The structure and kinematics of the ISM around HD 192281
- Autores
- Arnal, Edmundo Marcelo; Cichowolski, Silvina; Pineault, Serge; Testori, Juan Carlos; Cappa, Cristina Elisabet
- Año de publicación
- 2011
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. This work aims at investigating the interaction of HD 192281 (O5 Vn((f))p) with its local ISM. The purpose is to analyse the effects that a massive star has on the structure and kinematics of its surrounding gas. Methods. To carry out this study, we used high-resolution radio continuum and 21-cm H i line data from the Canadian Galactic Plane Survey (CGPS). This data base was complemented with radio continuum, infrared, and molecular data retrieved from available surveys. Given that HD 192281 is very likely a runaway star, we attempt to establish whether the observed H i distribution can be interpreted in terms of a simple bow shock model. Results. Analysis of the H i data shows the presence of an H i feature likely to be associated with HD 192281. This feature remains detectable from ~5 to-10 km s-1. At the most negative radial velocities, the shape of the H i feature is highly reminiscent of a bow shock structure seen projected onto the plane of the sky. This feature has counterparts at radio-continuum, infrared, and CO emissions. The analysis of the radio continuum data suggests a thermal spectrum for the gas related to this structure.
Instituto Argentino de Radioastronomía
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
ISM: bubbles
ISM: structure
outflows
Stars: individual: HD 192281
Stars: mass-loss
Stars: winds - 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:10915/84044
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The structure and kinematics of the ISM around HD 192281Arnal, Edmundo MarceloCichowolski, SilvinaPineault, SergeTestori, Juan CarlosCappa, Cristina ElisabetCiencias AstronómicasISM: bubblesISM: structureoutflowsStars: individual: HD 192281Stars: mass-lossStars: winds<b>Aims.</b> This work aims at investigating the interaction of HD 192281 (O5 Vn((f))p) with its local ISM. The purpose is to analyse the effects that a massive star has on the structure and kinematics of its surrounding gas. <b>Methods.</b> To carry out this study, we used high-resolution radio continuum and 21-cm H i line data from the Canadian Galactic Plane Survey (CGPS). This data base was complemented with radio continuum, infrared, and molecular data retrieved from available surveys. Given that HD 192281 is very likely a runaway star, we attempt to establish whether the observed H i distribution can be interpreted in terms of a simple bow shock model. <b>Results.</b> Analysis of the H i data shows the presence of an H i feature likely to be associated with HD 192281. This feature remains detectable from ~5 to-10 km s-1. At the most negative radial velocities, the shape of the H i feature is highly reminiscent of a bow shock structure seen projected onto the plane of the sky. This feature has counterparts at radio-continuum, infrared, and CO emissions. The analysis of the radio continuum data suggests a thermal spectrum for the gas related to this structure.Instituto Argentino de RadioastronomíaFacultad de Ciencias Astronómicas y Geofísicas2011-04-08info: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/10915/84044enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201015924info: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:UNLP2025-09-29T11:16:06Zoai:sedici.unlp.edu.ar:10915/84044Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:06.524SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
The structure and kinematics of the ISM around HD 192281 |
title |
The structure and kinematics of the ISM around HD 192281 |
spellingShingle |
The structure and kinematics of the ISM around HD 192281 Arnal, Edmundo Marcelo Ciencias Astronómicas ISM: bubbles ISM: structure outflows Stars: individual: HD 192281 Stars: mass-loss Stars: winds |
title_short |
The structure and kinematics of the ISM around HD 192281 |
title_full |
The structure and kinematics of the ISM around HD 192281 |
title_fullStr |
The structure and kinematics of the ISM around HD 192281 |
title_full_unstemmed |
The structure and kinematics of the ISM around HD 192281 |
title_sort |
The structure and kinematics of the ISM around HD 192281 |
dc.creator.none.fl_str_mv |
Arnal, Edmundo Marcelo Cichowolski, Silvina Pineault, Serge Testori, Juan Carlos Cappa, Cristina Elisabet |
author |
Arnal, Edmundo Marcelo |
author_facet |
Arnal, Edmundo Marcelo Cichowolski, Silvina Pineault, Serge Testori, Juan Carlos Cappa, Cristina Elisabet |
author_role |
author |
author2 |
Cichowolski, Silvina Pineault, Serge Testori, Juan Carlos Cappa, Cristina Elisabet |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas ISM: bubbles ISM: structure outflows Stars: individual: HD 192281 Stars: mass-loss Stars: winds |
topic |
Ciencias Astronómicas ISM: bubbles ISM: structure outflows Stars: individual: HD 192281 Stars: mass-loss Stars: winds |
dc.description.none.fl_txt_mv |
<b>Aims.</b> This work aims at investigating the interaction of HD 192281 (O5 Vn((f))p) with its local ISM. The purpose is to analyse the effects that a massive star has on the structure and kinematics of its surrounding gas. <b>Methods.</b> To carry out this study, we used high-resolution radio continuum and 21-cm H i line data from the Canadian Galactic Plane Survey (CGPS). This data base was complemented with radio continuum, infrared, and molecular data retrieved from available surveys. Given that HD 192281 is very likely a runaway star, we attempt to establish whether the observed H i distribution can be interpreted in terms of a simple bow shock model. <b>Results.</b> Analysis of the H i data shows the presence of an H i feature likely to be associated with HD 192281. This feature remains detectable from ~5 to-10 km s-1. At the most negative radial velocities, the shape of the H i feature is highly reminiscent of a bow shock structure seen projected onto the plane of the sky. This feature has counterparts at radio-continuum, infrared, and CO emissions. The analysis of the radio continuum data suggests a thermal spectrum for the gas related to this structure. Instituto Argentino de Radioastronomía Facultad de Ciencias Astronómicas y Geofísicas |
description |
<b>Aims.</b> This work aims at investigating the interaction of HD 192281 (O5 Vn((f))p) with its local ISM. The purpose is to analyse the effects that a massive star has on the structure and kinematics of its surrounding gas. <b>Methods.</b> To carry out this study, we used high-resolution radio continuum and 21-cm H i line data from the Canadian Galactic Plane Survey (CGPS). This data base was complemented with radio continuum, infrared, and molecular data retrieved from available surveys. Given that HD 192281 is very likely a runaway star, we attempt to establish whether the observed H i distribution can be interpreted in terms of a simple bow shock model. <b>Results.</b> Analysis of the H i data shows the presence of an H i feature likely to be associated with HD 192281. This feature remains detectable from ~5 to-10 km s-1. At the most negative radial velocities, the shape of the H i feature is highly reminiscent of a bow shock structure seen projected onto the plane of the sky. This feature has counterparts at radio-continuum, infrared, and CO emissions. The analysis of the radio continuum data suggests a thermal spectrum for the gas related to this structure. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-04-08 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo 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://sedici.unlp.edu.ar/handle/10915/84044 |
url |
http://sedici.unlp.edu.ar/handle/10915/84044 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201015924 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
dc.format.none.fl_str_mv |
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