On the Strength and Disruption Mechanisms of Small Bodies in the Solar System View Full Text


Ontology type: schema:Chapter     


Chapter Info

DATE

2008-08-05

AUTHORS

P. Michel

ABSTRACT

During their evolutions, the small bodies of our Solar System are affected by several mechanisms which can modify their properties. While dynamical mechanisms are at the origin of their orbital variations, there are other mechanisms which can change their shape, spin, and even their size when their strength threshold is reached, resulting in their disruption. Such mechanisms have been identified and studied, by both analytical and numerical tools. The main mechanisms that can result in the disruption of a small body are collisional events, tidal perturbations, and spin-ups. However, the efficiency of these mechanisms depends on the strength of the material constituing the small body, which also plays a role in its possible equilibrium shape. As it is often believed that most small bodies larger than a few hundreds meters in radius are gravitational aggregates or rubble piles, i.e., cohesionless bodies, a fluid model is often used to determine their bulk densities, based on their shape and assuming hydrostatic equilibrium. A representation by a fluid has also been often used to estimate their tidal disruption (Roche) distance to a planet. However, cohesionless bodies do not behave like fluids. In particular, they are subjected to different failure criteria depending on the supposed strength model. This chapter presents several important aspects of material strengths that are believed to be adapted to Solar System small bodies and reviews the most recent studies of the different mechanisms that can be at the origin of the disruption of these bodies. Our understanding of the complex process of rock failure is still poor and remains an open area of research. While our knowledge has improved on the disruption mechanisms of small bodies of our Solar System, there is still a large debate on the appropriate strength models for these bodies. Moreover, material properties of terrestrial rocks or meteorites are generally used to model small bodies in space, and only space missions to some of these bodies devoted to precise in situ analysis and sample return will allow us to determine whether those models are appropriate or need to be revised. More... »

