Accretion shocks and winds in T Tauri stars

The dynamics of accretion and outflow in the T Tauri stars (TTSs) is expected to be associated with the production of shocks. Accretion shocks are expected to occur at the locations on the stellar surface where the kinetic energy of the infalling material is released into heating. Wind shocks are ex...

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Detalles Bibliográficos
Autor: Gómez De Castro, Ana Inés
Tipo de recurso: capítulo de libro
Fecha de publicación:2001
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/60573
Acceso en línea:https://hdl.handle.net/20.500.14352/60573
Access Level:acceso abierto
Palabra clave:52
Emission-line
Young stars
Ratios
Jets
Iue
Astronomía (Matemáticas)
21 Astronomía y Astrofísica
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oai_identifier_str oai:docta.ucm.es:20.500.14352/60573
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network_name_str España
repository_id_str
spelling Accretion shocks and winds in T Tauri starsGómez De Castro, Ana Inés52Emission-lineYoung starsRatiosJetsIueAstronomía (Matemáticas)21 Astronomía y AstrofísicaThe dynamics of accretion and outflow in the T Tauri stars (TTSs) is expected to be associated with the production of shocks. Accretion shocks are expected to occur at the locations on the stellar surface where the kinetic energy of the infalling material is released into heating. Wind shocks are expected to be generated in the wind, at the base of the high velocity jets. Both types of shocks are expected to occur at velocities of some few hundreths of km/s and high densities (> 10(6) cm(-3)) producing strong semiforbidden lines of O III], C III] and Si III] in the ultraviolet range. High resolution profiles of the Si III](1892) and C III](1908) lines are available for three pre-main sequence stars (AB Dor, RY Tau, RU Lup) in the IUE and BST Archives. In this contribution, evidence for shocks in the circumstellar environment of these sources is presented. In two out of the three cases studied, the shock is observed to occur in the wind, at the base of the optical jet. This is estimated to be at 0.2 AU from the base of the wind for RY Tau.Astronomical Soc PacificUniversidad Complutense de Madrid20012001-01-0120012001-01-01book parthttp://purl.org/coar/resource_type/c_3248info:eu-repo/semantics/bookPartapplication/pdfhttps://hdl.handle.net/20.500.14352/60573reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/605732026-06-02T12:44:21Z
dc.title.none.fl_str_mv Accretion shocks and winds in T Tauri stars
title Accretion shocks and winds in T Tauri stars
spellingShingle Accretion shocks and winds in T Tauri stars
Gómez De Castro, Ana Inés
52
Emission-line
Young stars
Ratios
Jets
Iue
Astronomía (Matemáticas)
21 Astronomía y Astrofísica
title_short Accretion shocks and winds in T Tauri stars
title_full Accretion shocks and winds in T Tauri stars
title_fullStr Accretion shocks and winds in T Tauri stars
title_full_unstemmed Accretion shocks and winds in T Tauri stars
title_sort Accretion shocks and winds in T Tauri stars
dc.creator.none.fl_str_mv Gómez De Castro, Ana Inés
author Gómez De Castro, Ana Inés
author_facet Gómez De Castro, Ana Inés
author_role author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 52
Emission-line
Young stars
Ratios
Jets
Iue
Astronomía (Matemáticas)
21 Astronomía y Astrofísica
topic 52
Emission-line
Young stars
Ratios
Jets
Iue
Astronomía (Matemáticas)
21 Astronomía y Astrofísica
description The dynamics of accretion and outflow in the T Tauri stars (TTSs) is expected to be associated with the production of shocks. Accretion shocks are expected to occur at the locations on the stellar surface where the kinetic energy of the infalling material is released into heating. Wind shocks are expected to be generated in the wind, at the base of the high velocity jets. Both types of shocks are expected to occur at velocities of some few hundreths of km/s and high densities (> 10(6) cm(-3)) producing strong semiforbidden lines of O III], C III] and Si III] in the ultraviolet range. High resolution profiles of the Si III](1892) and C III](1908) lines are available for three pre-main sequence stars (AB Dor, RY Tau, RU Lup) in the IUE and BST Archives. In this contribution, evidence for shocks in the circumstellar environment of these sources is presented. In two out of the three cases studied, the shock is observed to occur in the wind, at the base of the optical jet. This is estimated to be at 0.2 AU from the base of the wind for RY Tau.
publishDate 2001
dc.date.none.fl_str_mv 2001
2001-01-01
2001
2001-01-01
dc.type.none.fl_str_mv book part
http://purl.org/coar/resource_type/c_3248
dc.type.openaire.fl_str_mv info:eu-repo/semantics/bookPart
format bookPart
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/60573
url https://hdl.handle.net/20.500.14352/60573
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Astronomical Soc Pacific
publisher.none.fl_str_mv Astronomical Soc Pacific
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869412844947111936
score 15,223283

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