The MIT/OSO 7 catalog of X-ray sources - Intensities, spectra, and long-term variability

Markert, T. H.; Laird, F. N.; Clark, G. W.; Hearn, D. R.; Sprott, G. F.; Li, F. K.; Bradt, H.; Lewin, W. H. G.; Schnopper, H. W.; Winkler, P. F.

doi:10.1086/190587

Cited by 49 publications

(34 citation statements)

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“…To investigate the long-term evolution of RX J1037.5-5647, we considered all the X-ray flux measurements obtained for this source since its discovery in the early 70s. For the UHURU (Forman et al 1978), OSO 7 (Markert et al 1979) and ARIEL V (Warwick et al 1981) detections, we used the published CR values and the appropriate count-rate-to-flux conversion factors to obtain the corresponding 2-10 keV fluxes. In the case of the RossiXTE All Sky Monitor (ASM), we considered the day-by-day light curve, which covers the time interval from January 1996 to March 2009.…”

Section: Discussionmentioning

confidence: 99%

XMM-Newton observation of the persistent Be/NS X-ray binary pulsar RX J1037.5–5647 in a low luminosity state

Palombara¹,

Sidoli²,

Esposito

et al. 2009

A&A

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The spectra of several X-ray binary pulsars display a clear soft excess, which in most cases can be described with a blackbody model, above the main power-law component. While in the high-luminosity sources it is usually characterized by low temperature (kT < 0.5 keV) and a large emission radius (R > 100 km), in the two persistent and low-luminosity pulsars 4U 0352+309 and RX J0146.9+6121 this component has a high temperature (kT > 1 keV) and a smaller radius (R < 0.5 km), consistent with the estimated size of the neutron-star polar cap. Here we report on the timing and spectral analysis of RX J1037.5-5647, another lowluminosity persistent Be binary pulsar, based on the first XMM-Newton observation of this source. We have found a best-fit period P = 853.4 ± 0.2 s, which implies an average pulsar spin-upṖ −2 × 10 −8 s s −1 in the last decade. The estimated source luminosity is L X ∼ 10 34 erg s −1 , a value comparable to the other persistent Be binary pulsars and about one order of magnitude lower than in most of the previous measurements. The source spectrum can be described with a power law plus blackbody model, with kT BB = 1.26 +0.16 −0.09 keV and R BB = 128 +13 −21 m, suggesting a polar-cap origin of this component. These results strengthen the hypothesis that, in addition to low luminosities and long periods, this class of sources is also characterized by common spectral properties.

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Section: Discussionmentioning

confidence: 99%

XMM-Newton observation of the persistent Be/NS X-ray binary pulsar RX J1037.5–5647 in a low luminosity state

Palombara¹,

Sidoli²,

Esposito

et al. 2009

A&A

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“…Further long-term broad-band X-ray behaviour 4U 0614+091 was discovered by UHURU with variable flux levels between about 15 and 70 mCrab (2−6 keV; Giacconi et al 1972). Other early measurements of the flux, besides those from UHURU, may be found in, e.g., Mason et al (1976), Swank et al (1978), Parsignault & Grindlay (1978), Markert et al (1979), and Warwick et al (1981). In that time it was always seen at a flux of about 10−100 mCrab in roughly the ∼2 to ∼10 keV band.…”

Section: Asm Long-term Persistent Flux and Burst Recurrence Timesmentioning

confidence: 92%

What ignites on the neutron star of 4U 0614+091?

