The density-magnetic field relation in the atomic ISM

Autores
Gazol, A.; Villagran Azuara, Marco Adrian
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present numerical experiments aimed to study the correlation between the magnetic field strength, B, and the density, n, in the cold atomic interstellar medium (CNM). We analyse 24 magnetohydrodynamic models with different initial magnetic field intensities (B 0 = 0.4, 2.1, 4.2, and 8.3 μG) and/or mean densities (2, 3, and 4 cm -3 ), in the presence of driven and decaying turbulence, with and without self-gravity, in a cubic computational domain with 100 pc by side. Our main findings are as follows: (i) For forced simulations that reproduce the main observed physical conditions of the CNM in the solar neighbourhood, a positive correlation between B and n develops for all the B 0 values. (ii) The density at which this correlation becomes significant (≲30 cm -3 ) depends onB 0 but is not sensitive to the presence of self-gravity. (iii) The effect of self-gravity, when noticeable, consists of producing a shallower correlation at high densities, suggesting that, in the studied regime, self-gravity induces motions along the field lines. (iv) Self-gravitating decaying modelswhere theCNMis subsonic and sub- Alfvénic with β ≲ 1 develop a high-density positive correlation whose slopes are consistent with a constant β(n). (v) Decaying models where the low-density CNM is subsonic and sub- Alfvénic with β > 1 show a negative correlation at intermediate densities, followed by a high-density positive correlation.
Fil: Gazol, A.. Universidad Nacional Autónoma de México; México
Fil: Villagran Azuara, Marco Adrian. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Materia
ISM: STRUCTURE
LOCAL INTERSTELLAR MATTER
MHD- ISM: MAGNETIC FIELDS
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:11336/80566
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/80566
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The density-magnetic field relation in the atomic ISMGazol, A.Villagran Azuara, Marco AdrianISM: STRUCTURELOCAL INTERSTELLAR MATTERMHD- ISM: MAGNETIC FIELDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present numerical experiments aimed to study the correlation between the magnetic field strength, B, and the density, n, in the cold atomic interstellar medium (CNM). We analyse 24 magnetohydrodynamic models with different initial magnetic field intensities (B 0 = 0.4, 2.1, 4.2, and 8.3 μG) and/or mean densities (2, 3, and 4 cm -3 ), in the presence of driven and decaying turbulence, with and without self-gravity, in a cubic computational domain with 100 pc by side. Our main findings are as follows: (i) For forced simulations that reproduce the main observed physical conditions of the CNM in the solar neighbourhood, a positive correlation between B and n develops for all the B 0 values. (ii) The density at which this correlation becomes significant (≲30 cm -3 ) depends onB 0 but is not sensitive to the presence of self-gravity. (iii) The effect of self-gravity, when noticeable, consists of producing a shallower correlation at high densities, suggesting that, in the studied regime, self-gravity induces motions along the field lines. (iv) Self-gravitating decaying modelswhere theCNMis subsonic and sub- Alfvénic with β ≲ 1 develop a high-density positive correlation whose slopes are consistent with a constant β(n). (v) Decaying models where the low-density CNM is subsonic and sub- Alfvénic with β > 1 show a negative correlation at intermediate densities, followed by a high-density positive correlation.Fil: Gazol, A.. Universidad Nacional Autónoma de México; MéxicoFil: Villagran Azuara, Marco Adrian. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaWiley Blackwell Publishing, Inc2018-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/80566Gazol, A.; Villagran Azuara, Marco Adrian; The density-magnetic field relation in the atomic ISM; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 478; 1; 7-2018; 146-1540035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1041info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:07:28Zoai:ri.conicet.gov.ar:11336/80566instacron: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 11:07:29.035CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The density-magnetic field relation in the atomic ISM
title The density-magnetic field relation in the atomic ISM
spellingShingle The density-magnetic field relation in the atomic ISM
Gazol, A.