PAGES

1-30

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-3-540-76935-4_4

DOI

http://dx.doi.org/10.1007/978-3-540-76935-4_4

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1043606661


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/2008/09", 
        "inDefinedTermSet": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/", 
        "name": "Engineering", 
        "type": "DefinedTerm"
      }, 
      {
        "id": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/0912", 
        "inDefinedTermSet": "http://purl.org/au-research/vocabulary/anzsrc-for/2008/", 
        "name": "Materials Engineering", 
        "type": "DefinedTerm"
      }
    ], 
    "author": [
      {
        "affiliation": {
          "alternateName": "Laboratoire Cassiop\u00e9e, Observatoire de la C\u00f4te d\u2019Azur, CNRS, Universit\u00e9 de Nice Sophia-Antipolis, boulevard de l\u2019Observatoire, 06300 Nice, France", 
          "id": "http://www.grid.ac/institutes/grid.440460.2", 
          "name": [
            "Laboratoire Cassiop\u00e9e, Observatoire de la C\u00f4te d\u2019Azur, CNRS, Universit\u00e9 de Nice Sophia-Antipolis, boulevard de l\u2019Observatoire, 06300 Nice, France"
          ], 
          "type": "Organization"
        }, 
        "familyName": "Michel", 
        "givenName": "P.", 
        "id": "sg:person.014600122327.15", 
        "sameAs": [
          "https://app.dimensions.ai/discover/publication?and_facet_researcher=ur.014600122327.15"
        ], 
        "type": "Person"
      }
    ], 
    "datePublished": "2008-08-05", 
    "datePublishedReg": "2008-08-05", 
    "description": "During their evolutions, the small bodies of our Solar System are affected by several mechanisms which can modify their properties. While dynamical mechanisms are at the origin of their orbital variations, there are other mechanisms which can change their shape, spin, and even their size when their strength threshold is reached, resulting in their disruption. Such mechanisms have been identified and studied, by both analytical and numerical tools. The main mechanisms that can result in the disruption of a small body are collisional events, tidal perturbations, and spin-ups. However, the efficiency of these mechanisms depends on the strength of the material constituing the small body, which also plays a role in its possible equilibrium shape. As it is often believed that most small bodies larger than a few hundreds meters in radius are gravitational aggregates or rubble piles, i.e., cohesionless bodies, a fluid model is often used to determine their bulk densities, based on their shape and assuming hydrostatic equilibrium. A representation by a fluid has also been often used to estimate their tidal disruption (Roche) distance to a planet. However, cohesionless bodies do not behave like fluids. In particular, they are subjected to different failure criteria depending on the supposed strength model. This chapter presents several important aspects of material strengths that are believed to be adapted to Solar System small bodies and reviews the most recent studies of the different mechanisms that can be at the origin of the disruption of these bodies. Our understanding of the complex process of rock failure is still poor and remains an open area of research. While our knowledge has improved on the disruption mechanisms of small bodies of our Solar System, there is still a large debate on the appropriate strength models for these bodies. Moreover, material properties of terrestrial rocks or meteorites are generally used to model small bodies in space, and only space missions to some of these bodies devoted to precise in situ analysis and sample return will allow us to determine whether those models are appropriate or need to be revised.", 
    "editor": [
      {
        "familyName": "Mann", 
        "givenName": "Ingrid", 
        "type": "Person"
      }, 
      {
        "familyName": "Nakamura", 
        "givenName": "Akiko", 
        "type": "Person"
      }, 
      {
        "familyName": "Mukai", 
        "givenName": "Tadashi", 
        "type": "Person"
      }
    ], 
    "genre": "chapter", 
    "id": "sg:pub.10.1007/978-3-540-76935-4_4", 
    "inLanguage": "en", 
    "isAccessibleForFree": false, 
    "isPartOf": {
      "isbn": [
        "978-3-540-76934-7", 
        "978-3-540-76935-4"
      ], 
      "name": "Small Bodies in Planetary Systems", 
      "type": "Book"
    }, 
    "keywords": [
      "dynamical mechanisms", 
      "numerical tool", 
      "fluid model", 
      "possible equilibrium shapes", 
      "Solar System small bodies", 
      "strength model", 
      "tidal perturbations", 
      "different failure criteria", 
      "model", 
      "hydrostatic equilibrium", 
      "material strength", 
      "rock failure", 
      "system", 
      "failure criterion", 
      "material properties", 
      "solar system", 
      "strength threshold", 
      "perturbations", 
      "space", 
      "bulk density", 
      "representation", 
      "hundreds meters", 
      "space missions", 
      "small bodies", 
      "strength", 
      "rubble piles", 
      "equilibrium", 
      "properties", 
      "equilibrium shape", 
      "important aspect", 
      "sample return", 
      "main mechanism", 
      "complex process", 
      "shape", 
      "tool", 
      "efficiency", 
      "fluid", 
      "criteria", 
      "disruption mechanism", 
      "situ analysis", 
      "piles", 
      "orbital variations", 
      "spin", 
      "materials", 
      "meters", 
      "chapter", 
      "evolution", 
      "radius", 
      "open areas", 
      "analysis", 
      "such mechanisms", 
      "density", 
      "distance", 
      "process", 
      "mission", 
      "threshold", 
      "aggregates", 
      "body", 
      "mechanism", 
      "size", 
      "aspects", 
      "rocks", 
      "variation", 
      "return", 
      "planets", 
      "failure", 
      "area", 
      "research", 
      "knowledge", 
      "origin", 
      "collisional event", 
      "different mechanisms", 
      "study", 
      "understanding", 
      "events", 
      "Recent studies", 
      "disruption", 
      "role", 
      "gravitational aggregates", 
      "terrestrial rocks", 
      "meteorites", 
      "debate", 
      "larger debate", 
      "most small bodies", 
      "cohesionless bodies", 
      "tidal disruption (Roche) distance", 
      "disruption (Roche) distance", 
      "System small bodies", 
      "appropriate strength models", 
      "only space missions"
    ], 
    "name": "On the Strength and Disruption Mechanisms of Small Bodies in the Solar System", 
    "pagination": "1-30", 
    "productId": [
      {
        "name": "dimensions_id", 
        "type": "PropertyValue", 
        "value": [
          "pub.1043606661"
        ]
      }, 
      {
        "name": "doi", 
        "type": "PropertyValue", 
        "value": [
          "10.1007/978-3-540-76935-4_4"
        ]
      }
    ], 
    "publisher": {
      "name": "Springer Nature", 
      "type": "Organisation"
    }, 
    "sameAs": [
      "https://doi.org/10.1007/978-3-540-76935-4_4", 
      "https://app.dimensions.ai/details/publication/pub.1043606661"
    ], 
    "sdDataset": "chapters", 
    "sdDatePublished": "2022-01-01T19:25", 
    "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_44.jsonl", 
    "type": "Chapter", 
    "url": "https://doi.org/10.1007/978-3-540-76935-4_4"
  }
]
 

