission to measure new rotation periods for 18 young brown dwarfs in the Taurus star-forming region. Our sample spans masses from 0.02 to 0.08 M ⊙ and has been characterized extensively in the past. To search for periods, we utilize three different methods (autocorrelation, periodogram, Gaussian processes). The median period for brown dwarfs with disks is twice as long as for those without (3.1 versus 1.6 days), a signature of rotational braking by the disk, albeit with small numbers. With an overall median period of 1.9 days, brown dwarfs in Taurus rotate slower than their counterparts in somewhat older (3–10 Myr) star-forming regions, consistent with spin-up of the latter due to contraction and angular momentum conservation, a clear sign that disk braking overall is inefficient and/or temporary in this mass domain. We confirm the presence of a linear increase of the typical rotation period as a function of mass in the substellar regime. The rotational velocities, when calculated forward to the age of the solar system, assuming angular momentum conservation, fit the known spin–mass relation for solar system planets and extra-solar planetary-mass objects. This spin–mass trend holds over six orders of magnitude in mass, including objects from several different formation paths. Our result implies that brown dwarfs by and large retain their primordial angular momentum through the first few Myr of their evolution.en
dc.format.extent10en
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2018, American Astronomical Society. 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 https://doi.org/https://doi.org/10.3847/1538-4357/aabfbeen
dc.subjectBrown dwarfsen
dc.subjectPlanets and satellites: formationen
dc.subjectProtoplanetary disksen
dc.subjectStars: rotationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleA universal spin-mass relation for brown dwarfs and planetsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aabfbe
dc.description.statusPeer revieweden


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