A Magnetar-Like Event From Ls I +61°303 and Its Nature as a Gamma-Ray Binary

Torres, D. F.; Rea, N.; Esposito, P.; Li, Jian; Chen, Yupeng; Zhang, Shu

doi:10.1088/0004-637x/744/2/106

Cited by 100 publications

(113 citation statements)

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“…Finally, it is worth mentioning the Swift/BAT detection of two short SGR-like bursts from the direction of the peculiar X-ray/radio/γ-ray source LS I +61 • 303 [186,15]. This is one of the very few X-ray binaries detected at GeV/TeV energies.…”

Section: Magnetars With Low External Fieldmentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the twenty AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

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Section: Magnetars With Low External Fieldmentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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“…The nature of GeV emission from these binaries is still unclear and controversial (Hadasch et al 2012;Papitto et al 2012;Torres et al 2012). They could be powered either by magnetospheric emission, as seen in many gamma-ray detected pulsars, or by electrons in the jets accelerated up to TeV energies (leptonic model; Hadasch et al 2012).…”

Section: An Lmxb Powering a Jet?mentioning

confidence: 99%

“…However, broad-band SEDs, if due to synchrotron cooling in optically thin regime, are expected to show a break at ∼500 keV, making them undetectable in the high-energy gamma-rays. The recent Fermi and AGILE detections of high-mass X-ray binaries (HMXBs; Abdo et al 2009c;Tavani et al 2009b;Ackermann et al 2012;Hadasch et al 2012), with some of them still thought to host neutron stars (NS) or BH (Hadasch et al 2012;Papitto et al 2012;Torres et al 2012) may open the possibility of detecting faint gamma-ray sources in different binary types (Hadasch et al 2012).…”

Section: Introductionmentioning

confidence: 99%

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Martino

Belloni

Falanga

et al. 2013

A&A

129

137

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Context. XSS J1227.0-4859 is a peculiar, hard X-ray source recently positionally associated to the Fermi-LAT source 1FGL J1227.9-4852/2FGL J1227.7-4853. Multi-wavelength observations have added information on this source, indicating a low-luminosity lowmass X-ray binary (LMXB), but its nature is still unclear. Aims. To progress in our understanding, we present new X-ray data from a monitoring campaign performed in 2011 with the XMM-Newton, RXTE, and Swift satellites and combine them with new gamma-ray data from the Fermi and AGILE satellites. We complement the study with simultaneous near-UV photometry from XMM-Newton and with previous UV/optical and near-IR data. Methods. We analysed the temporal characteristics in the X-rays, near-UV, and gamma rays and studied the broad-band spectral energy distribution from radio to gamma rays. Results. The X-ray history of XSS J1227 over 7 yr shows a persistent and rather stable low-luminosity (6 × 10 33 d 2 1 kpc erg s −1 ) source, with flares and dips being peculiar and permanent characteristics. The associated Fermi-LAT source 2FGL J1227.7-4853 is also stable over an overlapping period of 4.7 yr. Searches for X-ray fast pulsations down to msec give upper limits to pulse fractional amplitudes of 15 − 25% that do not rule out a fast spinning pulsar. The combined UV/optical/near-IR spectrum reveals a hot component at ∼13 kK and a cool one at ∼4.6 kK. The latter would suggest a late-type K2−K5 companion star, a distance range of 1.4−3.6 kpc, and an orbital period of 7-9 h. A near-UV variability ( 6 h) also suggests a longer orbital period than previously estimated. Conclusions. The analysis shows that the X-ray and UV/optical/near-IR emissions are more compatible with an accretion-powered compact object than with a rotational powered pulsar. The X-ray to UV bolometric luminosity ratio could be consistent with a binary hosting a neutron star, but the uncertainties in the radio data may also allow an LMXB black hole with a compact jet. In this case, it would be the first associated with a high-energy gamma-ray source.

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“…Magnetar bursts can be empirically divided into three main classes (although there is probably a continuum among them): the short bursts (∼0.01-1 s; 10 37 -10 40 erg s −1 ), the intermediate bursts (∼5-50 s; 10 40 -10 42 erg s −1 ), and the giant flares (∼100-500 s; 10 43 -10 47 erg s −1 ). Torres et al (2012) have started to study how a high-field NS could cope with the multi-wavelength phenomenology of LS I +61…”

Section: Introduction Ls I +61mentioning

confidence: 99%

Possible Changes of State and Relevant Timescales for a Neutron Star in Ls I +61°303

Papitto

Torres

Rea

2012

ApJ

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The properties of the short, energetic bursts recently observed from the γ -ray binary LS I +61• 303 are typical of those showed by high magnetic field neutron stars (NSs) and thus provide a strong indication in favor of a NS being the compact object in the system. Here, we discuss the transitions among the states accessible to a NS in a system like LS I +61• 303, such as the ejector, propeller, and accretor phases, depending on the NS spin period, magnetic field, and rate of mass captured. We show how the observed bolometric luminosity ( few × 10 35 erg s −1 ) and its broadband spectral distribution indicate that the compact object is most probably close to the transition between working as an ejector all along its orbit and being powered by the propeller effect when it is close to the orbit periastron, in a so-called flip-flop state. By assessing the torques acting onto the compact object in the various states, we follow the spin evolution of the system, evaluating the time spent by the system in each of them. Even taking into account the constraint set by the observed γ -ray luminosity, we found that the total age of the system is compatible with being ≈5-10 kyr, comparable to the typical spin-down ages of high-field NSs. The results obtained are discussed in the context of the various evolutionary stages expected for a NS with a high-mass companion.

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A Magnetar-Like Event From Ls I +61°303 and Its Nature as a Gamma-Ray Binary

Cited by 100 publications

References 112 publications

Pulsars and Magnetars

Pulsars and Magnetars

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Possible Changes of State and Relevant Timescales for a Neutron Star in Ls I +61°303

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