The trans-Neptunian object size distribution at small sizes

Autores
Gil Hutton, Ricardo Alfredo; Licandro, J.; Pinilla Alonso, N.; Brunetto, R.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. The aim. of this work, is to estimate the size distribution of small Trans-Neptunian objects. Methods. We simulate the irradiation and collisional processes affecting the surface of a Trans-Neptunian object for the first time using as a constraint the peculiar crystalline to amorphous water ice ratio observed on (136108) 2003 ELa. Results. We find that the size distribution changes its exponent from q0 = 4.2 at larger sizes to q1 = 2.40 ± 0.3 at the smaller ones, with a break, radius of r1 = 35 ± 15 km. If this size distribution is applied to studying the collisional surface evolution of (1361.08) 2003 EL61, we find that the object must be covered by a thin ice crust of ≈0.12 cm, while the original, composition of the object is still present at 1.61 cm or more below the surface. This result is not affected by a collision with a large projectile that occurred by chance more than 109 yr ago since after a short time the mean value obtained for the crystalline to amorphous water ice ratio is indistinguishable from the one obtained without a collision with a large projectile. Since the simulations are not sensitive to the effects of very small projectiles (rp < 10-30 m), it is possible that the exponent of the size distribution for these very small, objects changes again, approaching a Donhanyi's size distribution.
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina
Fil: Licandro, J.. Instituto de Astrofísica de Canarias; España
Fil: Pinilla Alonso, N.. Fundación Galileo Galilei & Telescopio Nazionale Galileo; España
Fil: Brunetto, R.. Université Paris-Sud; Francia
Materia
ASTROCHEMISTRY -
KUIPER BELT -
METHODS, NUMERICAL
SOLAR SYSTEM, FORMATION -
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/213848
Acceder
id CONICETDig_c2ad347779c1f0f2e7aed666dabab2b0
oai_identifier_str oai:ri.conicet.gov.ar:11336/213848
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The trans-Neptunian object size distribution at small sizesGil Hutton, Ricardo AlfredoLicandro, J.Pinilla Alonso, N.Brunetto, R.ASTROCHEMISTRY -KUIPER BELT -METHODS, NUMERICALSOLAR SYSTEM, FORMATION -https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. The aim. of this work, is to estimate the size distribution of small Trans-Neptunian objects. Methods. We simulate the irradiation and collisional processes affecting the surface of a Trans-Neptunian object for the first time using as a constraint the peculiar crystalline to amorphous water ice ratio observed on (136108) 2003 ELa. Results. We find that the size distribution changes its exponent from q0 = 4.2 at larger sizes to q1 = 2.40 ± 0.3 at the smaller ones, with a break, radius of r1 = 35 ± 15 km. If this size distribution is applied to studying the collisional surface evolution of (1361.08) 2003 EL61, we find that the object must be covered by a thin ice crust of ≈0.12 cm, while the original, composition of the object is still present at 1.61 cm or more below the surface. This result is not affected by a collision with a large projectile that occurred by chance more than 109 yr ago since after a short time the mean value obtained for the crystalline to amorphous water ice ratio is indistinguishable from the one obtained without a collision with a large projectile. Since the simulations are not sensitive to the effects of very small projectiles (rp < 10-30 m), it is possible that the exponent of the size distribution for these very small, objects changes again, approaching a Donhanyi's size distribution.Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; ArgentinaFil: Licandro, J.. Instituto de Astrofísica de Canarias; EspañaFil: Pinilla Alonso, N.. Fundación Galileo Galilei & Telescopio Nazionale Galileo; EspañaFil: Brunetto, R.. Université Paris-Sud; FranciaEDP Sciences2009-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/213848Gil Hutton, Ricardo Alfredo; Licandro, J.; Pinilla Alonso, N.; Brunetto, R.; The trans-Neptunian object size distribution at small sizes; EDP Sciences; Astronomy and Astrophysics; 500; 2; 6-2009; 909-9160004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200811301info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2009/23/aa11301-08/aa11301-08.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:36:44Zoai:ri.conicet.gov.ar:11336/213848instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:36:44.788CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The trans-Neptunian object size distribution at small sizes
title The trans-Neptunian object size distribution at small sizes
spellingShingle The trans-Neptunian object size distribution at small sizes
Gil Hutton, Ricardo Alfredo
ASTROCHEMISTRY -
KUIPER BELT -
METHODS, NUMERICAL
SOLAR SYSTEM, FORMATION -
title_short The trans-Neptunian object size distribution at small sizes
title_full The trans-Neptunian object size distribution at small sizes
title_fullStr The trans-Neptunian object size distribution at small sizes
title_full_unstemmed The trans-Neptunian object size distribution at small sizes
title_sort The trans-Neptunian object size distribution at small sizes
dc.creator.none.fl_str_mv Gil Hutton, Ricardo Alfredo
Licandro, J.
