000904521 001__ 904521
000904521 005__ 20220930130335.0
000904521 0247_ $$2doi$$a10.3847/1538-4357/ac19aa
000904521 0247_ $$2ISSN$$a0004-637X
000904521 0247_ $$2ISSN$$a1538-4357
000904521 0247_ $$2Handle$$a2128/29635
000904521 0247_ $$2altmetric$$aaltmetric:112245524
000904521 0247_ $$2WOS$$aWOS:000716744900001
000904521 037__ $$aFZJ-2021-06091
000904521 082__ $$a520
000904521 1001_ $$0P:(DE-Juel1)177668$$aPfalzner, Susanne$$b0$$eCorresponding author
000904521 245__ $$aClose Stellar Flybys Common in Low-mass Clusters
000904521 260__ $$aLondon$$bInstitute of Physics Publ.$$c2021
000904521 3367_ $$2DRIVER$$aarticle
000904521 3367_ $$2DataCite$$aOutput Types/Journal article
000904521 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1651563450_10981
000904521 3367_ $$2BibTeX$$aARTICLE
000904521 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000904521 3367_ $$00$$2EndNote$$aJournal Article
000904521 520__ $$aNumerous protoplanetary disks show distinct spiral arms features. While possibly caused by a range of processes, detailed pattern analysis points at close stellar flybys as cause for some of them. Surprisingly, these disks reside in young low-mass clusters, where close stellar flybys are expected to be rare. This fact motivated us to take a fresh look at the frequency of close flybys in low-mass clusters. In the solar neighborhood, low-mass clusters have smaller half-mass radii than their more massive counterparts. We show that this observational fact results in the mean and central stellar density of low-mass clusters being approximately the same as in high-mass clusters, which is rarely reflected in theoretical studies. We perform N-body simulations of the stellar dynamics in young clusters obeying the observed mass–radius relation. Taking the mean disk truncation radius as a proxy for the degree of influence of the environment, we find that the influence of the environment on disks is more or less the same in low- and high-mass clusters. Even the fraction of small disks (<10 au) is nearly identical. Our main conclusion is that the frequency of close flybys seems to have been severely underestimated for low-mass clusters. A testable prediction of this hypothesis is that low-mass clusters should contain 10%–15% of disks smaller than 30 au truncated by flybys. These truncated disks should be distinguishable from primordially small disks by their steep outer edge.
000904521 536__ $$0G:(DE-HGF)POF4-5111$$a5111 - Domain-Specific Simulation & Data Life Cycle Labs (SDLs) and Research Groups (POF4-511)$$cPOF4-511$$fPOF IV$$x0
000904521 588__ $$aDataset connected to CrossRef, Journals: juser.fz-juelich.de
000904521 7001_ $$0P:(DE-Juel1)184730$$aGovind, Amith$$b1$$ufzj
000904521 773__ $$0PERI:(DE-600)1473835-1$$a10.3847/1538-4357/ac19aa$$gVol. 921, no. 1, p. 90 -$$n1$$p90 -$$tThe astrophysical journal / 1$$v921$$x0004-637X$$y2021
000904521 8564_ $$uhttps://juser.fz-juelich.de/record/904521/files/Invoice_8198278.pdf
000904521 8564_ $$uhttps://juser.fz-juelich.de/record/904521/files/Pfalzner_2021_ApJ_921_90.pdf$$yOpenAccess
000904521 8767_ $$88198278$$92022-03-03$$a1200180724$$d2022-05-05$$ePage charges$$jZahlung erfolgt$$zUSD 2508,-
000904521 909CO $$ooai:juser.fz-juelich.de:904521$$popenCost$$pVDB$$pdriver$$pOpenAPC$$popen_access$$popenaire$$pdnbdelivery
000904521 9101_ $$0I:(DE-588b)5008462-8$$6P:(DE-Juel1)177668$$aForschungszentrum Jülich$$b0$$kFZJ
000904521 9101_ $$0I:(DE-588b)5008462-8$$6P:(DE-Juel1)184730$$aForschungszentrum Jülich$$b1$$kFZJ
000904521 9131_ $$0G:(DE-HGF)POF4-511$$1G:(DE-HGF)POF4-510$$2G:(DE-HGF)POF4-500$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$9G:(DE-HGF)POF4-5111$$aDE-HGF$$bKey Technologies$$lEngineering Digital Futures – Supercomputing, Data Management and Information Security for Knowledge and Action$$vEnabling Computational- & Data-Intensive Science and Engineering$$x0
000904521 9141_ $$y2021
000904521 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0300$$2StatID$$aDBCoverage$$bMedline$$d2021-02-02
000904521 915__ $$0LIC:(DE-HGF)CCBY4$$2HGFVOC$$aCreative Commons Attribution CC BY 4.0
000904521 915__ $$0StatID:(DE-HGF)0600$$2StatID$$aDBCoverage$$bEbsco Academic Search$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)1150$$2StatID$$aDBCoverage$$bCurrent Contents - Physical, Chemical and Earth Sciences$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)9905$$2StatID$$aIF >= 5$$bASTROPHYS J : 2019$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0150$$2StatID$$aDBCoverage$$bWeb of Science Core Collection$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0113$$2StatID$$aWoS$$bScience Citation Index Expanded$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000904521 915__ $$0StatID:(DE-HGF)0100$$2StatID$$aJCR$$bASTROPHYS J : 2019$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0020$$2StatID$$aNo Peer Review$$bASC$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0160$$2StatID$$aDBCoverage$$bEssential Science Indicators$$d2021-02-02
000904521 915__ $$0StatID:(DE-HGF)0199$$2StatID$$aDBCoverage$$bClarivate Analytics Master Journal List$$d2021-02-02
000904521 9201_ $$0I:(DE-Juel1)JSC-20090406$$kJSC$$lJülich Supercomputing Center$$x0
000904521 9801_ $$aFullTexts
000904521 980__ $$ajournal
000904521 980__ $$aVDB
000904521 980__ $$aI:(DE-Juel1)JSC-20090406
000904521 980__ $$aUNRESTRICTED
000904521 980__ $$aAPC