X-Ray and Optical Observations of a 0535+26

Camero-Arranz, A.; Finger, Mark H.; Wilson-Hodge, C.; Jenke, P.; Steele, I. A.; Coe, M. J.; Gutiérrez‐Soto, J.; Kretschmar, P.; Caballero, I.; Yan, Jing-Zhi; Rodríguez, J.; Suso, J.; Case, G.; Cherry, M. L.; Guiriec, S.; McBride, V. A.

doi:10.1088/0004-637x/754/1/20

Cited by 54 publications

(82 citation statements)

References 69 publications

(130 reference statements)

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“…A similar long-term behavior was detected in A0535+26 by Camero-Arranz et al (2012, see also Bildsten et al 1997. Such a long-term spin-down might be evidence for the "propeller" regime, where matter near the neutron star is expelled, removing angular momentum and causing the neutron star to spin down (Illarionov & Sunyaev 1975;Frank et al 1992;Bildsten et al 1997).…”

Section: Discussionsupporting

confidence: 71%

“…This discrepancy at high luminosities during the 2007 outburst can be explained by assuming that during this phase the pulsar underwent a spin-up, i.e.,Ṗ 0 s s −1 andP 0 s s −2 , between MJD 54 426 and MJD 54 434. This approach is not unreasonable since high-luminosity phases are coincident with a high angular momentum transfer onto the neutron star, which has been detected in other transient X-ray binaries as well, e.g., A0535+26 (Camero-Arranz et al 2012).…”

Section: Orbit Of Gro J1008−57mentioning

confidence: 99%

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GRO J1008−57: an (almost) predictable transient X-ray binary

Kühnel

Müller

Kreykenbohm

et al. 2013

A&A

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A study of archival RXTE, Swift, and Suzaku pointed observations of the transient high-mass X-ray binary GRO J1008−57 is presented. A new orbital ephemeris based on pulse arrival-timing shows the times of maximum luminosities during outbursts of GRO J1008−57 to be close to periastron at orbital phase −0.03. This makes the source one of a few for which outburst dates can be predicted with very high precision. Spectra of the source in 2005, 2007, and 2011 can be well described by a simple power law with high-energy cutoff and an additional black body at lower energies. The photon index of the power law and the black-body flux only depend on the 15-50 keV source flux. No apparent hysteresis effects are seen. These correlations allow us to predict the evolution of the pulsar's X-ray spectral shape over all outbursts as a function of just one parameter, the source's flux. If modified by an additional soft component, this prediction even holds during GRO J1008−57's 2012 type II outburst.

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Section: Discussionsupporting

confidence: 71%

Section: Orbit Of Gro J1008−57mentioning

confidence: 99%

GRO J1008−57: an (almost) predictable transient X-ray binary

Kühnel

Müller

Kreykenbohm

et al. 2013

A&A

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“…The QPO frequency was found to be correlated with flux, as was recently confirmed by Fermi GBM observations in similar energy range (Camero-Arranz et al 2012). This allowed the association of the QPOs with the inner edge of the accretion disk and the magnetosphere boundary (Finger et al 1996;Camero-Arranz et al 2012), although there are some problems with this interpretation.…”

Section: Introductionsupporting

confidence: 68%

“…During the 1994 giant outburst, quasiperiodical oscillations (QPOs) with frequency in the range 27−72 mHz have been observed in the source's hard (20−50 keV) X-ray light curve (Finger et al 1996). The QPO frequency was found to be correlated with flux, as was recently confirmed by Fermi GBM observations in similar energy range (Camero-Arranz et al 2012). This allowed the association of the QPOs with the inner edge of the accretion disk and the magnetosphere boundary (Finger et al 1996;Camero-Arranz et al 2012), although there are some problems with this interpretation.…”

Section: Introductionsupporting

confidence: 54%

XMM-Newtonobservations of 1A 0535+262 in quiescence

Doroshenko

Santangelo

Doroshenko

et al. 2014

A&A

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Accretion onto magnetized neutron stars is expected to be centrifugally inhibited at low accretion rates. Several sources, however, are known to pulsate in quiescence at luminosities below the theoretical limit predicted for the onset of the centrifugal barrier. The source 1A 0535+262 is one of them. Here we present the results of an analysis of a ∼50 ks long XMM-Newton observation of 1A 0535+262 in quiescence. At the time of the observation, the neutron star was close to apastron, and the source had remained quiet for two orbital cycles. In spite of this, we detected a pulsed X-ray flux of ∼3 × 10 −11 erg cm −2 s −1 . Several observed properties, including the power spectrum, remained similar to those observed in the outbursts. Particularly, we have found that the frequency of the break detected in the quiescent noise power spectrum follows the same correlation with flux observed when the source is in outburst. This correlation has been associated with the truncation of the accretion disk at the magnetosphere boundary. We argue that our result, along with other arguments previously reported in the literature, suggests that the accretion in quiescence also proceeds from an accretion disk around the neutron star. The proposed scenario consistently explains the energy of the cyclotron line observed in 1A 0535+262, and the timing properties of the source including the spin frequency evolution within and between the outbursts, and the frequency of the break in power spectrum.

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“…Case et al (2011b) have presented initial results, with positive identification above 100 keV of six persistent sources (the Crab, Cyg X−1, SWIFT J1753.5−0127, 1E 1740−29, Cen A, and GRS 1915+105) and two transient sources (GX 339−4 and XTE J1752−223). Wilson-Hodge et al (2011a) used the GBM occultation measurements to demonstrate that the 15-100 keV flux from the Crab had decreased by approximately 7% over the time from launch through 2010 August, and Camero-Arranz et al (2012) have presented the GBM observations of the transient Be/X-ray binary system A0535+26. The present paper describes the GBM approach in detail and presents the results of the first three years of GBM Earth occultation measurements.…”

Section: Introductionmentioning

confidence: 99%

THREE YEARS OF FERMI GBM EARTH OCCULTATION MONITORING: OBSERVATIONS OF HARD X-RAY/SOFT GAMMA-RAY SOURCES

Wilson-Hodge

Case

Cherry

et al. 2012

ApJS

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The Gamma-ray Burst Monitor (GBM) on board Fermi has been providing continuous data to the astronomical community since 2008 August 12. In this paper, we present the results of the analysis of the first three years of these continuous data using the Earth occultation technique to monitor a catalog of 209 sources. From this catalog, we detect 99 sources, including 40 low-mass X-ray binary/neutron star systems, 31 high-mass X-ray binary/neutron star systems, 12 black hole binaries, 12 active galaxies, and 2 other sources, plus the Crab Nebula, and the Sun. Nine of these sources are detected in the 100-300 keV band, including seven black hole binaries, the active galaxy Cen A, and the Crab. The Crab and Cyg X-1 are also detected in the 300-500 keV band. GBM provides complementary data to other sky-monitors below 100 keV and is the only all-sky monitor above 100 keV. Up-to-date light curves for all of the catalog sources can be found online.

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X-Ray and Optical Observations of a 0535+26

Cited by 54 publications

References 69 publications

GRO J1008−57: an (almost) predictable transient X-ray binary

GRO J1008−57: an (almost) predictable transient X-ray binary

XMM-Newtonobservations of 1A 0535+262 in quiescence

THREE YEARS OF FERMI GBM EARTH OCCULTATION MONITORING: OBSERVATIONS OF HARD X-RAY/SOFT GAMMA-RAY SOURCES

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