A 0535+26: back in business

Coe, M. J.; Reig, P.; McBride, V. A.; Galache, J. L.; Fabregat, J.

doi:10.1111/j.1365-2966.2006.10127.x

Cited by 53 publications

(96 citation statements)

References 26 publications

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“…The system has been frequently observed to undergo transient X-ray flares with a wide range of intensities. In fact, very recently it underwent another major outburst that was detected with instruments of the Rossi X-ray Timing Explorer (Coe et al 2006). The simultaneity of X-ray activity with transitions between infrared states strongly suggests that these outbursts occur in relation with increments of the accretion rate onto the neutron star.…”

Section: A Case Of Study: A0535+26mentioning

confidence: 99%

Very high energy γ-ray emission from X-ray transients during major outbursts

Orellana

Romero

Pellizza

et al. 2007

A&A

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Context. Some high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called "Approximation A" to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal.

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Section: A Case Of Study: A0535+26mentioning

confidence: 99%

Very high energy γ-ray emission from X-ray transients during major outbursts

Orellana

Romero

Pellizza

et al. 2007

A&A

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“…Then, both magnitudes peaked in this period, and afterward a dramatic decrease took place, which continued through 2011 March. Furthermore, the shape of the Hα profile was more simple around 2009, evolving from a clear double structure (Coe et al 2006) to a single peak. Later on, a double-peaked structure is observed (see Figure 4).…”

Section: Optical Measurementsmentioning

confidence: 99%

“…Then A 0535+26 went back to quiescence for almost 11 years. Only a few observations were reported during that period (Coe et al 2006;Hill et al 2007;Negueruela et al 2000;Orlandini et al 2004). The source renewed activity in 2005 May with another giant outburst and two normal outbursts.…”

Section: Observations and Analysismentioning

confidence: 99%

“…We transformed the HIPPARCOS filter to visual magnitude, following the procedure found in Harmanec (1998) and applying B − V and U − B values from Lyuty & Zaitseva (2000). We computed the V magnitude from Coe et al (2006) based on the work done by Grundstrom et al (2007). As we mentioned before, the spectroscopic observations come from the 2 m telescope at LT and the 2.16 m telescope at NAOC.…”

Section: Observations and Analysismentioning

confidence: 99%

“…Whether or not type I or II outbursts are produced depends on the eccentricity of the system. For the case of the moderate eccentricity of A 0535+26 (e = 0.47), both types of behavior are possible as the disk expands and contracts between different resonant radii (Haigh et al 2004;Coe et al 2006). We would therefore expect some correlation between the disk status as inferred from Hα equivalent width (EW) and profile and the presence or otherwise of X-ray outbursts.…”

Section: Introductionmentioning

confidence: 99%

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X-Ray and Optical Observations of a 0535+26

Camero-Arranz

Finger

Wilson-Hodge

et al. 2012

ApJ

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We present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A 0535+26 with the Fermi/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data (since ∼1978) and discussed in terms of the neutron-star-Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray quasi-periodic oscillation was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25 keV. In the long term a strong optical/X-ray correlation was found for this system, however in the medium term the Hα equivalent width and the V-band brightness showed an anti-correlation after ∼2002 August. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the Hα showed a strong emission. In late 2010 and before the 2011 February outburst, rapid V /R variations are observed in the strength of the two peaks of the Hα line. These had a period of ∼25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V /R variability beginning ∼6 months following a giant outburst.

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Tidal interaction in High‐Mass X‐ray Binaries

Stoyanov

Zamanov

2009

Astron Nachr

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Our aim is to investigate tidal interaction in High-Mass X-ray Binary stars in order to determine in which objects the rotation of the mass donors is synchronized or pseudosynchronized with the orbital motion of the compact companion. We calculate the pseudosynchronization period (Pps) and compare it with the rotational period of the mass donors (Prot). We find that (1) the Be/X-ray binaries are not synchronized, the mass donors rotate faster than the orbital period and the ratio Pps/Prot is 2 -300; (2) the giant and supergiant systems are close to synchronization and for them the ratio Pps/Prot is 0.3 -2.

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A 0535+26: back in business

Cited by 53 publications

References 26 publications

Very high energy γ-ray emission from X-ray transients during major outbursts

Very high energy γ-ray emission from X-ray transients during major outbursts

X-Ray and Optical Observations of a 0535+26

Tidal interaction in High‐Mass X‐ray Binaries

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