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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/80566
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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 Técnicas2025-09-29T09:39:07Zoai: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:34982025-09-29 09:39:08.017CONICET 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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1844613237358723072 |
score |
13.070432 |