Kuulkers¹,

Zand

Atteia

et al. 2010

A&A

103

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The low-mass X-ray binary 4U 0614+091 is a source of sporadic thermonuclear (type I) X-ray bursts. We find bursts with a wide variety of characteristics in serendipitous wide-field X-ray observations by the WATCH on EURECA, the ASM on RXTE, the WFCs on BeppoSAX, the FREGATE on HETE-2, the IBIS/ISGRI on INTEGRAL, and the BAT on Swift, as well as pointed observations with the PCA and HEXTE on RXTE. Most of the bursts are bright, i.e., they reach a peak flux of about 15 Crab, but a few are weak and only reach a peak flux below a Crab. One of the bursts shows a very strong photospheric radius-expansion phase. This allows us to evaluate the distance to the source, which we estimate to be 3.2 kpc. The burst durations vary generally from about 10 s to 5 min. However, after one of the intermediate-duration bursts, a faint tail is seen to at least about 2.4 h after the start of the burst. One very long burst was observed, which lasted for several hours. This superburst candidate was followed by a normal type-I burst only 19 days later. This is, to our knowledge, the shortest burst-quench time among the superbursters. The observation of a superburst in this system is difficult to reconcile if the system is accreting at about 1% of the Eddington limit. We describe the burst properties in relation to the persistent emission. No strong correlations are apparent, except that the intermediate-duration bursts occurred when 4U 0614+091's persistent emission was lowest and calm, and when bursts were infrequent (on average roughly one every month to 3 months). The average burst rate increased significantly after this period. The maximum average burst recurrence rate is about once every week to 2 weeks. The burst behaviour may be partly understood if there is at least an appreciable amount of helium present in the accreted material from the donor star. If the system is an ultra-compact X-ray binary with a CO white-dwarf donor, as has been suggested, this is unexpected. If the bursts are powered by helium, we find that the energy production per accumulated mass is about 2.5 times less than expected for pure helium matter.

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“…All the values listed below are absorbed fluxes in the 2-10 keV band, unless otherwise stated. The HEAO-1 (Wood et al 1984) flux is 6.58 ± 0.07 × 10 −13 W m −2 (15.8.1977 to 15.2.1978), Ariel V (Warwick et al 1981) 6.9 ± 0.07 × 10 (15.10.1974 to 14.3.1980), varying between 3.0-12.0 × 10 −13 W m −2 , OSO-7 (Markert et al 1979) 8.09 ± 0.85 × 10 −13 W m −2 (October 1971 to May 1973) and UHURU (Forman et al 1978) 12.12.1970 to 18.3.1973). Einstein observations on 17.3.1979 (Christian & Swank 1997) …”

Section: Temporal Variability Analysismentioning

confidence: 99%

X-ray properties of 4U 1543–624

Schultz

2002

A&A

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Abstract. 4U 1543-624 is a relatively bright persistent low-mass X-ray binary. Analysis of archival data from ASCA, SAX and RXTE is presented. The X-ray continuum be can modeled with the standard low-mass X-ray binary spectrum, an isothermal blackbody and a Comptonized component. Variations in the luminosity and flux ratio of the continuum components are seen. An increase in luminosity is accompanied by a decrease in the blackbody luminosity and a hardening of the spectrum. Most low-mass X-ray binaries have softer spectra and higher blackbody luminosities in high luminosity states. The Fe K α line is seen only in the high luminosity spectra. A narrow feature near 0.7 keV, previously detected in the ASCA data, is also seen in the SAX data. A qualitative model of the system is presented. The X-ray observations can be explained by a low inclination system (face-on disk) containing a slowly (P ms) rotating neutron star. A slowly rotating neutron star would imply either that the system is a young low-mass X-ray binary, or that the accretion rate is unusually low. The empirical relation between optical and X-ray luminosity and orbital period suggests a relatively short period.

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The MIT/OSO 7 catalog of X-ray sources - Intensities, spectra, and long-term variability

Cited by 49 publications

References 0 publications

XMM-Newton observation of the persistent Be/NS X-ray binary pulsar RX J1037.5–5647 in a low luminosity state

XMM-Newton observation of the persistent Be/NS X-ray binary pulsar RX J1037.5–5647 in a low luminosity state

What ignites on the neutron star of 4U 0614+091?

X-ray properties of 4U 1543–624

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