Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2
- Autores
- Wijnands, Rudy; Homan, Jeroen; Klis, Michiel van der; Méndez, Mariano R.; Kuulkers, Erik; Paradijs, Jan van; Lewin, Walter H. G.; Lamb, Frederick K.; Psaltis, Dimitrios; Vaughan, Brian A.
- Año de publicación
- 1997
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We observed the low-mass X-ray binary and Z source GX 17+2 with the Rossi X-Ray Timing Explorer during 1997 February 6-8, April 1-4, and July 26-27. The X-ray color-color diagram shows a clear Z track. Two simultaneous kHz quasi-periodic oscillations (QPOs) are present in each observation, whose frequencies are well correlated with the position of the source on the Z track. At the left end of the horizontal branch (HB), only the higher frequency peak is observed, at 645 ± 9 Hz, with an rms amplitude of 5.7% ± 0.5% and an FWHM of 183 ± 35 Hz. When the source moves down the Z track to the upper normal branch, the frequency of the kHz QPO increases to 1087 ± 12 Hz, and the rms amplitude and FWHM decrease by a factor of 2. Farther down the Z track, the QPO becomes undetectable, with rms upper limits typically of 2.0%. Halfway down the HB, a second QPO appears in the power spectra with a frequency of 480 ± 23 Hz. The frequency of this QPO also increases when the source moves along the Z track, up to 781 ± 11 Hz halfway down the normal branch, while the rms amplitude and FWHM stay approximately constant at 2.5% and 70 Hz. The QPO frequency difference is constant at 293.5 ± 7.5 Hz. Simultaneously with the kHz QPOs, we detect HB QPOs (HBOs). The simultaneous presence of HBOs and kHz QPOs excludes the magnetospheric beat-frequency model as the explanation for at least one of these two phenomena.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Astronomía
accretion, accretion disks
stars: individual (GX 1712)
stars: neutron
X-rays: stars - 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:10915/123155
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Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2Wijnands, RudyHoman, JeroenKlis, Michiel van derMéndez, Mariano R.Kuulkers, ErikParadijs, Jan vanLewin, Walter H. G.Lamb, Frederick K.Psaltis, DimitriosVaughan, Brian A.Astronomíaaccretion, accretion disksstars: individual (GX 1712)stars: neutronX-rays: starsWe observed the low-mass X-ray binary and Z source GX 17+2 with the <i>Rossi X-Ray Timing Explorer</i> during 1997 February 6-8, April 1-4, and July 26-27. The X-ray color-color diagram shows a clear Z track. Two simultaneous kHz quasi-periodic oscillations (QPOs) are present in each observation, whose frequencies are well correlated with the position of the source on the Z track. At the left end of the horizontal branch (HB), only the higher frequency peak is observed, at 645 ± 9 Hz, with an rms amplitude of 5.7% ± 0.5% and an FWHM of 183 ± 35 Hz. When the source moves down the Z track to the upper normal branch, the frequency of the kHz QPO increases to 1087 ± 12 Hz, and the rms amplitude and FWHM decrease by a factor of 2. Farther down the Z track, the QPO becomes undetectable, with rms upper limits typically of 2.0%. Halfway down the HB, a second QPO appears in the power spectra with a frequency of 480 ± 23 Hz. The frequency of this QPO also increases when the source moves along the Z track, up to 781 ± 11 Hz halfway down the normal branch, while the rms amplitude and FWHM stay approximately constant at 2.5% and 70 Hz. The QPO frequency difference is constant at 293.5 ± 7.5 Hz. Simultaneously with the kHz QPOs, we detect HB QPOs (HBOs). The simultaneous presence of HBOs and kHz QPOs excludes the magnetospheric beat-frequency model as the explanation for at least one of these two phenomena.Facultad de Ciencias Astronómicas y Geofísicas1997-12-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf157-160http://sedici.unlp.edu.ar/handle/10915/123155enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1086/311039info: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:UNLP2025-09-29T11:29:18Zoai:sedici.unlp.edu.ar:10915/123155Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:29:19.029SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
title |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
spellingShingle |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 Wijnands, Rudy Astronomía accretion, accretion disks stars: individual (GX 1712) stars: neutron X-rays: stars |
title_short |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
title_full |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
title_fullStr |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
