The discovery of hard X-ray emission in the persistent flux of the Rapid Burster

Falanga, M.; Farinelli, R.; Goldoni, P.; Frontera, F.; Goldwurm, A.; Stella, L.

doi:10.1051/0004-6361:20041243

Cited by 10 publications

(10 citation statements)

References 18 publications

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“…Due to the fact that INTEGRAL is able to image the sky at high angular resolution (12 ′ for ISGRI and 3 ′ for JEM-X), we were able to clearly distinguish and isolate the high-energy fluxes from the two sources. This allowed us to study the Xray emission of 4U 1728-34 during its entire observation without contamination (see also for the Rapid Burster Falanga et al, 2004). In Fig.…”

Section: Resultsmentioning

confidence: 99%

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

Falanga

Götz²,

Goldoni

et al. 2006

A&A

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We present for the first time a study of the 3-200 keV broad band spectra of the bursting atoll source 4U 1728-34 (GX 354-0) along its hardness intensity diagram. The analysis was done using the INTEGRAL public and Galactic Center deep exposure data ranging from February 2003 to October 2004. The spectra are well described by a thermal Comptonization model with an electron temperature from 35 keV to 3 keV and Thomson optical depth, τ T , from 0.5 to 5 in a slab geometry. The source undergoes a transition from an intermediate/hard to a soft state where the source luminosity increases from 2 to 12% of Eddington. We have also detected 36 type I X-ray bursts two of which show photospheric radius expansion. The energetic bursts with photospheric radius expansion occurred at an inferred low mass accretion rate per unit area ofṁ ∼ 1.7 × 10 3 g cm −2 s −1 , while the others at a higher one between 2.4 × 10 3 −9.4 × 10 3 g m −2 s −1 . For 4U 1728-34 the bursts' total fluence, and the bursts' peak flux are anti-correlated with the mass accretion rate. The type I X-ray bursts involve pure helium burning either during the hard state, or during the soft state of the source.

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Section: Resultsmentioning

confidence: 99%

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

Falanga

Götz²,

Goldoni

et al. 2006

A&A

Self Cite

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“…All active PCUs were employed, and a correction was applied for deadtime (although it is always small for the RB). Low-energy absorption by the interstellar medium was taken into account using the model of Morrison & McCammon (1983), with an equivalent hydrogen column density of NH = 1.6×10 22 cm −2 (Frogel, Kuchinski & Tiede 1995;Masetti et al 2000;Falanga et al 2004). Following the RXTE Cookbook prescription 1 , the analysis was limited to the 3 − 30 keV range, and a systematic error of 0.5% was added to the results.…”

Section: Burst Energeticsmentioning

confidence: 99%

Indications for a slow rotator in the Rapid Burster from its thermonuclear bursting behaviour

Bagnoli¹,

Zand²,

Watts³

2013

Monthly Notices of the Royal Astronomical Society

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We perform time-resolved spectroscopy of all the type I bursts from the Rapid Burster (MXB 1730−335) detected with the Rossi X-ray Timing Explorer. Type I bursts are detected at high accretion rates, up to 45% of the Eddington luminosity. We find evidence that bursts lacking the canonical cooling in their time-resolved spectra are, none the less, thermonuclear in nature. The type I bursting rate keeps increasing with the persistent luminosity, well above the threshold at which it is known to abruptly drop in other bursting low-mass X-ray binaries. The only other known source in which the bursting rate keeps increasing over such a large range of mass accretion rates is the 11 Hz pulsar IGR J17480−2446. This may indicate a similarly slow spin for the neutron star in the Rapid Burster.

