Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09

We report three <i>RXTE</i>/PCA observations of the low-mass X-ray binary 4U 0614+09. They show strong (~30% rms) band-limited noise with a cutoff frequency varying between 0.7 and 15 Hz in correlation with the X-ray flux, fₓ. We observe two nonsimultaneous 11%-15% (rms) kHz peaks near 7...

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Detalles Bibliográficos
Autores: Méndez, Mariano R., Klis, M. van der, Paradijs, J. van, Lewin, Walter H. G., Lamb, Frederick K., Vaughan, Brian A., Kuulkers, Erik, Psaltis, Dimitrios
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:1997
País:Argentina
Institución:Universidad Nacional de La Plata
Repositorio:SEDICI (UNLP)
Idioma:inglés
OAI Identifier:oai:sedici.unlp.edu.ar:10915/123162
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/123162
Access Level:acceso abierto
Palabra clave:Astronomía
accretion, accretion disks
stars: individual (4U 06141091)
stars: neutron
X-rays: stars
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spelling Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09Méndez, Mariano R.Klis, M. van derParadijs, J. vanLewin, Walter H. G.Lamb, Frederick K.Vaughan, Brian A.Kuulkers, ErikPsaltis, DimitriosAstronomíaaccretion, accretion disksstars: individual (4U 06141091)stars: neutronX-rays: starsWe report three <i>RXTE</i>/PCA observations of the low-mass X-ray binary 4U 0614+09. They show strong (~30% rms) band-limited noise with a cutoff frequency varying between 0.7 and 15 Hz in correlation with the X-ray flux, fₓ. We observe two nonsimultaneous 11%-15% (rms) kHz peaks near 728 and 629 Hz in the power spectra of two of our observations when fₓ ~ 10<sup>-9</sup> ergs cm⁻² s⁻¹ (2-10 keV) but find no quasi-periodic oscillations (QPOs; <6% rms) when fₓ is half that. We suggest that count rate may not be a good measure for dot Ṁ even in sources as intrinsically weak as 4U 0614+09 and that QPO frequency and noise cutoff frequency track dot Ṁ more closely than count rate. The QPO increases in rms amplitude from 11% ± 1.3% at 3 keV to 37% ± 12% at 23 keV; the fractional amplitude of the band-limited noise is energy independent. This suggests different sites of origin for these two phenomena. The spectrum of the oscillating flux roughly corresponds to a black body with temperature 1.56 ± 0.2 keV and radius 500 ± 200 m (other models fit as well), which might indicate that the oscillations originate at a small region on the neutron star surface.Facultad de Ciencias Astronómicas y Geofísicas1997-08-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf37-40http://sedici.unlp.edu.ar/handle/10915/123162enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1086/310803info: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:UNLP2024-05-08T13:07:26Zoai:sedici.unlp.edu.ar:10915/123162Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292024-05-08 13:07:26.547SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
title Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
spellingShingle Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
Méndez, Mariano R.
Astronomía
accretion, accretion disks
stars: individual (4U 06141091)
stars: neutron
X-rays: stars
title_short Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
title_full Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
title_fullStr Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
title_full_unstemmed Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
title_sort Kilohertz Quasi-periodic Oscillation and Atoll Source States in 4U 0614+09
dc.creator.none.fl_str_mv Méndez, Mariano R.
Klis, M. van der
Paradijs, J. van
Lewin, Walter H. G.
Lamb, Frederick K.
Vaughan, Brian A.
Kuulkers, Erik
Psaltis, Dimitrios
author Méndez, Mariano R.
author_facet Méndez, Mariano R.
Klis, M. van der
Paradijs, J. van
Lewin, Walter H. G.
Lamb, Frederick K.
Vaughan, Brian A.
Kuulkers, Erik
Psaltis, Dimitrios
author_role author
author2 Klis, M. van der
Paradijs, J. van
Lewin, Walter H. G.
Lamb, Frederick K.
Vaughan, Brian A.
Kuulkers, Erik
Psaltis, Dimitrios
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Astronomía
accretion, accretion disks
stars: individual (4U 06141091)
stars: neutron
X-rays: stars
topic Astronomía
accretion, accretion disks
stars: individual (4U 06141091)
stars: neutron
X-rays: stars
description We report three <i>RXTE</i>/PCA observations of the low-mass X-ray binary 4U 0614+09. They show strong (~30% rms) band-limited noise with a cutoff frequency varying between 0.7 and 15 Hz in correlation with the X-ray flux, fₓ. We observe two nonsimultaneous 11%-15% (rms) kHz peaks near 728 and 629 Hz in the power spectra of two of our observations when fₓ ~ 10<sup>-9</sup> ergs cm⁻² s⁻¹ (2-10 keV) but find no quasi-periodic oscillations (QPOs; <6% rms) when fₓ is half that. We suggest that count rate may not be a good measure for dot Ṁ even in sources as intrinsically weak as 4U 0614+09 and that QPO frequency and noise cutoff frequency track dot Ṁ more closely than count rate. The QPO increases in rms amplitude from 11% ± 1.3% at 3 keV to 37% ± 12% at 23 keV; the fractional amplitude of the band-limited noise is energy independent. This suggests different sites of origin for these two phenomena. The spectrum of the oscillating flux roughly corresponds to a black body with temperature 1.56 ± 0.2 keV and radius 500 ± 200 m (other models fit as well), which might indicate that the oscillations originate at a small region on the neutron star surface.
publishDate 1997
dc.date.none.fl_str_mv 1997-08-10
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/10915/123162
url http://sedici.unlp.edu.ar/handle/10915/123162
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.1086/310803
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 application/pdf
37-40
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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score 15.812429

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