Modelling Collisions Between Asteroids: From Laboratory Experiments to Numerical Simulations View Full Text


Ontology type: schema:Chapter     


Chapter Info

DATE

2006

AUTHORS

Patrick Michel

ABSTRACT

Thanks to the development of sophisticated numerical codes, a major breakthrough has been achieved in our understanding of the process involved in small body collisions. Such events play a fundamental role in all the stages of the formation and evolution of planetary systems, and more particularly of our Solar System. Laboratory experiments on centimeter-sized targets have been performed to improve our knowledge on this process, but their extrapolation to asteroid scales remains confronted to major diffculties. In this lecture, we present a brief review of our current understanding of the fragmentation process of solid bodies and its implementation in numerical codes aimed at simulating asteroid break-up events. The most recent results provided by numerical simulations are also presented. Although our current understanding is still based on several limitations and assumptions, the development of sophisticated numerical codes accounting for the fragmentation of an asteroid and for the gravitational interactions of the generated fragments have allowed to improve greatly our knowledge on the main mechanisms that are at the origin of some observed features in the asteroid belt. In particular, the simulations have demonstrated that, for bodies larger than several kilometers, the collisional process does not only involves the fragmentation of the asteroid but also the gravitational interactions between the fragments that are ejected. This latter mechanism can lead to the formation of large agregates by gravitational reaccumulation of smaller fragments, allowing to explain the presence of large members within asteroid families. Numerical simulations of the complete process have thus been able to reproduce for the first time the main properties of asteroid families, each formed by the disruption of a large parent body, and also to derive some information on the possible internal structure of the parent bodies. A large amount of work remains however necessary to understand in deeper details the physical process as a function of material properties that are relevant to asteroids and to determine in a more quantitative way the outcome properties such as fragments’ shapes and rotational states. More... »

PAGES

117-143

Book

TITLE

Dynamics of Extended Celestial Bodies and Rings

ISBN

978-3-540-28024-8
978-3-540-32455-3

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/3-540-32455-0_5

DOI

http://dx.doi.org/10.1007/3-540-32455-0_5

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1004150688


Indexing Status Check whether this publication has been indexed by Scopus and Web Of Science using the SN Indexing Status Tool
Incoming Citations Browse incoming citations for this publication using opencitations.net

JSON-LD is the canonical representation for SciGraph data.

TIP: You can open this SciGraph record using an external JSON-LD service: JSON-LD Playground Google SDTT

