Cratering rate on Pluto produced by the inner trans-Neptunian population
- Autores
- Calandra, María Florencia; Gil-Hutton, Ricardo
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Kuiper belt: General
Methods: Numerical
Planets and satellites: General - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/87357
Ver los metadatos del registro completo
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Cratering rate on Pluto produced by the inner trans-Neptunian populationCalandra, María FlorenciaGil-Hutton, RicardoCiencias AstronómicasKuiper belt: GeneralMethods: NumericalPlanets and satellites: GeneralAims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.Facultad de Ciencias Astronómicas y Geofísicas2017info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/87357enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628930info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:17:14Zoai:sedici.unlp.edu.ar:10915/87357Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:17:15.088SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
title |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
spellingShingle |
Cratering rate on Pluto produced by the inner trans-Neptunian population Calandra, María Florencia Ciencias Astronómicas Kuiper belt: General Methods: Numerical Planets and satellites: General |
title_short |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
title_full |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
title_fullStr |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
title_full_unstemmed |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
title_sort |
Cratering rate on Pluto produced by the inner trans-Neptunian population |
dc.creator.none.fl_str_mv |
Calandra, María Florencia Gil-Hutton, Ricardo |
author |
Calandra, María Florencia |
author_facet |
Calandra, María Florencia Gil-Hutton, Ricardo |
author_role |
author |
author2 |
Gil-Hutton, Ricardo |
author2_role |
author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Kuiper belt: General Methods: Numerical Planets and satellites: General |
topic |
Ciencias Astronómicas Kuiper belt: General Methods: Numerical Planets and satellites: General |
dc.description.none.fl_txt_mv |
Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence. Facultad de Ciencias Astronómicas y Geofísicas |
description |
Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence. |
publishDate |
2017 |
dc.date.none.fl_str_mv |
2017 |
dc.type.none.fl_str_mv |
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article |
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publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/87357 |
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http://sedici.unlp.edu.ar/handle/10915/87357 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628930 |
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