Distinguishing circumstellar from stellar photometric variability in Eta Carinae
- Autores
- Damineli, A.; Fernandez Lajus, Eduardo Eusebio; Almeida, L.A.; Corcoran, M.F.; Damineli, D.S.C.; Gull, T.R.; Hamaguchi, K; Hillier, D.J.; Jablonski, F.J.; Madura, T.I.; Moffat, A.F.J.; Navarete, F.; Richardson, N.D.; Ruiz, G.F.; Salerno, N.E.; Scalia, María Cecilia; Weigelt, G.
- Año de publicación
- 2019
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The interacting binary Eta Carinae remains one of the most enigmatic massive stars in our Galaxy despite over four centuries of observations. In this work, its light curve from the ultraviolet to the near-infrared is analysed using spatially resolved HST observations and intense monitoring at the La Plata Observatory, combined with previously published photometry. We have developed a method to separate the central stellar object in the ground-based images using HST photometry and applying it to the more numerous ground-based data, which supports the hypothesis that the central source is brightening faster than the almost-constant Homunculus. After detrending from long-term brightening, the light curve shows periodic orbital modulation (V ∼ 0.6 mag) attributed to the wind–wind collision cavity as it sweeps around the primary star and it shows variable projected area to our line-of-sight. Two quasi-periodic components with time-scales of 2–3 and 8–10 yr and low amplitude, V < 0.2 mag, are superimposed on the brightening light curve, being the only stellar component of variability found, which indicates minimal stellar instability. Moreover, the light-curve analysis shows no evidence of ‘shell ejections’ at periastron. We propose that the long-term brightening of the stellar core is due to the dissipation of a dusty clump in front of the central star, which works like a natural coronagraph. Thus, the central stars appear to be more stable than previously thought since the dominant variability originates from a changing circumstellar medium. We predict that the brightening phase, due mainly to dust dissipation, will be completed around 2032 ± 4 yr, when the star will be brighter than in the 1600s by up to V ∼ 1 mag.
Fil: Damineli, A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Almeida, L.A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil. Universidade Federal do Rio Grande do Norte; Brasil
Fil: Corcoran, M.F.. National Aeronautics and Space Administration; Estados Unidos. The Catholic University of America; Estados Unidos
Fil: Damineli, D.S.C.. University of Maryland; Estados Unidos
Fil: Gull, T.R.. National Aeronautics and Space Administration; Estados Unidos
Fil: Hamaguchi, K. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados Unidos
Fil: Hillier, D.J.. University of Pittsburgh; Estados Unidos
Fil: Jablonski, F.J.. Centro de Previsao de Tempo e Estudos Climáticos. Instituto Nacional de Pesquisas Espaciais; Brasil
Fil: Madura, T.I.. San Jose State University; Estados Unidos
Fil: Moffat, A.F.J.. Université du Québec a Montreal; Canadá
Fil: Navarete, F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil
Fil: Richardson, N.D.. University Of Toledo (utoledo); Estados Unidos
Fil: Ruiz, G.F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil
Fil: Salerno, N.E.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Scalia, María Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Weigelt, G.. Max Planck Institute For Radio Astronomy; Alemania - Materia
-
BINARIES: GENERAL
DUST
EXTINCTION
OUTFLOWS
STARS: EVOLUTION
STARS: INDIVIDUAL (Η CARINAE)
STARS: WINDS - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/145392
Ver los metadatos del registro completo
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Distinguishing circumstellar from stellar photometric variability in Eta CarinaeDamineli, A.Fernandez Lajus, Eduardo EusebioAlmeida, L.A.Corcoran, M.F.Damineli, D.S.C.Gull, T.R.Hamaguchi, KHillier, D.J.Jablonski, F.J.Madura, T.I.Moffat, A.F.J.Navarete, F.Richardson, N.D.Ruiz, G.F.Salerno, N.E.Scalia, María CeciliaWeigelt, G.BINARIES: GENERALDUSTEXTINCTIONOUTFLOWSSTARS: EVOLUTIONSTARS: INDIVIDUAL (Η CARINAE)STARS: WINDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The interacting binary Eta Carinae remains one of the most enigmatic massive stars in our Galaxy despite over four centuries of observations. In this work, its light curve from the ultraviolet to the near-infrared is analysed using spatially resolved HST observations and intense monitoring at the La Plata Observatory, combined with previously published photometry. We have developed a method to separate the central stellar object in the ground-based images using HST photometry and applying it to the more numerous ground-based data, which supports the hypothesis that the central source is brightening faster than the almost-constant Homunculus. After detrending from long-term brightening, the light curve shows periodic orbital modulation (V ∼ 0.6 mag) attributed to the wind–wind collision cavity as it sweeps around the primary star and it shows variable projected area to our line-of-sight. Two quasi-periodic components with time-scales of 2–3 and 8–10 yr and low amplitude, V < 0.2 mag, are superimposed on the brightening light curve, being the only stellar component of variability found, which