A further analysis for galactic dark matter halos with pressure

Autores
Aceña, Andrés Esteban; Barranco, Juan; Bernal, Argelia; López, Ericson; Llerena, Mario
Año de publicación
2021
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Spherically symmetric and static dark matter halos in hydrostatic equilibrium demand that dark matter should have an effective pressure that compensates the gravitational force of the mass of the halo. An effective equation of state can be obtained for each rotational velocity profile of the stars in galaxies. In this work, we study one of this dark matter equation of state obtained for the Universal Velocity Profile and analyze the properties of the self-gravitating structures that emerges from this equation of state. The resulting configurations explaining the observed rotational speeds are found to be unstable. We conclude that either the halo is not in hydrostatic equilibrium,or it is non spherically symmetric, or it is not static if the Universal Velocity profile should be valid to fit the rotational velocity curve of the galaxies.
Fil: Aceña, Andrés Esteban. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; Argentina
Fil: Barranco, Juan. Universidad de Guanajuato; México
Fil: Bernal, Argelia. Universidad de Guanajuato; México
Fil: López, Ericson. Escuela Politécnica Nacional; Ecuador
Fil: Llerena, Mario. Universidad de La Serena; Chile
Materia
DARK MATTER
GALACTIC HALO
EQUATION OF STAT
STABILITY
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:11336/212383
Acceder
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network_name_str CONICET Digital (CONICET)
spelling A further analysis for galactic dark matter halos with pressureAceña, Andrés EstebanBarranco, JuanBernal, ArgeliaLópez, EricsonLlerena, MarioDARK MATTERGALACTIC HALOEQUATION OF STATSTABILITYhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Spherically symmetric and static dark matter halos in hydrostatic equilibrium demand that dark matter should have an effective pressure that compensates the gravitational force of the mass of the halo. An effective equation of state can be obtained for each rotational velocity profile of the stars in galaxies. In this work, we study one of this dark matter equation of state obtained for the Universal Velocity Profile and analyze the properties of the self-gravitating structures that emerges from this equation of state. The resulting configurations explaining the observed rotational speeds are found to be unstable. We conclude that either the halo is not in hydrostatic equilibrium,or it is non spherically symmetric, or it is not static if the Universal Velocity profile should be valid to fit the rotational velocity curve of the galaxies.Fil: Aceña, Andrés Esteban. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; ArgentinaFil: Barranco, Juan. Universidad de Guanajuato; MéxicoFil: Bernal, Argelia. Universidad de Guanajuato; MéxicoFil: López, Ericson. Escuela Politécnica Nacional; EcuadorFil: Llerena, Mario. Universidad de La Serena; ChileCornell University2021-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/212383Aceña, Andrés Esteban; Barranco, Juan; Bernal, Argelia; López, Ericson; Llerena, Mario; A further analysis for galactic dark matter halos with pressure; Cornell University; ArXiv.org; 12-2021; 1-212331-8422CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2112.05865info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:47:43Zoai:ri.conicet.gov.ar:11336/212383instacron: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:34982025-09-03 09:47:43.594CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A further analysis for galactic dark matter halos with pressure
title A further analysis for galactic dark matter halos with pressure
spellingShingle A further analysis for galactic dark matter halos with pressure
Aceña, Andrés Esteban
DARK MATTER
GALACTIC HALO
EQUATION OF STAT
STABILITY
title_short A further analysis for galactic dark matter halos with pressure
title_full A further analysis for galactic dark matter halos with pressure
title_fullStr A further analysis for galactic dark matter halos with pressure
title_full_unstemmed A further analysis for galactic dark matter halos with pressure
title_sort A further analysis for galactic dark matter halos with pressure
dc.creator.none.fl_str_mv Aceña, Andrés Esteban
Barranco, Juan
Bernal, Argelia
López, Ericson
Llerena, Mario
author Aceña, Andrés Esteban
author_facet Aceña, Andrés Esteban
Barranco, Juan
Bernal, Argelia
López, Ericson
Llerena, Mario
author_role author
author2 Barranco, Juan
Bernal, Argelia
López, Ericson
Llerena, Mario
author2_role author
author
author
author
dc.subject.none.fl_str_mv DARK MATTER
GALACTIC HALO
EQUATION OF STAT
STABILITY
topic DARK MATTER
GALACTIC HALO
EQUATION OF STAT
STABILITY
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Spherically symmetric and static dark matter halos in hydrostatic equilibrium demand that dark matter should have an effective pressure that compensates the gravitational force of the mass of the halo. An effective equation of state can be obtained for each rotational velocity profile of the stars in galaxies. In this work, we study one of this dark matter equation of state obtained for the Universal Velocity Profile and analyze the properties of the self-gravitating structures that emerges from this equation of state. The resulting configurations explaining the observed rotational speeds are found to be unstable. We conclude that either the halo is not in hydrostatic equilibrium,or it is non spherically symmetric, or it is not static if the Universal Velocity profile should be valid to fit the rotational velocity curve of the galaxies.
Fil: Aceña, Andrés Esteban. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; Argentina
Fil: Barranco, Juan. Universidad de Guanajuato; México
Fil: Bernal, Argelia. Universidad de Guanajuato; México
Fil: López, Ericson. Escuela Politécnica Nacional; Ecuador
Fil: Llerena, Mario. Universidad de La Serena; Chile
description Spherically symmetric and static dark matter halos in hydrostatic equilibrium demand that dark matter should have an effective pressure that compensates the gravitational force of the mass of the halo. An effective equation of state can be obtained for each rotational velocity profile of the stars in galaxies. In this work, we study one of this dark matter equation of state obtained for the Universal Velocity Profile and analyze the properties of the self-gravitating structures that emerges from this equation of state. The resulting configurations explaining the observed rotational speeds are found to be unstable. We conclude that either the halo is not in hydrostatic equilibrium,or it is non spherically symmetric, or it is not static if the Universal Velocity profile should be valid to fit the rotational velocity curve of the galaxies.
publishDate 2021
dc.date.none.fl_str_mv 2021-12
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/11336/212383
Aceña, Andrés Esteban; Barranco, Juan; Bernal, Argelia; López, Ericson; Llerena, Mario; A further analysis for galactic dark matter halos with pressure; Cornell University; ArXiv.org; 12-2021; 1-21
2331-8422
CONICET Digital
CONICET
url http://hdl.handle.net/11336/212383
identifier_str_mv Aceña, Andrés Esteban; Barranco, Juan; Bernal, Argelia; López, Ericson; Llerena, Mario; A further analysis for galactic dark matter halos with pressure; Cornell University; ArXiv.org; 12-2021; 1-21
2331-8422
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2112.05865
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 Cornell University
publisher.none.fl_str_mv Cornell University
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_ 1842268876569575424
score 13.13397

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