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dc.contributor.author
Alabarta, K.
dc.contributor.author
Altamirano, D.
dc.contributor.author
Méndez, M.
dc.contributor.author
Cúneo, V. A.
dc.contributor.author
Vincentelli, F. M.
dc.contributor.author
Castro Segura, N.
dc.contributor.author
García, Federico
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dc.contributor.author
Luff, B.
dc.contributor.author
Veledina, A.
dc.date.available
2022-06-03T13:49:18Z
dc.date.issued
2021-11
dc.identifier.citation
Alabarta, K.; Altamirano, D.; Méndez, M.; Cúneo, V. A.; Vincentelli, F. M.; et al.; Failed-transition outbursts in black hole low-mass X-ray binaries; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 507; 4; 11-2021; 5507-5522
dc.identifier.issn
0035-8711
dc.identifier.uri
http://hdl.handle.net/11336/158855
dc.description.abstract
Black hole low-mass X-ray binaries (BH LMXBs) evolve in a similar way during outburst. Based on the X-ray spectrum and variability, this evolution can be divided into three canonical states: low/hard, intermediate, and high/soft state. BH LMXBs evolve from the low/hard to the high/soft state through the intermediate state in some outbursts (here called ´full outbursts´). However, in other cases, BH LMXBs undergo outbursts in which the source never reaches the high/soft state, here called ´failed-transition outbursts´ (FT outbursts). From a sample of 56 BH LMXBs undergoing 128 outbursts, we find that 36 per cent of these BH LMXBs experienced at least one FT outburst, and that FT outbursts represent ∼33 per cent of the outbursts of the sample, showing that these are common events. We compare all the available X-ray data of full and FT outbursts of BH LMXBs from RXTE/PCA, Swift/BAT, and MAXI, and find that FT and full outbursts cannot be distinguished from their X-ray light curves, hardness-intensity diagrams, or X-ray variability during the initial 10-60 d after the outburst onset. This suggests that both types of outbursts are driven by the same physical process. We also compare the optical and infrared (O/IR) data of FT and full outbursts of GX 339-4. We found that this system is generally brighter in O/IR bands before an FT outburst, suggesting that the O/IR flux points to the physical process that later leads to a full or an FT outburst. We discuss our results in the context of models that describe the onset and evolution of outbursts in accreting X-ray binaries.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Wiley Blackwell Publishing, Inc
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
ACCRETION, ACCRETION DISCS
dc.subject
BLACK HOLE PHYSICS
dc.subject
X-RAYS: BINARIES
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Failed-transition outbursts in black hole low-mass X-ray binaries
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2022-05-06T15:38:09Z
dc.journal.volume
507
dc.journal.number
4
dc.journal.pagination
5507-5522
dc.journal.pais
Reino Unido
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dc.description.fil
Fil: Alabarta, K.. University of Southampton; Reino Unido
dc.description.fil
Fil: Altamirano, D.. University of Southampton; Reino Unido
dc.description.fil
Fil: Méndez, M.. University of Groningen; Países Bajos
dc.description.fil
Fil: Cúneo, V. A.. Universidad de La Laguna; España
dc.description.fil
Fil: Vincentelli, F. M.. University of Southampton; Reino Unido
dc.description.fil
Fil: Castro Segura, N.. University of Southampton; Reino Unido
dc.description.fil
Fil: García, Federico. University of Groningen; Países Bajos
dc.description.fil
Fil: Luff, B.. University of Southampton; Reino Unido
dc.description.fil
Fil: Veledina, A.. Royal Institute of Technology; Suecia. University of Turku; Finlandia
dc.journal.title
Monthly Notices of the Royal Astronomical Society
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1093/mnras/stab2241
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/507/4/5507/6352347
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