Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/23707
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | DELL'ORO, Aldo | en_US |
dc.contributor.author | CELLINO, Alberto | en_US |
dc.contributor.author | Paolicchi, P. | en_US |
dc.contributor.author | Tanga, P. | en_US |
dc.date.accessioned | 2020-03-30T14:37:27Z | - |
dc.date.available | 2020-03-30T14:37:27Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0032-0633 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23707 | - |
dc.description | Acknowledgments The authors are grateful to two anonymous reviewers for their constructive comments. | - |
dc.description.abstract | According to the results of hydrodynamical simulations, the creation of an asteroid dynamical family as the outcome of a high-energy collision consists of the partial or complete shattering of the parent body followed by re-accumulation of many fragments into larger bodies due to the mutual gravity. This scenario seems to reproduce satisfactorily the observed properties of the asteroid families, and in particular the size distribution of the members. In this paper we show a preliminary analysis of the ejection velocity fields predicted by hydrodynamical models, in comparison with the ejection velocity fields simulated by semi-empirical models, in order to identify the features of the velocity distribution that trigger or prevent the fragments' gravitational re-accumulation. <P /> | en_US |
dc.language.iso | eng | en_US |
dc.title | Analysis of the kinematics of ejecta created after a catastrophic collision | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1016/j.pss.2015.09.009 | en_US |
dc.identifier.scopus | 2-s2.0-84948845758 | en_US |
dc.identifier.isi | 000370460100035 | en_US |
dc.identifier.url | https://www.sciencedirect.com/science/article/abs/pii/S0032063315002597 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 118 | en_US |
dc.relation.firstpage | 285 | en_US |
dc.relation.lastpage | 295 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FRA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | PLANETARY AND SPACE SCIENCE | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015P&SS..118..285D | en_US |
dc.relation.ercsector | Scienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_2 Planetary systems sciences | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0003-1561-9685 | - |
crisitem.author.orcid | 0000-0002-6645-334X | - |
crisitem.journal.journalissn | 0032-0633 | - |
crisitem.journal.ance | E132431 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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File | Descrizione | Dimensioni | Formato | |
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pss.118.285-295-pre.pdf | 1.82 MB | Adobe PDF | Visualizza/apri | |
1-s2.0-S0032063315002597-main.pdf | [Administrators only] | 2.08 MB | Adobe PDF |
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