ISM: STRUCTURE
LOCAL INTERSTELLAR MATTER
MHD- ISM: MAGNETIC FIELDS
title_short The density-magnetic field relation in the atomic ISM
title_full The density-magnetic field relation in the atomic ISM
title_fullStr The density-magnetic field relation in the atomic ISM
title_full_unstemmed The density-magnetic field relation in the atomic ISM
title_sort The density-magnetic field relation in the atomic ISM
dc.creator.none.fl_str_mv Gazol, A.
Villagran Azuara, Marco Adrian
author Gazol, A.
author_facet Gazol, A.
Villagran Azuara, Marco Adrian
author_role author
author2 Villagran Azuara, Marco Adrian
author2_role author
dc.subject.none.fl_str_mv ISM: STRUCTURE
LOCAL INTERSTELLAR MATTER
MHD- ISM: MAGNETIC FIELDS
topic ISM: STRUCTURE
LOCAL INTERSTELLAR MATTER
MHD- ISM: MAGNETIC FIELDS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present numerical experiments aimed to study the correlation between the magnetic field strength, B, and the density, n, in the cold atomic interstellar medium (CNM). We analyse 24 magnetohydrodynamic models with different initial magnetic field intensities (B 0 = 0.4, 2.1, 4.2, and 8.3 μG) and/or mean densities (2, 3, and 4 cm -3 ), in the presence of driven and decaying turbulence, with and without self-gravity, in a cubic computational domain with 100 pc by side. Our main findings are as follows: (i) For forced simulations that reproduce the main observed physical conditions of the CNM in the solar neighbourhood, a positive correlation between B and n develops for all the B 0 values. (ii) The density at which this correlation becomes significant (≲30 cm -3 ) depends onB 0 but is not sensitive to the presence of self-gravity. (iii) The effect of self-gravity, when noticeable, consists of producing a shallower correlation at high densities, suggesting that, in the studied regime, self-gravity induces motions along the field lines. (iv) Self-gravitating decaying modelswhere theCNMis subsonic and sub- Alfvénic with β ≲ 1 develop a high-density positive correlation whose slopes are consistent with a constant β(n). (v) Decaying models where the low-density CNM is subsonic and sub- Alfvénic with β > 1 show a negative correlation at intermediate densities, followed by a high-density positive correlation.
Fil: Gazol, A.. Universidad Nacional Autónoma de México; México
Fil: Villagran Azuara, Marco Adrian. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
description We present numerical experiments aimed to study the correlation between the magnetic field strength, B, and the density, n, in the cold atomic interstellar medium (CNM). We analyse 24 magnetohydrodynamic models with different initial magnetic field intensities (B 0 = 0.4, 2.1, 4.2, and 8.3 μG) and/or mean densities (2, 3, and 4 cm -3 ), in the presence of driven and decaying turbulence, with and without self-gravity, in a cubic computational domain with 100 pc by side. Our main findings are as follows: (i) For forced simulations that reproduce the main observed physical conditions of the CNM in the solar neighbourhood, a positive correlation between B and n develops for all the B 0 values. (ii) The density at which this correlation becomes significant (≲30 cm -3 ) depends onB 0 but is not sensitive to the presence of self-gravity. (iii) The effect of self-gravity, when noticeable, consists of producing a shallower correlation at high densities, suggesting that, in the studied regime, self-gravity induces motions along the field lines. (iv) Self-gravitating decaying modelswhere theCNMis subsonic and sub- Alfvénic with β ≲ 1 develop a high-density positive correlation whose slopes are consistent with a constant β(n). (v) Decaying models where the low-density CNM is subsonic and sub- Alfvénic with β > 1 show a negative correlation at intermediate densities, followed by a high-density positive correlation.
publishDate 2018
dc.date.none.fl_str_mv 2018-07
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/11336/80566
Gazol, A.; Villagran Azuara, Marco Adrian; The density-magnetic field relation in the atomic ISM; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 478; 1; 7-2018; 146-154
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/80566
identifier_str_mv Gazol, A.; Villagran Azuara, Marco Adrian; The density-magnetic field relation in the atomic ISM; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 478; 1; 7-2018; 146-154
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1041
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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
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score 12.982451

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