[
  {
    "@context": "https://springernature.github.io/scigraph/jsonld/sgcontext.json", 
    "about": [
      {
        "id": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/02", 
        "inDefinedTermSet": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/", 
        "name": "Physical Sciences", 
        "type": "DefinedTerm"
      }, 
      {
        "id": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/0202", 
        "inDefinedTermSet": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/", 
        "name": "Atomic, Molecular, Nuclear, Particle and Plasma Physics", 
        "type": "DefinedTerm"
      }
    ], 
    "author": [
      {
        "affiliation": {
          "alternateName": "Observatoire de la C\u2019te d\u2019Azur, UMR 6529 Cassini/CNRS, 06304 Nice cedex 4, 4229, France", 
          "id": "http://www.grid.ac/institutes/None", 
          "name": [
            "Observatoire de la C\u2019te d\u2019Azur, UMR 6529 Cassini/CNRS, 06304 Nice cedex 4, 4229, France"
          ], 
          "type": "Organization"
        }, 
        "familyName": "Michel", 
        "givenName": "Patrick", 
        "id": "sg:person.014600122327.15", 
        "sameAs": [
          "https://app.dimensions.ai/discover/publication?and_facet_researcher=ur.014600122327.15"
        ], 
        "type": "Person"
      }
    ], 
    "datePublished": "2006", 
    "datePublishedReg": "2006-01-01", 
    "description": "Thanks to the development of sophisticated numerical codes, a major breakthrough has been achieved in our understanding of the process involved in small body collisions. Such events play a fundamental role in all the stages of the formation and evolution of planetary systems, and more particularly of our Solar System. Laboratory experiments on centimeter-sized targets have been performed to improve our knowledge on this process, but their extrapolation to asteroid scales remains confronted to major diffculties. In this lecture, we present a brief review of our current understanding of the fragmentation process of solid bodies and its implementation in numerical codes aimed at simulating asteroid break-up events. The most recent results provided by numerical simulations are also presented. Although our current understanding is still based on several limitations and assumptions, the development of sophisticated numerical codes accounting for the fragmentation of an asteroid and for the gravitational interactions of the generated fragments have allowed to improve greatly our knowledge on the main mechanisms that are at the origin of some observed features in the asteroid belt. In particular, the simulations have demonstrated that, for bodies larger than several kilometers, the collisional process does not only involves the fragmentation of the asteroid but also the gravitational interactions between the fragments that are ejected. This latter mechanism can lead to the formation of large agregates by gravitational reaccumulation of smaller fragments, allowing to explain the presence of large members within asteroid families. Numerical simulations of the complete process have thus been able to reproduce for the first time the main properties of asteroid families, each formed by the disruption of a large parent body, and also to derive some information on the possible internal structure of the parent bodies. A large amount of work remains however necessary to understand in deeper details the physical process as a function of material properties that are relevant to asteroids and to determine in a more quantitative way the outcome properties such as fragments\u2019 shapes and rotational states.", 
    "editor": [
      {
        "familyName": "Souchay", 
        "givenName": "Jean", 
        "type": "Person"
      }
    ], 
    "genre": "chapter", 
    "id": "sg:pub.10.1007/3-540-32455-0_5", 
    "inLanguage": "en", 
    "isAccessibleForFree": false, 
    "isPartOf": {
      "isbn": [
        "978-3-540-28024-8", 
        "978-3-540-32455-3"
      ], 
      "name": "Dynamics of Extended Celestial Bodies and Rings", 
      "type": "Book"
    }, 
    "keywords": [
      "sophisticated numerical codes", 
      "numerical code", 
      "numerical simulations", 
      "parent body", 
      "solar system", 
      "laboratory experiments", 
      "solid body", 
      "asteroid break", 
      "simulations", 
      "asteroid belt", 
      "collisional processes", 
      "complete process", 
      "large parent body", 
      "physical processes", 
      "material properties", 
      "process", 
      "body collisions", 
      "collisions", 
      "such events", 
      "events", 
      "planetary systems", 
      "experiments", 
      "current understanding", 
      "fragmentation process", 
      "asteroids", 
      "gravitational interaction", 
      "main mechanism", 
      "observed features", 
      "belt", 
      "kilometers", 
      "latter mechanism", 
      "gravitational reaccumulation", 
      "largest member", 
      "asteroid families", 
      "main properties", 
      "properties", 
      "possible internal structure", 
      "internal structure", 
      "large amount", 
      "outcome properties", 
      "thanks", 
      "development", 
      "code", 
      "major breakthrough", 
      "breakthrough", 
      "understanding", 
      "fundamental role", 
      "stage", 
      "formation", 
      "evolution", 
      "system", 
      "extrapolation", 
      "scale", 
      "brief review", 
      "body", 
      "implementation", 
      "breaks", 
      "recent results", 
      "results", 
      "limitations", 
      "assumption", 
      "interaction", 
      "fragments", 
      "mechanism", 
      "origin", 
      "features", 
      "agregates", 
      "small fragments", 
      "first time", 
      "time", 
      "structure", 
      "amount", 
      "work", 
      "deeper detail", 
      "detail", 
      "quantitative way", 
      "shape", 
      "rotational states", 
      "role", 
      "target", 
      "knowledge", 
      "diffculties", 
      "review", 
      "fragmentation", 
      "reaccumulation", 
      "presence", 
      "members", 
      "disruption", 
      "information", 
      "function", 
      "way", 
      "state", 
      "lectures", 
      "family", 
      "small body collisions", 
      "centimeter-sized targets", 
      "major diffculties", 
      "large agregates"
    ], 
    "name": "Modelling Collisions Between Asteroids: From Laboratory Experiments to Numerical Simulations", 
    "pagination": "117-143", 
    "productId": [
      {
        "name": "dimensions_id", 
        "type": "PropertyValue", 
        "value": [
          "pub.1004150688"
        ]
      }, 
      {
        "name": "doi", 
        "type": "PropertyValue", 
        "value": [
          "10.1007/3-540-32455-0_5"
        ]
      }
    ], 
    "publisher": {
      "name": "Springer Nature", 
      "type": "Organisation"
    }, 
    "sameAs": [
      "https://doi.org/10.1007/3-540-32455-0_5", 
      "https://app.dimensions.ai/details/publication/pub.1004150688"
    ], 
    "sdDataset": "chapters", 
    "sdDatePublished": "2022-01-01T19:07", 
    "sdLicense": "https://scigraph.springernature.com/explorer/license/", 
    "sdPublisher": {
      "name": "Springer Nature - SN SciGraph project", 
      "type": "Organization"
    }, 
    "sdSource": "s3://com-springernature-scigraph/baseset/20220101/entities/gbq_results/chapter/chapter_116.jsonl", 
    "type": "Chapter", 
    "url": "https://doi.org/10.1007/3-540-32455-0_5"
  }
]
 

