The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity
- Autores
- Méndez, Mariano R.; Klis, Michiel van der; Ford, Eric C.
- Año de publicación
- 2001
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We study the kilohertz quasi-periodic oscillations (kHz QPOs) in the low-mass X-ray binaries 4U 1728-34, 4U 1608-52, and Aq1 X-1. Each source traces out a set of nearly parallel tracks in a frequency versus X-ray count rate diagram. We find that between two of these tracks, for similar QPO frequency, the 2-60 keV source count rate can differ by up to a factor of ∼4, whereas at the same time the rms amplitude of the kHz QPOs is only a factor of ∼1.1 different. We also find that, for 4U 1608-52 and Aq1 X-1, the rms spectrum of the kHz QPOs does not depend upon which track the source occupies in the frequency versus X-ray count rate diagram. Our results for 4U 1728-34, 4U 1608-52, and Aq1 X-1 are inconsistent with simple "extra source of X-rays" scenarios for the parallel tracks, such as those in which the properties of the kHz QPOs are determined only by the mass accretion rate through the disk, whereas X-ray count rate also depends upon other sources of energy that do not affect the QPOs.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Accretion, accretion disks
Stars: individual (4U 1608-52, 4U 1728-34, Aquila X-1)
Stars: neutron
X-rays: stars - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84694
Ver los metadatos del registro completo
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The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensityMéndez, Mariano R.Klis, Michiel van derFord, Eric C.Ciencias AstronómicasAccretion, accretion disksStars: individual (4U 1608-52, 4U 1728-34, Aquila X-1)Stars: neutronX-rays: starsWe study the kilohertz quasi-periodic oscillations (kHz QPOs) in the low-mass X-ray binaries 4U 1728-34, 4U 1608-52, and Aq1 X-1. Each source traces out a set of nearly parallel tracks in a frequency versus X-ray count rate diagram. We find that between two of these tracks, for similar QPO frequency, the 2-60 keV source count rate can differ by up to a factor of ∼4, whereas at the same time the rms amplitude of the kHz QPOs is only a factor of ∼1.1 different. We also find that, for 4U 1608-52 and Aq1 X-1, the rms spectrum of the kHz QPOs does not depend upon which track the source occupies in the frequency versus X-ray count rate diagram. Our results for 4U 1728-34, 4U 1608-52, and Aq1 X-1 are inconsistent with simple "extra source of X-rays" scenarios for the parallel tracks, such as those in which the properties of the kHz QPOs are determined only by the mass accretion rate through the disk, whereas X-ray count rate also depends upon other sources of energy that do not affect the QPOs.Facultad de Ciencias Astronómicas y Geofísicas2001info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1016-1026http://sedici.unlp.edu.ar/handle/10915/84694enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1086/323486info: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:UNLP2025-10-22T16:57:07Zoai:sedici.unlp.edu.ar:10915/84694Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:57:07.917SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| title |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| spellingShingle |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity Méndez, Mariano R. Ciencias Astronómicas Accretion, accretion disks Stars: individual (4U 1608-52, 4U 1728-34, Aquila X-1) Stars: neutron X-rays: stars |
| title_short |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| title_full |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| title_fullStr |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| title_full_unstemmed |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| title_sort |
The amplitude of the kilohertz quasi-periodic oscillations in 4U 1728-34, 4U 1608-52, and aquila X-1, as a function of X-ray intensity |
| dc.creator.none.fl_str_mv |
Méndez, Mariano R. Klis, Michiel van der Ford, Eric C. |
| author |
Méndez, Mariano R. |
| author_facet |
Méndez, Mariano R. Klis, Michiel van der Ford, Eric C. |
| author_role |
author |
| author2 |
Klis, Michiel van der Ford, Eric C. |
| author2_role |
author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Accretion, accretion disks Stars: individual (4U 1608-52, 4U 1728-34, Aquila X-1) Stars: neutron X-rays: stars |
| topic |
Ciencias Astronómicas Accretion, accretion disks Stars: individual (4U 1608-52, 4U 1728-34, Aquila X-1) Stars: neutron X-rays: stars |
| dc.description.none.fl_txt_mv |
We study the kilohertz quasi-periodic oscillations (kHz QPOs) in the low-mass X-ray binaries 4U 1728-34, 4U 1608-52, and Aq1 X-1. Each source traces out a set of nearly parallel tracks in a frequency versus X-ray count rate diagram. We find that between two of these tracks, for similar QPO frequency, the 2-60 keV source count rate can differ by up to a factor of ∼4, whereas at the same time the rms amplitude of the kHz QPOs is only a factor of ∼1.1 different. We also find that, for 4U 1608-52 and Aq1 X-1, the rms spectrum of the kHz QPOs does not depend upon which track the source occupies in the frequency versus X-ray count rate diagram. Our results for 4U 1728-34, 4U 1608-52, and Aq1 X-1 are inconsistent with simple "extra source of X-rays" scenarios for the parallel tracks, such as those in which the properties of the kHz QPOs are determined only by the mass accretion rate through the disk, whereas X-ray count rate also depends upon other sources of energy that do not affect the QPOs. Facultad de Ciencias Astronómicas y Geofísicas |
| description |
We study the kilohertz quasi-periodic oscillations (kHz QPOs) in the low-mass X-ray binaries 4U 1728-34, 4U 1608-52, and Aq1 X-1. Each source traces out a set of nearly parallel tracks in a frequency versus X-ray count rate diagram. We find that between two of these tracks, for similar QPO frequency, the 2-60 keV source count rate can differ by up to a factor of ∼4, whereas at the same time the rms amplitude of the kHz QPOs is only a factor of ∼1.1 different. We also find that, for 4U 1608-52 and Aq1 X-1, the rms spectrum of the kHz QPOs does not depend upon which track the source occupies in the frequency versus X-ray count rate diagram. Our results for 4U 1728-34, 4U 1608-52, and Aq1 X-1 are inconsistent with simple "extra source of X-rays" scenarios for the parallel tracks, such as those in which the properties of the kHz QPOs are determined only by the mass accretion rate through the disk, whereas X-ray count rate also depends upon other sources of energy that do not affect the QPOs. |
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2001 |
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2001 |
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http://sedici.unlp.edu.ar/handle/10915/84694 |
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eng |
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