Positions of galactic X-ray sources: 55° &lt; lII &lt; 320°

Dower, R. G.; Apparao, K. M. V.; Bradt, H.; Doxsey, R.; Jernigan, J. G.; Kulik, Joanna

doi:10.1038/273364a0

Cited by 30 publications

(12 citation statements)

References 36 publications

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“…A more precise value of the pulse period (292.4 s) was provided by Nagase (1989). The optical counterpart of H 1145-619, Hen 3-715, was discovered in 1978(Dower et al 1978) and classified as a 9-mag B1 Ve (Stevens et al 1997). This system is one of the closest Be/XBs, as it is located at 3.1 ± 0.5 kpc from Earth (Stevens et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

Alfonso-Garzón

Fabregat

Reig

et al. 2017

A&A

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Context. Multiwavelength monitoring of Be/X-ray binaries is crucial to understand the mechanisms producing their outbursts. H 1145-619 is one of these systems, which has recently displayed X-ray activity. Aims. We investigate the correlation between the optical emission and X-ray activity to predict the occurrence of new X-ray outbursts from the inferred state of the circumstellar disc. Methods. We have performed a multiwavelength study of H 1145-619 from 1973 to 2017 and present here a global analysis of its variability over the last 40 yr. We used optical spectra from the SAAO, SMARTS, and SALT telescopes and optical photometry from the Optical Monitoring Camera (OMC) onboard INTEGRAL and from the All Sky Automated Survey (ASAS). We also used X-ray observations from INTEGRAL/JEM-X, and IBIS to generate the light curves and combined them with Swift/XRT to extract the X-ray spectra. In addition, we compiled archival observations and measurements from the literature to complement these data.Results. Comparing the evolution of the optical continuum emission with the Hα line variability, we identified three different patterns of optical variability: first, global increases and decreases of the optical brightness, observed from 1982 to 1994 and from 2009 to 2017, which can be explained by the dissipation and replenishment of the circumstellar disc; second, superorbital variations with a period of P superorb ≈ 590 days, observed in 2002-2009, which seems to be related to the circumstellar disc; and third, optical outbursts, observed in 1998-1999 and 2002-2005, which we interpret as mass ejections from the Be star. We discovered the presence of a retrograde one-armed density wave, which appeared in 2016 and is still present in the circumstellar disc. Conclusions. We carried out the most complete long-term optical study of the Be/X-ray binary H 1145-619 in correlation with its X-ray activity. For the first time, we found the presence of a retrograde density perturbation in the circumstellar disc of a Be/X-ray binary.

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Section: Introductionmentioning

confidence: 99%

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

Alfonso-Garzón

Fabregat

Reig

et al. 2017

A&A

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“…It was discovered by the SAS-3 satellite Deceased. (Dower et al 1978) and extensively observed in the X-ray band by several spacecraft.…”

Section: Introductionmentioning

confidence: 99%

TheBeppoSAXview of the galactic high-mass X-ray binary 4U 0114+65

Masetti¹,

Orlandini²,

Fiume³

et al. 2005

A&A

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A pointed observation of the galactic high-mass X-ray binary 4U 0114+65 was carried out with BeppoSAX to compare the X-ray spectral and timing characteristics observed by this satellite over the broadest range of energies thus far (1.5-100 keV) with the information previously obtained with other spacecraft. The light curve of 4U 0114+65 shows a large flare at the beginning of the BeppoSAX pointing and no significant hardness evolution either during the flare or in the low state occurring after the flare itself. The modulation at ∼2.7 h, attributed to the accreting neutron star (NS) spin periodicity, is not significantly detected in our data, although fluctuations with timescales of ∼3 h can be seen in the 2-10 keV light curve. Shorter modulations down to timescales of minutes are also found and interpreted as due to accretion of matter onto the NS. The flaring and the low state spectra of 4U 0114+65 can be equally well fitted either with a power law modulated by a high-energy exponential cutoff or with a Comptonization model. During the low state the presence, although tentative, of a thermal component (with kT ∼ 0.3 keV) at low energies, possibly produced by an ionized plasma cloud around the NS, cannot be excluded. Contrary to previous claims, a cyclotron resonant feature in absorption at ∼22 keV was not detected in the BeppoSAX spectroscopic data, whereas evidence for a Fe emission line around 6.4 keV is found only during the low state emission. Using all of the above information, a scenario for the system in which the NS is embedded in, and accreting from, a low angular momentum gas cloud is envisaged.

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“…4U 1145À619 is a %292 s transient pulsar associated with a B1 Vne star (V801 Cen; Bradt et al 1977;Dower et al 1978). The X-ray source exhibits outbursts periodically, at 186.5 day intervals, likely the binary orbital period ( Watson et al 1981;Priedhorsky & Terrell 1983).…”

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Pulsations Detected from Accreting High‐Mass X‐Ray Binaries at Low Luminosities

Rutledge¹,

Bildsten²,

Brown³

et al. 2007

ApJ

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We report the detection of pulsations from two accreting transient high-mass X-ray binaries (HMXBs) at low X-ray luminosities (%1Y 4 ; 10 34 ergs s À1). While one (4U 1145À619) has been detected pulsing previously at a lower luminosity, the second (1A 1118À615) has not, making it the third such transient HMXB from which pulsations are detected at low luminosity. The pulsars exhibit broadband rms variability (22:3% AE 0:1% and 9:2% AE 0:1%, respectively). While the present observations do not permit measurement of a spin frequency derivative, spin-down is implied in comparison with previous Compton Gamma Ray Observatory/ BATSE observations. If spin-down occurred at the presently observed X-ray luminosity of 4U 1145À619, the required mass accretion rate is insufficient to produce the observed X-ray luminosity from a shock at the magnetosphere, and only a fraction of the mass accretion makes its way to the neutron star surface, with most of the mass leaving the system, carrying away angular momentum to affect spin-down.

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Positions of galactic X-ray sources: 55° < lII < 320°

Cited by 30 publications

References 36 publications

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

Long-term optical and X-ray variability of the Be/X-ray binary H 1145-619: Discovery of an ongoing retrograde density wave

TheBeppoSAXview of the galactic high-mass X-ray binary 4U 0114+65

Pulsations Detected from Accreting High‐Mass X‐Ray Binaries at Low Luminosities

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