J/MNRAS/492/2683ivo://CDS.VizieR/J/MNRAS/492/2683doi:10.26093/cds/vizier.74922683CDSBonsor A.Carter P.J.Hollands M.Gansicke B.T.Leinhardt Z.,Harrison J.H.D.2024-08-20T20:15:34Z2023-06-12T14:54:13ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frexoplanetswhite-dwarf-starschemically-peculiar-starseffective-temperaturevisible-astronomyspectroscopyMetals observed in the atmospheres of white dwarfs suggest that many have recently accreted planetary bodies. In some cases, the compositions observed suggest the accretion of material dominantly from the core (or the mantle) of a differentiated planetary body. Collisions between differentiated exoplanetesimals produce such fragments. In this work, we take advantage of the large numbers of white dwarfs where at least one siderophile (core-loving) and one lithophile (rock-loving) species have been detected to assess how commonly exoplanetesimals differentiate. We utilize N-body simulations that track the fate of core and mantle material during the collisional evolution of planetary systems to show that most remnants of differentiated planetesimals retain core fractions similar to their parents, while some are extremely core rich or mantle rich. Comparison with the white dwarf data for calcium and iron indicates that the data are consistent with a model in which 66^+4^_-6_ per cent have accreted the remnants of differentiated planetesimals, while 31^+5^_-5_ per cent have Ca/Fe abundances altered by the effects of heating (although the former can be as high as 100 per cent, if heating is ignored). These conclusions assume pollution by a single body and that collisional evolution retains similar features across diverse planetary systems. These results imply that both collisions and differentiation are key processes in exoplanetary systems. We highlight the need for a larger sample of polluted white dwarfs with precisely determined metal abundances to better understand the process of differentiation in exoplanetary systems.2020MNRAS.492.2683Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/492/2683CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/492/2683https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/492/2683http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/492/2683https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/492/2683https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/492/2683http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/492/2683GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/492/2683/tablea1 (The polluted white dwarfs where both calcium and iron were detected, as used in this work)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/492/2683/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/492/2683/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/492/2683/tablea1?GETtext/xml+votable180.050000true21.1864-22.48524530.0055555555555555566/670 678 1449 2098 2280 4156 4202 4292 4328 4331 4333 4428 4445 4621 4733 4746 4770 4813 4887 4895 4898 4977 5089 5139 5155 5236 5290 5331 5334 5347 5503 5505 5529 5598 5780 5787 5809 5871 5920 6015 6218 6237 6255 6395 6548 6568 6584 6591 7223 7250 7327 7457 8213 8345 8350 8480 8526 8544 8692 8749 8808 8938 8941 9201 9386 9397 9417 9501 9606 9869 9953 10019 10271 10307 10378 10413 10432 10457 10476 10510 10540 10542 10616 10777 10852 11147 11149 11335 11345 13348 15816 16243 17372 17497 17599 17757 17806 17837 18012 18127 18303 18375 18801 18850 18856 18902 19107 19120 19205 19263 19386 19483 19597 19766 19806 19893 19897 19958 20195 20238 20363 20395 20419 20427 21789 21982 22821 23416 25460 25931 26038 26143 26236 26279 26365 26482 26490 26572 26580 27048 27061 27129 27417 27631 27645 27685 27692 27719 27742 27749 27769 27829 27903 27993 28106 28226 28435 28493 28510 28632 28654 30465 31732 32419 32441 32493 34686 35663 35832 36845 36861 40551 44732 45110 45506 45561 45921https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/492/2683?format=asciiOpticaldefaultJ/MNRAS/492/2683/tablea1The polluted white dwarfs where both calcium and iron were detected, as used in this workSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameWhite dwarf namemeta.id;meta.maincharRefReferences (1)meta.refcharTeffEffective temperatureKphys.temperature.effectiveint[Ca/H]Ca/H abundance ratiophys.abundfloate_[Ca/H]Error on Ca/Hstat.error;phys.abundfloat[Fe/H]Fe/H abundance ratiophys.abund.Fe;arith.ratiofloate_[Fe/H]Error on Fe/Hstat.error;phys.abund.Fefloat[Ca/Fe]Ca/Fe abundance ratiophys.abund;arith.ratiofloate_[Ca/Fe]Error on Ca/Festat.error;phys.abundfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main