title_full_unstemmed |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
title_sort |
Discovery of Kilohertz Quasi-periodic Oscillations in GX 17+2 |
dc.creator.none.fl_str_mv |
Wijnands, Rudy Homan, Jeroen Klis, Michiel van der Méndez, Mariano R. Kuulkers, Erik Paradijs, Jan van Lewin, Walter H. G. Lamb, Frederick K. Psaltis, Dimitrios Vaughan, Brian A. |
author |
Wijnands, Rudy |
author_facet |
Wijnands, Rudy Homan, Jeroen Klis, Michiel van der Méndez, Mariano R. Kuulkers, Erik Paradijs, Jan van Lewin, Walter H. G. Lamb, Frederick K. Psaltis, Dimitrios Vaughan, Brian A. |
author_role |
author |
author2 |
Homan, Jeroen Klis, Michiel van der Méndez, Mariano R. Kuulkers, Erik Paradijs, Jan van Lewin, Walter H. G. Lamb, Frederick K. Psaltis, Dimitrios Vaughan, Brian A. |
author2_role |
author author author author author author author author author |
dc.subject.none.fl_str_mv |
Astronomía accretion, accretion disks stars: individual (GX 1712) stars: neutron X-rays: stars |
topic |
Astronomía accretion, accretion disks stars: individual (GX 1712) stars: neutron X-rays: stars |
dc.description.none.fl_txt_mv |
We observed the low-mass X-ray binary and Z source GX 17+2 with the <i>Rossi X-Ray Timing Explorer</i> during 1997 February 6-8, April 1-4, and July 26-27. The X-ray color-color diagram shows a clear Z track. Two simultaneous kHz quasi-periodic oscillations (QPOs) are present in each observation, whose frequencies are well correlated with the position of the source on the Z track. At the left end of the horizontal branch (HB), only the higher frequency peak is observed, at 645 ± 9 Hz, with an rms amplitude of 5.7% ± 0.5% and an FWHM of 183 ± 35 Hz. When the source moves down the Z track to the upper normal branch, the frequency of the kHz QPO increases to 1087 ± 12 Hz, and the rms amplitude and FWHM decrease by a factor of 2. Farther down the Z track, the QPO becomes undetectable, with rms upper limits typically of 2.0%. Halfway down the HB, a second QPO appears in the power spectra with a frequency of 480 ± 23 Hz. The frequency of this QPO also increases when the source moves along the Z track, up to 781 ± 11 Hz halfway down the normal branch, while the rms amplitude and FWHM stay approximately constant at 2.5% and 70 Hz. The QPO frequency difference is constant at 293.5 ± 7.5 Hz. Simultaneously with the kHz QPOs, we detect HB QPOs (HBOs). The simultaneous presence of HBOs and kHz QPOs excludes the magnetospheric beat-frequency model as the explanation for at least one of these two phenomena. Facultad de Ciencias Astronómicas y Geofísicas |
description |
We observed the low-mass X-ray binary and Z source GX 17+2 with the <i>Rossi X-Ray Timing Explorer</i> during 1997 February 6-8, April 1-4, and July 26-27. The X-ray color-color diagram shows a clear Z track. Two simultaneous kHz quasi-periodic oscillations (QPOs) are present in each observation, whose frequencies are well correlated with the position of the source on the Z track. At the left end of the horizontal branch (HB), only the higher frequency peak is observed, at 645 ± 9 Hz, with an rms amplitude of 5.7% ± 0.5% and an FWHM of 183 ± 35 Hz. When the source moves down the Z track to the upper normal branch, the frequency of the kHz QPO increases to 1087 ± 12 Hz, and the rms amplitude and FWHM decrease by a factor of 2. Farther down the Z track, the QPO becomes undetectable, with rms upper limits typically of 2.0%. Halfway down the HB, a second QPO appears in the power spectra with a frequency of 480 ± 23 Hz. The frequency of this QPO also increases when the source moves along the Z track, up to 781 ± 11 Hz halfway down the normal branch, while the rms amplitude and FWHM stay approximately constant at 2.5% and 70 Hz. The QPO frequency difference is constant at 293.5 ± 7.5 Hz. Simultaneously with the kHz QPOs, we detect HB QPOs (HBOs). The simultaneous presence of HBOs and kHz QPOs excludes the magnetospheric beat-frequency model as the explanation for at least one of these two phenomena. |
publishDate |
1997 |
dc.date.none.fl_str_mv |
1997-12-01 |
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 |
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article |
status_str |
publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/123155 |
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http://sedici.unlp.edu.ar/handle/10915/123155 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-637X info:eu-repo/semantics/altIdentifier/doi/10.1086/311039 |
dc.rights.none.fl_str_mv |
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openAccess |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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