Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission

Bałucińska‐Church, M.; Schulz, Norbert S.; Wilms, J.; Gibiec, A.; Hanke, Manfred; Spencer, R. E.; Rushton, A.; Church, M. J.

doi:10.1051/0004-6361/201015931

Cited by 13 publications

(11 citation statements)

References 41 publications

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“…showing a clear correlation with Z-track position (Hjellming et al 1990a). Similarly, Ba lucińska- Church et al (2011) found a 5σ upper limit of < 150 µJy at 5 GHz in e-EVN observations in 2009, May. Sco X-1 on the other hand has both radio-loud and radio-weak states and weak radio emission has been detected when on the FB (Hjellming et al 1990b).…”

Section: A Model For the Sco X-1 Like Sourcesmentioning

confidence: 76%

“…In multi-wavelength observations of Cygnus X-2 in 2009 (Ba lucińska- Church et al 2011) a series of absorption edges below 1.4 keV remarkably had no detectable increase in depth during dips, showing that part of the continuum emission had to be extended so that part was not covered, while covered emission below 1.4 keV was completely removed.…”

Section: The Extended Adcmentioning

confidence: 99%

“…However, there has been some confusion in the Cyg-like sources between dipping and flaring in that reductions in X-ray intensity in dipping (seen in hardness-intensity) when plotted in colour-colour look like a FB. In Cyg X-2 recent multi-wavelength observations show that intensity reductions were indeed absorption dips unrelated to flaring (Ba lucińska- Church et al 2011Church et al , 2012. In GX 340+0 and GX 5-1, a 4th track has been seen at the end of the FB with decreasing intensity suggesting a dipping-flaring link.…”

Section: A Monotonic Variation Of Mass Accretion Rate ?mentioning

confidence: 99%

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Spectral investigations of the nature of the Scorpius X-1 like sources

Church

Gibiec

Bałucińska‐Church

et al. 2012

A&A

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We present results of spectral investigations of the Sco X-1 like Z-track sources Sco X-1, GX 349+2, and GX 17+2 based on Rossi-XTE (RXTE) observations determining spectral evolution along the Z-track. Results are obtained for a spectral model describing an extended accretion disk corona. The results are compared with previous results for the Cyg X-2 like group: Cyg X-2, GX 340+0, and GX 5-1 and a general model for the Z-track sources proposed. On the normal branch, the Sco-like and Cyg-like sources are similar, the results indicating an increase of mass accretion rateṀ between soft and hard apex, not as in the standard view that this increases monotonically around the Z. In the Cyg-like sources, increasingṀ causes the neutron star temperature kT to increase from ∼1 to ∼2 keV. At the lower temperature, the radiation pressure is small, but at the higher kT , the emitted flux of the neutron star is several times super-Eddington and the high radiation pressure disrupts the inner disk and launches the relativistic jets observed on the upper normal and horizontal branches. In the Sco-like sources, the main physical difference is the high kT of more than 2 keV on all parts of the Z-track suggesting jets are always possible, even on the flaring branch. The flaring branch in the Cyg-like sources is associated with a release of energy on the neutron star consistent with unstable nuclear burning. The Sco-like sources are very different as flaring appears to be a combination of unstable burning and an increase ofṀ which makes flaring much stronger. Analysis of 15 years of RXTE ASM data on all 6 classic Z-track sources shows the high rate and strength of flaring in the Sco-like sources suggesting that the continual release of energy heats the neutron star causing the high kT . Analysis of a Sco X-1 observation with unusually little flaring supports this. GX 17+2 appears to be transitional between the Cyg and Sco-like types. Our results do not support the suggestion that Cyg or Sco-like nature is determined by the luminosity.