Download the RDF metadata as:  json-ld nt turtle xml License info

HOW TO GET THIS DATA PROGRAMMATICALLY:

JSON-LD is a popular format for linked data which is fully compatible with JSON.

curl -H 'Accept: application/ld+json' 'https://scigraph.springernature.com/pub.10.1007/3-540-32455-0_5'

N-Triples is a line-based linked data format ideal for batch operations.

curl -H 'Accept: application/n-triples' 'https://scigraph.springernature.com/pub.10.1007/3-540-32455-0_5'

Turtle is a human-readable linked data format.

curl -H 'Accept: text/turtle' 'https://scigraph.springernature.com/pub.10.1007/3-540-32455-0_5'

RDF/XML is a standard XML format for linked data.

curl -H 'Accept: application/rdf+xml' 'https://scigraph.springernature.com/pub.10.1007/3-540-32455-0_5'


 

This table displays all metadata directly associated to this object as RDF triples.

158 TRIPLES      23 PREDICATES      124 URIs      117 LITERALS      7 BLANK NODES

Subject Predicate Object
1 sg:pub.10.1007/3-540-32455-0_5 schema:about anzsrc-for:02
2 anzsrc-for:0202
3 schema:author Nfc1f416ce3d545dc829f9f4c5191a7ed
4 schema:datePublished 2006
5 schema:datePublishedReg 2006-01-01
6 schema:description Thanks to the development of sophisticated numerical codes, a major breakthrough has been achieved in our understanding of the process involved in small body collisions. Such events play a fundamental role in all the stages of the formation and evolution of planetary systems, and more particularly of our Solar System. Laboratory experiments on centimeter-sized targets have been performed to improve our knowledge on this process, but their extrapolation to asteroid scales remains confronted to major diffculties. In this lecture, we present a brief review of our current understanding of the fragmentation process of solid bodies and its implementation in numerical codes aimed at simulating asteroid break-up events. The most recent results provided by numerical simulations are also presented. Although our current understanding is still based on several limitations and assumptions, the development of sophisticated numerical codes accounting for the fragmentation of an asteroid and for the gravitational interactions of the generated fragments have allowed to improve greatly our knowledge on the main mechanisms that are at the origin of some observed features in the asteroid belt. In particular, the simulations have demonstrated that, for bodies larger than several kilometers, the collisional process does not only involves the fragmentation of the asteroid but also the gravitational interactions between the fragments that are ejected. This latter mechanism can lead to the formation of large agregates by gravitational reaccumulation of smaller fragments, allowing to explain the presence of large members within asteroid families. Numerical simulations of the complete process have thus been able to reproduce for the first time the main properties of asteroid families, each formed by the disruption of a large parent body, and also to derive some information on the possible internal structure of the parent bodies. A large amount of work remains however necessary to understand in deeper details the physical process as a function of material properties that are relevant to asteroids and to determine in a more quantitative way the outcome properties such as fragments’ shapes and rotational states.
7 schema:editor N582f9eee099e413baea4483178fe4e5d
8 schema:genre chapter
9 schema:inLanguage en
10 schema:isAccessibleForFree false
11 schema:isPartOf Nd453f080147e4212ae386cc5bd88d091
12 schema:keywords agregates
13 amount
14 assumption
15 asteroid belt
16 asteroid break
17 asteroid families
18 asteroids
19 belt
20 body
21 body collisions
22 breaks
23 breakthrough
24 brief review
25 centimeter-sized targets
26 code
27 collisional processes
28 collisions
29 complete process