indicates minimal stellar instability. Moreover, the light-curve analysis shows no evidence of ‘shell ejections’ at periastron. We propose that the long-term brightening of the stellar core is due to the dissipation of a dusty clump in front of the central star, which works like a natural coronagraph. Thus, the central stars appear to be more stable than previously thought since the dominant variability originates from a changing circumstellar medium. We predict that the brightening phase, due mainly to dust dissipation, will be completed around 2032 ± 4 yr, when the star will be brighter than in the 1600s by up to V ∼ 1 mag.Fil: Damineli, A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; BrasilFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Almeida, L.A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil. Universidade Federal do Rio Grande do Norte; BrasilFil: Corcoran, M.F.. National Aeronautics and Space Administration; Estados Unidos. The Catholic University of America; Estados UnidosFil: Damineli, D.S.C.. University of Maryland; Estados UnidosFil: Gull, T.R.. National Aeronautics and Space Administration; Estados UnidosFil: Hamaguchi, K. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados UnidosFil: Hillier, D.J.. University of Pittsburgh; Estados UnidosFil: Jablonski, F.J.. Centro de Previsao de Tempo e Estudos Climáticos. Instituto Nacional de Pesquisas Espaciais; BrasilFil: Madura, T.I.. San Jose State University; Estados UnidosFil: Moffat, A.F.J.. Université du Québec a Montreal; CanadáFil: Navarete, F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; BrasilFil: Richardson, N.D.. University Of Toledo (utoledo); Estados UnidosFil: Ruiz, G.F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; BrasilFil: Salerno, N.E.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Scalia, María Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Weigelt, G.. Max Planck Institute For Radio Astronomy; AlemaniaOxford University Press2019-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/145392Damineli, A.; Fernandez Lajus, Eduardo Eusebio; Almeida, L.A.; Corcoran, M.F.; Damineli, D.S.C.; et al.; Distinguishing circumstellar from stellar photometric variability in Eta Carinae; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 484; 1; 3-2019; 1325-13460035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz067info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/484/1/1325/5289420info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:07:58Zoai:ri.conicet.gov.ar:11336/145392instacron: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 10:07:59.238CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| title |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| spellingShingle |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae Damineli, A. BINARIES: GENERAL DUST EXTINCTION OUTFLOWS STARS: EVOLUTION STARS: INDIVIDUAL (Η CARINAE) STARS: WINDS |
| title_short |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| title_full |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| title_fullStr |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| title_full_unstemmed |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| title_sort |
Distinguishing circumstellar from stellar photometric variability in Eta Carinae |
| dc.creator.none.fl_str_mv |
Damineli, A. Fernandez Lajus, Eduardo Eusebio Almeida, L.A. Corcoran, M.F. Damineli, D.S.C. Gull, T.R. Hamaguchi, K Hillier, D.J. Jablonski, F.J. Madura, T.I. Moffat, A.F.J. Navarete, F. Richardson, N.D. Ruiz, G.F. Salerno, N.E. Scalia, María Cecilia Weigelt, G. |
| author |
Damineli, A. |
| author_facet |
Damineli, A. Fernandez Lajus, Eduardo Eusebio Almeida, L.A. Corcoran, M.F. Damineli, D.S.C. Gull, T.R. Hamaguchi, K Hillier, D.J. Jablonski, F.J. Madura, T.I. Moffat, A.F.J. Navarete, F. Richardson, N.D. Ruiz, G.F. Salerno, N.E. Scalia, María Cecilia Weigelt, G. |
| author_role |
author |
| author2 |
Fernandez Lajus, Eduardo Eusebio Almeida, L.A. Corcoran, M.F. Damineli, D.S.C. Gull, T.R. Hamaguchi, K Hillier, D.J. Jablonski, F.J. Madura, T.I. Moffat, A.F.J. Navarete, F. Richardson, N.D. Ruiz, G.F. Salerno, N.E. Scalia, María Cecilia Weigelt, G. |
| author2_role |
author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
BINARIES: GENERAL DUST EXTINCTION OUTFLOWS STARS: EVOLUTION STARS: INDIVIDUAL (Η CARINAE) STARS: WINDS |
| topic |
BINARIES: GENERAL DUST EXTINCTION OUTFLOWS STARS: EVOLUTION STARS: INDIVIDUAL (Η CARINAE) STARS: WINDS |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The interacting binary Eta Carinae remains one of the most enigmatic massive stars in our Galaxy despite over four centuries of observations. In this work, its light curve from the ultraviolet to the near-infrared is analysed using spatially resolved HST observations and intense monitoring at the La Plata Observatory, combined with previously published photometry. We have developed a method to separate the central stellar object in the ground-based images using HST photometry and applying it to the more numerous ground-based data, which supports the hypothesis that the central source is brightening faster than the almost-constant Homunculus. After detrending from long-term brightening, the light curve shows periodic orbital modulation (V ∼ 0.6 