000888553 001__ 888553
000888553 005__ 20220930130259.0
000888553 0247_ $$2doi$$a10.3847/1538-4357/abb9ae
000888553 0247_ $$2ISSN$$a0004-637X
000888553 0247_ $$2ISSN$$a1538-4357
000888553 0247_ $$2Handle$$a2128/26421
000888553 0247_ $$2altmetric$$aaltmetric:90800658
000888553 0247_ $$2WOS$$aWOS:000588213700001
000888553 037__ $$aFZJ-2020-05017
000888553 082__ $$a520
000888553 1001_ $$0P:(DE-Juel1)177668$$aPfalzner, Susanne$$b0$$eCorresponding author
000888553 245__ $$aOumuamuas Passing through Molecular Clouds
000888553 260__ $$aLondon$$bInstitute of Physics Publ.86747$$c2020
000888553 3367_ $$2DRIVER$$aarticle
000888553 3367_ $$2DataCite$$aOutput Types/Journal article
000888553 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1607437437_11439
000888553 3367_ $$2BibTeX$$aARTICLE
000888553 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000888553 3367_ $$00$$2EndNote$$aJournal Article
000888553 520__ $$aThe detections of 1I/'Oumuamua and 2I/Borisov within just two years of each other impressively demonstrate that interstellar objects (ISOs) must be common in the Milky Way. Once released from their parent system, these ISOs travel for billions of years through interstellar space. While often imagined as empty, interstellar space contains gas and dust most prominent in the form of molecular clouds. Performing numerical simulations, we test how often ISOs cross such molecular clouds (MCs). We find that the ISOs pass through MCs amazingly often. In the solar neighborhood, ISOs typically spend 0.1%-0.2% of their journey inside MCs, for relatively slow ISOs (<5 km s-1) this can increase to 1%-2%, equivalent to 10-20 Myr per Gyr. Thus the dynamically youngest ISOs spend the longest time in MCs. In other words, MCs must mainly contain relatively young ISOs (<1-2 Gyr). Thus the half-life of the seeding process by ISOs is substantially shorter than a stellar lifetime. The actual amount of time spent in MCs decreases with distance to the Galactic center. We find that ISOs pass through MCs so often that backtracing their path to find their parent star beyond 250 Myr seems pointless. Besides, we give a first estimate of the ISO density depending on the distance to the Galactic center based on the stellar distribution.
000888553 536__ $$0G:(DE-HGF)POF3-511$$a511 - Computational Science and Mathematical Methods (POF3-511)$$cPOF3-511$$fPOF III$$x0
000888553 588__ $$aDataset connected to CrossRef
000888553 7001_ $$0P:(DE-HGF)0$$aDavies, Melvyn B.$$b1
000888553 7001_ $$0P:(DE-HGF)0$$aKokaia, Giorgi$$b2
000888553 7001_ $$00000-0003-3257-4490$$aBannister, Michele T.$$b3
000888553 773__ $$0PERI:(DE-600)1473835-1$$a10.3847/1538-4357/abb9ae$$gVol. 903, no. 2, p. 114 -$$n2$$p114 -$$tThe astrophysical journal / 1$$v903$$x1538-4357$$y2020
000888553 8564_ $$uhttps://juser.fz-juelich.de/record/888553/files/Oumuamuas_in_clouds.pdf$$yOpenAccess
000888553 8767_ $$88164227$$92020-12-07$$d2020-12-29$$eOther$$jZahlung erfolgt$$z821 $  /  Belegnr. 1200161143
000888553 909CO $$ooai:juser.fz-juelich.de:888553$$popenCost$$pVDB$$pdriver$$pOpenAPC$$popen_access$$popenaire$$pdnbdelivery
000888553 9101_ $$0I:(DE-588b)5008462-8$$6P:(DE-Juel1)177668$$aForschungszentrum Jülich$$b0$$kFZJ
000888553 9131_ $$0G:(DE-HGF)POF3-511$$1G:(DE-HGF)POF3-510$$2G:(DE-HGF)POF3-500$$3G:(DE-HGF)POF3$$4G:(DE-HGF)POF$$aDE-HGF$$bKey Technologies$$lSupercomputing & Big Data$$vComputational Science and Mathematical Methods$$x0
000888553 9141_ $$y2020
000888553 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0300$$2StatID$$aDBCoverage$$bMedline$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0600$$2StatID$$aDBCoverage$$bEbsco Academic Search$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)1150$$2StatID$$aDBCoverage$$bCurrent Contents - Physical, Chemical and Earth Sciences$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)9905$$2StatID$$aIF >= 5$$bASTROPHYS J : 2018$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0150$$2StatID$$aDBCoverage$$bWeb of Science Core Collection$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0113$$2StatID$$aWoS$$bScience Citation Index Expanded$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000888553 915__ $$0StatID:(DE-HGF)0100$$2StatID$$aJCR$$bASTROPHYS J : 2018$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0020$$2StatID$$aNo Peer Review$$bASC$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0160$$2StatID$$aDBCoverage$$bEssential Science Indicators$$d2020-08-32
000888553 915__ $$0StatID:(DE-HGF)0199$$2StatID$$aDBCoverage$$bClarivate Analytics Master Journal List$$d2020-08-32
000888553 9201_ $$0I:(DE-Juel1)JSC-20090406$$kJSC$$lJülich Supercomputing Center$$x0
000888553 9801_ $$aFullTexts
000888553 980__ $$ajournal
000888553 980__ $$aVDB
000888553 980__ $$aUNRESTRICTED
000888553 980__ $$aI:(DE-Juel1)JSC-20090406
000888553 980__ $$aAPC