30 current understanding
31 deeper detail
32 detail
33 development
34 diffculties
35 disruption
36 events
37 evolution
38 experiments
39 extrapolation
40 family
41 features
42 first time
43 formation
44 fragmentation
45 fragmentation process
46 fragments
47 function
48 fundamental role
49 gravitational interaction
50 gravitational reaccumulation
51 implementation
52 information
53 interaction
54 internal structure
55 kilometers
56 knowledge
57 laboratory experiments
58 large agregates
59 large amount
60 large parent body
61 largest member
62 latter mechanism
63 lectures
64 limitations
65 main mechanism
66 main properties
67 major breakthrough
68 major diffculties
69 material properties
70 mechanism
71 members
72 numerical code
73 numerical simulations
74 observed features
75 origin
76 outcome properties
77 parent body
78 physical processes
79 planetary systems
80 possible internal structure
81 presence
82 process
83 properties
84 quantitative way
85 reaccumulation
86 recent results
87 results
88 review
89 role
90 rotational states
91 scale
92 shape
93 simulations
94 small body collisions
95 small fragments
96 solar system
97 solid body
98 sophisticated numerical codes
99 stage
100 state
101 structure
102 such events
103 system
104 target
105 thanks
106 time
107 understanding
108 way
109 work
110 schema:name Modelling Collisions Between Asteroids: From Laboratory Experiments to Numerical Simulations
111 schema:pagination 117-143
112 schema:productId N180125777e8342ee8f52f0d3c6b5c048
113 N1cd98e3f080c41dba49ad2409b1a6b5c
114 schema:publisher N7fa64540cc734fa8bf12fc2cfd4be766
115 schema:sameAs https://app.dimensions.ai/details/publication/pub.1004150688
116 https://doi.org/10.1007/3-540-32455-0_5
117 schema:sdDatePublished 2022-01-01T19:07
118 schema:sdLicense https://scigraph.springernature.com/explorer/license/
119 schema:sdPublisher N2412f56f7c734ffbabe428babea8cd12
120 schema:url https://doi.org/10.1007/3-540-32455-0_5
121 sgo:license sg:explorer/license/
122 sgo:sdDataset chapters
123 rdf:type schema:Chapter
124 N180125777e8342ee8f52f0d3c6b5c048 schema:name dimensions_id
125 schema:value pub.1004150688
126 rdf:type schema:PropertyValue
127 N1cd98e3f080c41dba49ad2409b1a6b5c schema:name doi
128 schema:value 10.1007/3-540-32455-0_5
129 rdf:type schema:PropertyValue
130 N2412f56f7c734ffbabe428babea8cd12 schema:name Springer Nature - SN SciGraph project
131 rdf:type schema:Organization
132 N582f9eee099e413baea4483178fe4e5d rdf:first Nd54f4f4c524346139d5000b3bdf30ce1
133 rdf:rest rdf:nil
134 N7fa64540cc734fa8bf12fc2cfd4be766 schema:name Springer Nature
135 rdf:type schema:Organisation
136 Nd453f080147e4212ae386cc5bd88d091 schema:isbn 978-3-540-28024-8
137 978-3-540-32455-3
138 schema:name Dynamics of Extended Celestial Bodies and Rings
139 rdf:type schema:Book
140 Nd54f4f4c524346139d5000b3bdf30ce1 schema:familyName Souchay
141 schema:givenName Jean
142 rdf:type schema:Person
143 Nfc1f416ce3d545dc829f9f4c5191a7ed rdf:first sg:person.014600122327.15
144 rdf:rest rdf:nil
145 anzsrc-for:02 schema:inDefinedTermSet anzsrc-for:
146 schema:name Physical Sciences
147 rdf:type schema:DefinedTerm
148 anzsrc-for:0202 schema:inDefinedTermSet anzsrc-for:
149 schema:name Atomic, Molecular, Nuclear, Particle and Plasma Physics
150 rdf:type schema:DefinedTerm
151 sg:person.014600122327.15 schema:affiliation grid-institutes:None
152 schema:familyName Michel
153 schema:givenName Patrick
154 schema:sameAs https://app.dimensions.ai/discover/publication?and_facet_researcher=ur.014600122327.15
155 rdf:type schema:Person
156 grid-institutes:None schema:alternateName Observatoire de la C’te d’Azur, UMR 6529 Cassini/CNRS, 06304 Nice cedex 4, 4229, France
157 schema:name Observatoire de la C’te d’Azur, UMR 6529 Cassini/CNRS, 06304 Nice cedex 4, 4229, France
158 rdf:type schema:Organization
 




Preview window. Press ESC to close (or click here)


...