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.10.1007/978-3-540-76935-4_4'

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

curl -H 'Accept: application/n-triples' 'https://scigraph.springernature.com/pub.10.1007/978-3-540-76935-4_4'

Turtle is a human-readable linked data format.

curl -H 'Accept: text/turtle' 'https://scigraph.springernature.com/pub.10.1007/978-3-540-76935-4_4'

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

curl -H 'Accept: application/rdf+xml' 'https://scigraph.springernature.com/pub.10.1007/978-3-540-76935-4_4'


 

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

160 TRIPLES      23 PREDICATES      114 URIs      107 LITERALS      7 BLANK NODES

Subject Predicate Object
1 sg:pub.10.1007/978-3-540-76935-4_4 schema:about anzsrc-for:09
2 anzsrc-for:0912
3 schema:author Nddfb855d79fe4bb0ae9c6f8f823e1b4a
4 schema:datePublished 2008-08-05
5 schema:datePublishedReg 2008-08-05
6 schema:description During their evolutions, the small bodies of our Solar System are affected by several mechanisms which can modify their properties. While dynamical mechanisms are at the origin of their orbital variations, there are other mechanisms which can change their shape, spin, and even their size when their strength threshold is reached, resulting in their disruption. Such mechanisms have been identified and studied, by both analytical and numerical tools. The main mechanisms that can result in the disruption of a small body are collisional events, tidal perturbations, and spin-ups. However, the efficiency of these mechanisms depends on the strength of the material constituing the small body, which also plays a role in its possible equilibrium shape. As it is often believed that most small bodies larger than a few hundreds meters in radius are gravitational aggregates or rubble piles, i.e., cohesionless bodies, a fluid model is often used to determine their bulk densities, based on their shape and assuming hydrostatic equilibrium. A representation by a fluid has also been often used to estimate their tidal disruption (Roche) distance to a planet. However, cohesionless bodies do not behave like fluids. In particular, they are subjected to different failure criteria depending on the supposed strength model. This chapter presents several important aspects of material strengths that are believed to be adapted to Solar System small bodies and reviews the most recent studies of the different mechanisms that can be at the origin of the disruption of these bodies. Our understanding of the complex process of rock failure is still poor and remains an open area of research. While our knowledge has improved on the disruption mechanisms of small bodies of our Solar System, there is still a large debate on the appropriate strength models for these bodies. Moreover, material properties of terrestrial rocks or meteorites are generally used to model small bodies in space, and only space missions to some of these bodies devoted to precise in situ analysis and sample return will allow us to determine whether those models are appropriate or need to be revised.
7 schema:editor Na6033c9f9dd041a49a27928df05f314a
8 schema:genre chapter
9 schema:inLanguage en
10 schema:isAccessibleForFree false
11 schema:isPartOf N32f233603d4f45b88e6a48bf97c9a946
12 schema:keywords Recent studies
13 Solar System small bodies
14 System small bodies
15 aggregates
16 analysis
17 appropriate strength models
18 area
19 aspects
20 body
21 bulk density
22 chapter
23 cohesionless bodies
24 collisional event
25 complex process
26 criteria
27 debate
28 density
29 different failure criteria
30 different mechanisms
31 disruption
32 disruption (Roche) distance
33 disruption mechanism
34 distance
35 dynamical mechanisms
36 efficiency
37 equilibrium
38 equilibrium shape
39 events
40 evolution
41 failure
42 failure criterion
43 fluid
44 fluid model
45 gravitational aggregates
46 hundreds meters
47 hydrostatic equilibrium