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Section: A Model For the Sco X-1 Like Sourcesmentioning

confidence: 76%

Section: The Extended Adcmentioning

confidence: 99%

Section: A Monotonic Variation Of Mass Accretion Rate ?mentioning

confidence: 99%

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Spectral investigations of the nature of the Scorpius X-1 like sources

Church

Gibiec

Bałucińska‐Church

et al. 2012

A&A

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“…The sudden drops to a low flux mode appear to be of an entirely different nature than the dips in the X-ray dipper variety of LMXBs (e.g., White & Swank 1982;Smale et al 1988;Balucinska-Church et al 2011) as they do not show spectral changes in either soft X-rays (as shown in Section 6) or hard X-rays (see Tendulkar et al 2014). In general, based on the results of the X-ray spectral fits presented in Section 6, any interpretation that evokes obscuration/absorption is unlikely.…”

Section: −1mentioning

confidence: 94%

Coordinated X-Ray, Ultraviolet, Optical, and Radio Observations of the PSR J1023+0038 System in a Low-Mass X-Ray Binary State

Bogdanov

Archibald

Bassa

et al. 2015

ApJ

103

112

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The PSR J1023+0038 binary system hosts a neutron star and a low-mass, main-sequence-like star. It switches on year timescales between states as an eclipsing radio millisecond pulsar and a low-mass X-ray binary (LMXB). We present a multi-wavelength observational campaign of PSR J1023+0038 in its most recent LMXB state. Two long XMM-Newton observations reveal that the system spends ∼70% of the time in a ≈3 × 10 33 erg s −1 X-ray luminosity mode, which, as shown in Archibald et al., exhibits coherent X-ray pulsations. This emission is interspersed with frequent lower flux mode intervals with 5 10 32 ≈ × erg s −1 and sporadic flares reaching up to ≈10 34 erg s −1 , with neither mode showing significant X-ray pulsations. The switches between the three flux modes occur on timescales of order 10 s. In the UV and optical, we observe occasional intense flares coincident with those observed in X-rays. Our radio timing observations reveal no pulsations at the pulsar period during any of the three X-ray modes, presumably due to complete quenching of the radio emission mechanism by the accretion flow. Radio imaging detects highly variable, flat-spectrum continuum radiation from PSR J1023+0038, consistent with an origin in a weak jet-like outflow. Our concurrent X-ray and radio continuum data sets do not exhibit any correlated behavior. The observational evidence we present bears qualitative resemblance to the behavior predicted by some existing "propeller" and "trapped" disk accretion models although none can account for key aspects of the rich phenomenology of this system.

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“…It has been proposed that these variations are due to progressive and partial covering of an extended ADC by an extended absorber (see Bałucińska-Church et al 2011;Church et al 2005Church et al , 1998, for example). Authors such as Boirin et al (2005) and Díaz Trigo et al (2006), on the other hand, propose that an ionized absorber can explain dipping and non-dipping intervals, without the need of an extended ADC.…”

Section: Variability and Dippingmentioning

confidence: 99%

AN Fe XXIV ABSORPTION LINE IN THE PERSISTENT SPECTRUM OF THE DIPPING LOW-MASS X-RAY BINARY 1A 1744–361

Gavriil¹,

Strohmayer²,

Bhattacharyya³

2012

ApJ

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We report on Chandra X-ray Observatory (Chandra) High Energy Transmission Grating spectra of the dipping low-mass X-ray binary 1A 1744−361 during its 2008 July outburst. We find that its persistent emission is well modeled by a blackbody (kT ∼ 1.0 keV) plus power law (Γ ∼ 1.7) with an absorption edge. In the residuals of the combined spectrum, we find a significant absorption line at 6.961 ± 0.002 keV, consistent with the Fe xxvi (hydrogen-like Fe) 2-1 transition. We place an upper limit on the velocity of a redshifted flow of v < 221 km s −1 . We find an equivalent width for the line of 27 +2 −3 eV, from which we determine a column density of (7 ± 1) × 10 17 cm −2 via a curve-of-growth analysis. Using XSTAR simulations, we place a lower limit on the ionization parameter of >10 3.6 erg cm s −1 . We discuss what implications the feature has on the system and its geometry. We also present Rossi X-ray Timing Explorer data accumulated during this latest outburst and, via an updated color-color diagram, clearly show that 1A 1744−361 is an "atoll" source.

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Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission

Cited by 13 publications

References 41 publications

Spectral investigations of the nature of the Scorpius X-1 like sources

Spectral investigations of the nature of the Scorpius X-1 like sources

Coordinated X-Ray, Ultraviolet, Optical, and Radio Observations of the PSR J1023+0038 System in a Low-Mass X-Ray Binary State

AN Fe XXIV ABSORPTION LINE IN THE PERSISTENT SPECTRUM OF THE DIPPING LOW-MASS X-RAY BINARY 1A 1744–361

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