Pinilla Alonso, N.
Brunetto, R.
author Gil Hutton, Ricardo Alfredo
author_facet Gil Hutton, Ricardo Alfredo
Licandro, J.
Pinilla Alonso, N.
Brunetto, R.
author_role author
author2 Licandro, J.
Pinilla Alonso, N.
Brunetto, R.
author2_role author
author
author
dc.subject.none.fl_str_mv ASTROCHEMISTRY -
KUIPER BELT -
METHODS, NUMERICAL
SOLAR SYSTEM, FORMATION -
topic ASTROCHEMISTRY -
KUIPER BELT -
METHODS, NUMERICAL
SOLAR SYSTEM, FORMATION -
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. The aim. of this work, is to estimate the size distribution of small Trans-Neptunian objects. Methods. We simulate the irradiation and collisional processes affecting the surface of a Trans-Neptunian object for the first time using as a constraint the peculiar crystalline to amorphous water ice ratio observed on (136108) 2003 ELa. Results. We find that the size distribution changes its exponent from q0 = 4.2 at larger sizes to q1 = 2.40 ± 0.3 at the smaller ones, with a break, radius of r1 = 35 ± 15 km. If this size distribution is applied to studying the collisional surface evolution of (1361.08) 2003 EL61, we find that the object must be covered by a thin ice crust of ≈0.12 cm, while the original, composition of the object is still present at 1.61 cm or more below the surface. This result is not affected by a collision with a large projectile that occurred by chance more than 109 yr ago since after a short time the mean value obtained for the crystalline to amorphous water ice ratio is indistinguishable from the one obtained without a collision with a large projectile. Since the simulations are not sensitive to the effects of very small projectiles (rp < 10-30 m), it is possible that the exponent of the size distribution for these very small, objects changes again, approaching a Donhanyi's size distribution.
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina
Fil: Licandro, J.. Instituto de Astrofísica de Canarias; España
Fil: Pinilla Alonso, N.. Fundación Galileo Galilei & Telescopio Nazionale Galileo; España
Fil: Brunetto, R.. Université Paris-Sud; Francia
description Aims. The aim. of this work, is to estimate the size distribution of small Trans-Neptunian objects. Methods. We simulate the irradiation and collisional processes affecting the surface of a Trans-Neptunian object for the first time using as a constraint the peculiar crystalline to amorphous water ice ratio observed on (136108) 2003 ELa. Results. We find that the size distribution changes its exponent from q0 = 4.2 at larger sizes to q1 = 2.40 ± 0.3 at the smaller ones, with a break, radius of r1 = 35 ± 15 km. If this size distribution is applied to studying the collisional surface evolution of (1361.08) 2003 EL61, we find that the object must be covered by a thin ice crust of ≈0.12 cm, while the original, composition of the object is still present at 1.61 cm or more below the surface. This result is not affected by a collision with a large projectile that occurred by chance more than 109 yr ago since after a short time the mean value obtained for the crystalline to amorphous water ice ratio is indistinguishable from the one obtained without a collision with a large projectile. Since the simulations are not sensitive to the effects of very small projectiles (rp < 10-30 m), it is possible that the exponent of the size distribution for these very small, objects changes again, approaching a Donhanyi's size distribution.
publishDate 2009
dc.date.none.fl_str_mv 2009-06
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/213848
Gil Hutton, Ricardo Alfredo; Licandro, J.; Pinilla Alonso, N.; Brunetto, R.; The trans-Neptunian object size distribution at small sizes; EDP Sciences; Astronomy and Astrophysics; 500; 2; 6-2009; 909-916
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/213848
identifier_str_mv Gil Hutton, Ricardo Alfredo; Licandro, J.; Pinilla Alonso, N.; Brunetto, R.; The trans-Neptunian object size distribution at small sizes; EDP Sciences; Astronomy and Astrophysics; 500; 2; 6-2009; 909-916
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200811301
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2009/23/aa11301-08/aa11301-08.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1846782010194919424
score 12.982451

Publicaciones similares