48 important aspect
49 knowledge
50 larger debate
51 main mechanism
52 material properties
53 material strength
54 materials
55 mechanism
56 meteorites
57 meters
58 mission
59 model
60 most small bodies
61 numerical tool
62 only space missions
63 open areas
64 orbital variations
65 origin
66 perturbations
67 piles
68 planets
69 possible equilibrium shapes
70 process
71 properties
72 radius
73 representation
74 research
75 return
76 rock failure
77 rocks
78 role
79 rubble piles
80 sample return
81 shape
82 situ analysis
83 size
84 small bodies
85 solar system
86 space
87 space missions
88 spin
89 strength
90 strength model
91 strength threshold
92 study
93 such mechanisms
94 system
95 terrestrial rocks
96 threshold
97 tidal disruption (Roche) distance
98 tidal perturbations
99 tool
100 understanding
101 variation
102 schema:name On the Strength and Disruption Mechanisms of Small Bodies in the Solar System
103 schema:pagination 1-30
104 schema:productId Nb919a05f6ba44abfbc0e5c79448ffb39
105 Nc52fecda670140a6887ee79885e0f25a
106 schema:publisher N22135d2d8d0b461585c6bb3f5fed582f
107 schema:sameAs https://app.dimensions.ai/details/publication/pub.1043606661
108 https://doi.org/10.1007/978-3-540-76935-4_4
109 schema:sdDatePublished 2022-01-01T19:25
110 schema:sdLicense https://scigraph.springernature.com/explorer/license/
111 schema:sdPublisher N39a1ab9b5ceb4314878099d3dd584f13
112 schema:url https://doi.org/10.1007/978-3-540-76935-4_4
113 sgo:license sg:explorer/license/
114 sgo:sdDataset chapters
115 rdf:type schema:Chapter
116 N22135d2d8d0b461585c6bb3f5fed582f schema:name Springer Nature
117 rdf:type schema:Organisation
118 N32f233603d4f45b88e6a48bf97c9a946 schema:isbn 978-3-540-76934-7
119 978-3-540-76935-4
120 schema:name Small Bodies in Planetary Systems
121 rdf:type schema:Book
122 N39a1ab9b5ceb4314878099d3dd584f13 schema:name Springer Nature - SN SciGraph project
123 rdf:type schema:Organization
124 N49a8a2da75f74032a8a7ec3f25c24fdb schema:familyName Mann
125 schema:givenName Ingrid
126 rdf:type schema:Person
127 N54e50707fafc44c4886c58e2c707288c rdf:first Naa8a1979ac074211a81640e1e32868ed
128 rdf:rest rdf:nil
129 N6e50aca178514f648ed75792ab3d3630 schema:familyName Nakamura
130 schema:givenName Akiko
131 rdf:type schema:Person
132 N9224045a68c14369b8df8a7a6b40d18a rdf:first N6e50aca178514f648ed75792ab3d3630
133 rdf:rest N54e50707fafc44c4886c58e2c707288c
134 Na6033c9f9dd041a49a27928df05f314a rdf:first N49a8a2da75f74032a8a7ec3f25c24fdb
135 rdf:rest N9224045a68c14369b8df8a7a6b40d18a
136 Naa8a1979ac074211a81640e1e32868ed schema:familyName Mukai
137 schema:givenName Tadashi
138 rdf:type schema:Person
139 Nb919a05f6ba44abfbc0e5c79448ffb39 schema:name dimensions_id
140 schema:value pub.1043606661
141 rdf:type schema:PropertyValue
142 Nc52fecda670140a6887ee79885e0f25a schema:name doi
143 schema:value 10.1007/978-3-540-76935-4_4
144 rdf:type schema:PropertyValue
145 Nddfb855d79fe4bb0ae9c6f8f823e1b4a rdf:first sg:person.014600122327.15
146 rdf:rest rdf:nil
147 anzsrc-for:09 schema:inDefinedTermSet anzsrc-for:
148 schema:name Engineering
149 rdf:type schema:DefinedTerm
150 anzsrc-for:0912 schema:inDefinedTermSet anzsrc-for:
151 schema:name Materials Engineering
152 rdf:type schema:DefinedTerm
153 sg:person.014600122327.15 schema:affiliation grid-institutes:grid.440460.2
154 schema:familyName Michel
155 schema:givenName P.
156 schema:sameAs https://app.dimensions.ai/discover/publication?and_facet_researcher=ur.014600122327.15
157 rdf:type schema:Person
158 grid-institutes:grid.440460.2 schema:alternateName Laboratoire Cassiopée, Observatoire de la Côte d’Azur, CNRS, Université de Nice Sophia-Antipolis, boulevard de l’Observatoire, 06300 Nice, France
159 schema:name Laboratoire Cassiopée, Observatoire de la Côte d’Azur, CNRS, Université de Nice Sophia-Antipolis, boulevard de l’Observatoire, 06300 Nice, France
160 rdf:type schema:Organization
 




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


...