mag) attributed to the wind–wind collision cavity as it sweeps around the primary star and it shows variable projected area to our line-of-sight. Two quasi-periodic components with time-scales of 2–3 and 8–10 yr and low amplitude, V < 0.2 mag, are superimposed on the brightening light curve, being the only stellar component of variability found, which indicates minimal stellar instability. Moreover, the light-curve analysis shows no evidence of ‘shell ejections’ at periastron. We propose that the long-term brightening of the stellar core is due to the dissipation of a dusty clump in front of the central star, which works like a natural coronagraph. Thus, the central stars appear to be more stable than previously thought since the dominant variability originates from a changing circumstellar medium. We predict that the brightening phase, due mainly to dust dissipation, will be completed around 2032 ± 4 yr, when the star will be brighter than in the 1600s by up to V ∼ 1 mag. Fil: Damineli, A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Almeida, L.A.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil. Universidade Federal do Rio Grande do Norte; Brasil Fil: Corcoran, M.F.. National Aeronautics and Space Administration; Estados Unidos. The Catholic University of America; Estados Unidos Fil: Damineli, D.S.C.. University of Maryland; Estados Unidos Fil: Gull, T.R.. National Aeronautics and Space Administration; Estados Unidos Fil: Hamaguchi, K. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados Unidos Fil: Hillier, D.J.. University of Pittsburgh; Estados Unidos Fil: Jablonski, F.J.. Centro de Previsao de Tempo e Estudos Climáticos. Instituto Nacional de Pesquisas Espaciais; Brasil Fil: Madura, T.I.. San Jose State University; Estados Unidos Fil: Moffat, A.F.J.. Université du Québec a Montreal; Canadá Fil: Navarete, F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil Fil: Richardson, N.D.. University Of Toledo (utoledo); Estados Unidos Fil: Ruiz, G.F.. Universidade do Sao Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brasil Fil: Salerno, N.E.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Scalia, María Cecilia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Weigelt, G.. Max Planck Institute For Radio Astronomy; Alemania |
| description |
The interacting binary Eta Carinae remains one of the most enigmatic massive stars in our Galaxy despite over four centuries of observations. In this work, its light curve from the ultraviolet to the near-infrared is analysed using spatially resolved HST observations and intense monitoring at the La Plata Observatory, combined with previously published photometry. We have developed a method to separate the central stellar object in the ground-based images using HST photometry and applying it to the more numerous ground-based data, which supports the hypothesis that the central source is brightening faster than the almost-constant Homunculus. After detrending from long-term brightening, the light curve shows periodic orbital modulation (V ∼ 0.6 mag) attributed to the wind–wind collision cavity as it sweeps around the primary star and it shows variable projected area to our line-of-sight. Two quasi-periodic components with time-scales of 2–3 and 8–10 yr and low amplitude, V < 0.2 mag, are superimposed on the brightening light curve, being the only stellar component of variability found, which indicates minimal stellar instability. Moreover, the light-curve analysis shows no evidence of ‘shell ejections’ at periastron. We propose that the long-term brightening of the stellar core is due to the dissipation of a dusty clump in front of the central star, which works like a natural coronagraph. Thus, the central stars appear to be more stable than previously thought since the dominant variability originates from a changing circumstellar medium. We predict that the brightening phase, due mainly to dust dissipation, will be completed around 2032 ± 4 yr, when the star will be brighter than in the 1600s by up to V ∼ 1 mag. |
| publishDate |
2019 |
| dc.date.none.fl_str_mv |
2019-03 |
| 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/11336/145392 Damineli, A.; Fernandez Lajus, Eduardo Eusebio; Almeida, L.A.; Corcoran, M.F.; Damineli, D.S.C.; et al.; Distinguishing circumstellar from stellar photometric variability in Eta Carinae; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 484; 1; 3-2019; 1325-1346 0035-8711 1365-2966 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/145392 |
| identifier_str_mv |
Damineli, A.; Fernandez Lajus, Eduardo Eusebio; Almeida, L.A.; Corcoran, M.F.; Damineli, D.S.C.; et al.; Distinguishing circumstellar from stellar photometric variability in Eta Carinae; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 484; 1; 3-2019; 1325-1346 0035-8711 1365-2966 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz067 info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/484/1/1325/5289420 |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf application/pdf |
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Oxford University Press |
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Oxford University Press |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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