Discovery of 3·6-s X-ray pulsations from 4U0115+63

Cominsky, L.; Clark, G. W.; Li, F.; Mayer, W.; Rappaport, S.

doi:10.1038/273367a0

Cited by 52 publications

(36 citation statements)

References 18 publications

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“…During the SAS-3 observations in 1978, Cominsky et al (1978) found a pulsation period of 3.61 sec. Rappaport et al (1978) determined the binary's main parameters: orbital period ∼ 24.3 days, orbital eccentricity 0.34, and projected semimajor axis of the relativistic object axsini ∼ 140 light seconds (see also Tamura et al, 1992;Lutovinov et al, 1994, for an improvement of the parameters).…”

Section: Discussionmentioning

confidence: 98%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: Discussionmentioning

confidence: 98%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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“…On that occasion the X-ray luminosity of the source rose to > ∼ 10 37 erg s −1 , a value that is about two orders of magnitude higher than its typical quiescent level. X-ray pulsations at a period of P S = 3.6 s were reported first by Cominsky et al (1978). Rappaport et al (1978) measured later the orbital parameters of the system by using SAS data, and estimated an orbital period of P orb = 24.3 d, an eccentricity of e = 0.34, and a value of the semi-major axis of the orbit of a X sin i = 140.1 lt − s. Here i is the unknown inclination angle between the normal to the plane of the orbit and the line of sight to the observer.…”

Section: U 0115+63mentioning

confidence: 93%

4U 0115 + 63: phase lags and cyclotron resonant scattering

Ferrigno

Falanga

Bozzo

et al. 2011

A&A

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Context. High-mass X-ray binaries are among the brightest objects of our Galaxy in the high-energy domain (0.1-100 keV). Despite our relatively good knowledge of their basic emission mechanisms, the complex problem of understanding their time-and energydependent X-ray emission has not been completely solved. Aims. In this paper, we study the energy-dependent pulse profiles of the high-mass X-ray binary pulsar 4U 0115+63 to investigate how they are affected by cyclotron resonant scattering. Methods. We analyzed archival BeppoSAX and RXTE observations performed during the giant outburst of the source that occurred in 1999. We exploited a cross correlation technique to compare the pulse profiles in different energy ranges and developed a relativistic ray-tracing model to interpret our findings. We also studied the phase dependency of the cyclotron absorption features by performing phase-resolved spectroscopy. Results. The pulse profiles of 4U 0115+63 displayed clear "phase-lags" at energies close to those of the cyclotron absorption features that characterize the X-ray emission of the source. We reproduce this phenomenon qualitatively by assuming an energy-dependent beaming of the emission from the column surface and verify that our model is also compatible with the results of phase-resolved spectral analysis. Conclusions. We show that cyclotron resonant scattering affects the pulse profile formation mechanisms in a complex way, which necessitates both improvements in the modeling and the study of other sources to be better understood.

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“…The subsequent analysis of the archival data of the Vela 5B satellite revealed that the source had also been detected in 1969 (Whitlock et al 1989). Rappaport et al (1978) measured the orbital motion of the source from observations with the SAS 3 satellite in 1978, obtaining an orbital period of 24.3 d, while Cominsky et al (1978) detected pulsations with a pulse period of 3.61 s. Soon thereafter, a strongly reddened Be-star V635 Cas was found as its optical counterpart (Johns et al 1978;Hutchings & Crampton 1981;Kholopov et al 1981). This star was later classified as a B0.2Ve star at a distance of 7-8 kpc (Negueruela & Okazaki 2001).…”

Section: U 0115+63mentioning

confidence: 99%

Analysing X-ray pulsar profiles

Sasaki¹,

Müller²,

Kraus³

et al. 2012

A&A

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Aims. By analysing the asymmetric pulse profiles of the transient Be/X-ray binaries 4U 0115+63 and V 0332+53 we aim to identify the origin of the pulsed emission to understand the geometry of the accretion onto the neutron star. Methods. We have applied the pulse-profile decomposition method, which enabled us to find two symmetric pulse profiles for the two magnetic poles of the neutron star. We derived beam patterns for different energy bands and luminosity states. This allowed us to identify the components that are responsible for the emission. The analysis and the models used for the interpretation of the results take relativistic light deflection into account. Results. We find that the magnetic field of the neutron star is distorted in both 4U 0115+63 and V 0332+53. The beam patterns are interpreted in terms of a model for an accretion column that includes the formation of a halo at the bottom of the accretion column and scattering in the upper accretion stream. Conclusions. In both systems, an accretion column forms while the accretion rate is high. If the accretion decreases and the sources become fainter, the emission from the halo and the accretion column disappears. In 4U 0115+63 there seems to be significant scattering of photons in the still existing accretion stream even at the end of the outburst. In V 0332+53, the scattering in the upper stream also disappears at the end and we apparently observe the emission from the hot spots on the neutron star.

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Discovery of 3·6-s X-ray pulsations from 4U0115+63

Cited by 52 publications

References 18 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

4U 0115 + 63: phase lags and cyclotron resonant scattering

Analysing X-ray pulsar profiles

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