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“…References are: 1 Liu, van Paradijs & van den Heuvel (2001), 2 Schultz (1999), 3 Christian & Swank (1997), 4 Nelemans et al (2004), 5 Fender & Hendry (2000), 6 Jonker et al (2001), 7 Juett & Chakrabarty (2003), 8 Díaz Trigo et al (2006), 9 Smale, Church & Bałucińska‐Church (2002), 10 Courvoisier et al (1986), 11 in't Zand et al (2003a), 12 Schultz (2002), 13 Wang & Chakrabarty (2004), 14 Farinelli et al (2003), 15 Piro & Bildsten (2005), 16 Gierliński & Done (2002), 17 Garcia et al (2001), 18 Owens, Oosterbroek & Parmar (1997), 19 Chakrabarty (1997), 20 Angelini et al (1995), 21 Wijnands (2001), 22 Oosterbroek et al (2001), 23 Wijnands, Strohmayer & Franco (2001), 24 Oosterbroek et al (2001), 25 (Di Salvo et al 2005), 26 Migliari et al (2003a), 27 Wilson et al (2003), 28 Molkov, Grebenev & Lutovinov (2000), 29 Emelyanov et al (2002), 30 Yao & Wang (2005), 31 Di Salvo et al (2000), 32 Shaposhnikov, Titarchuk & Haberl (2003), 33 Migliari et al (2003a), 34 Falanga et al (2004), 35 Cornelisse et al (2000), 36 Jonker et al (2000), 37 Bałucińska‐Church et al (2004), 38 Barret, Olive & Oosterbroek (2003), 39 Shaposhnikov & Titarchuk (2004), 40 Sidoli et al (2005), 41 Homer et al (1996), 42 Chevalier et al (1999), 43 Bloser et al (2000), 44 Chevalier et al (1999), 45 Maccarone & Coppi (2003a), 46 Galloway et al (2001), 47 Barret et al (2000), 48 Galloway at al. (2004), 49 Thompson et al (2005), 50 Mignani et al (2002), 51 Burderi et al (2002), 52 Pavlinsky et al (2001), 53 Cackett et al (2006), 54 Molkov et al (2005), 55 Wijnands & van der Klis (1999a), 56 Jonker et al (2004), 57 Wijnands & van der Klis (1999b), 58 Revnivtsev, Borozdin & Emelyanov (1999), 59 Tomsick et al (2004), 60 Galloway et al (2005), 61 Poutanen (2006), 62 Jonker et al (2005a), 63 …”

Section: Sample Selection and Data Analysismentioning

confidence: 99%

Analysing the atolls: X-ray spectral transitions of accreting neutron stars

Gladstone

Done

Gierliński

2007

Monthly Notices of the Royal Astronomical Society

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We systematically analyse all the available X-ray spectra of disc accreting neutron stars (atolls and millisecond pulsars) from the RXTE data base. We show that while all these have similar spectral evolution as a function of mass accretion rate, there are also subtle differences. There are two different types of hard/soft transition, those where the spectrum softens at all energies, leading to a diagonal track on a colour-colour diagram, and those where only the higher energy spectrum softens, giving a vertical track. The luminosity at which the transition occurs is correlated with this spectral behaviour, with the vertical transition at L/L Edd ∼ 0.02 while the diagonal one is at ∼0.1. Superimposed on this is the well-known hysteresis effect, but we show that classic, large-scale hysteresis occurs only in the outbursting sources, indicating that its origin is in the dramatic rate of change of mass accretion rate during the disc instability. We show that the long-term mass accretion rate correlates with the transition behaviour, and speculate that this is due to the magnetic field being able to emerge from the neutron star surface for low average mass accretion rates. While this is not strong enough to collimate the flow except in the millisecond pulsars, its presence may affect the inner accretion flow by changing the properties of the jet.

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The discovery of hard X-ray emission in the persistent flux of the Rapid Burster

Cited by 10 publications

References 18 publications

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

The X-ray spectrum of the bursting atoll source 4U 1728-34 observed with INTEGRAL

Indications for a slow rotator in the Rapid Burster from its thermonuclear bursting behaviour

Analysing the atolls: X-ray spectral transitions of accreting neutron stars

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