The X‐Ray Binary GRS 1741.9−2853 in Outburst and Quiescence

Muno, M. P.; Baganoff, Frederick K.; Arabadjis, J. S.

doi:10.1086/378851

Cited by 31 publications

(53 citation statements)

References 37 publications

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“…We do not find evidence that the fraction of magnetic CVs (polars and intermediate polars) in globular clusters is higher than the ∼ 10% estimated for the field (Liebert et al 2003). Muno et al (2004) characterize the Galactic Center sources, finding typical X-ray luminosities of 3 × 10 31 -10 33 ergs/s, and very hard X-ray spectra, with equivalent photon indices generally between 1 and -1. This is rather harder than the typical globular cluster CV or field CV, or even the magnetic CVs in either location (Heinke et al 2006).…”

Section: Globular Cluster Cvscontrasting

confidence: 69%

“…The Galactic Center sources have been inferred (Muno et al 2003(Muno et al , 2004, by their X-ray luminosity and spectral hardness, to be composed largely of the class of CVs known as intermediate polars (Patterson 1994). Intermediate polars have white dwarf accretors with relatively high magnetic fields, which force the accreting material to follow the magnetic field lines of the accretor down onto the magnetic poles.…”

Section: Introductionmentioning

confidence: 99%

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Cataclysmic Variables in Globular Clusters, the Galactic Center, and Local Space

Heinke¹,

Ruiter²,

Muno³

et al. 2008

AIP Conference Proceedings

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Abstract.We compare the X-ray spectra and luminosities, in the 2-8 keV band, of known and suspected cataclysmic variables (CVs) in different environments, assessing the nature of these source populations. These objects include nearby CVs observed with ASCA; the Galactic Center X-ray source population identified by Muno et al.; and likely CVs identified in globular clusters. Both of the latter have been suggested to be dominated by magnetic CVs. We find that the brighter objects in both categories are likely to be magnetic CVs, but that the fainter objects are likely to include a substantial contribution from normal CVs. The strangely hard spectra observed from the Galactic Center sources reflect the high and variable extinction, which is significantly greater than the canonical 6 × 10 22 cm −2 over much of the region, and the magnetic nature of many of the brightest CVs. The total numbers of faint Galactic Center sources are compatible with expectations of the numbers of CVs in this field.

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Section: Globular Cluster Cvscontrasting

confidence: 69%

Section: Introductionmentioning

confidence: 99%

Cataclysmic Variables in Globular Clusters, the Galactic Center, and Local Space

Heinke¹,

Ruiter²,

Muno³

et al. 2008

AIP Conference Proceedings

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“…Since then, the system has been detected in outburst on multiple occasions with 2-10 keV luminosities of ∼10 36 erg s −1 (e.g., Sakano et al 2002;Muno et al 2003a;Wijnands et al 2006a;Trap et al 2009). In quiescence the source displays a luminosity of ∼10 32 erg s −1 (Muno et al 2003a). The detection of thermonuclear X-ray bursts by BeppoSAX established that this system is an LMXB harboring a neutron star (Cocchi et al 1999).…”

Section: Grs 1741-2853mentioning

confidence: 99%

A four-year baselineSwiftstudy of enigmatic X-ray transients located near the Galactic center

Degenaar

Wijnands

2010

A&A

108

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We report on continued monitoring observations of the Galactic center carried out by the X-ray telescope aboard the Swift satellite in 2008 and 2009. This campaign revealed activity of the five known X-ray transients AX J1745.6-2901, CXOGC J174535.5-290124, GRS 1741-2853, XMM J174457-2850.3 and CXOGC J174538.0-290022. All these sources are known to undergo very faint X-ray outbursts with 2-10 keV peak luminosities of L X,peak ∼ 10 34−36 erg s −1 , although the two confirmed neutron star low-mass X-ray binaries AX J1745.6-2901 and GRS 1741-2853 can also become brighter (L X,peak ∼ 10 36−37 erg s −1 ). We discuss the observed longterm lightcurves and X-ray spectra of these five enigmatic transients. In 2008, AX J1745.6-2901 returned to quiescence following an unusually long accretion outburst of more than 1.5 years. GRS 1741-2853 was active in 2009 and displayed the brightest outburst ever recorded for this source, reaching up to a 2-10 keV luminosity of L X ∼ 1 × 10 37 (D/7.2 kpc) 2 erg s −1 . This system appears to undergo recurrent accretion outbursts approximately every 2 years. Furthermore, we find that the unclassified transient XMM J174457-2850.3 becomes bright only during short episodes (days) and is often found active in between quiescence (L X ∼ 10 32 erg s −1 ) and its maximum outburst luminosity of L X ∼ 10 36 erg s −1 . CXOGC J174535.5-290124 and CXOGC J174538.0-290022, as well as three other veryfaint X-ray transients that were detected by Swift monitoring observations in 2006, have very low time-averaged mass-accretion rates of Ṁ long < ∼ 2 × 10 −12 M yr −1 . Despite having obtained two years of new data in 2008 and 2009, no new X-ray transients were detected.

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“…1 the long term light curves extracted from Muno et al (2003) and Wijnands et al (2006), which represents data spanning from 2002 to 2007 (Table 1). Over the past 18 years, the X-ray luminosity of GRS 1741.9-2853 has varied regularly from 10 32 erg s −1 in quiescence, up to 10 36 erg s −1 in outburst, justifying its source classification as a faint soft X-ray transient.…”

Section: History Of Grs 17419-2853 From 1990 To 2004mentioning

confidence: 99%

Bursting behavior of the Galactic center faint X-ray transient GRS 1741.9–2853

Trap

Falanga

Goldwurm

et al. 2009

A&A

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Aims. The neutron star low-mass X-ray binary GRS 1741.9-2853 is a known type-I burster at the Galactic center. It is transient, faint, and located in a very crowded region, only 10 from the supermassive black hole Sgr A . Therefore, its bursting behavior has been poorly studied so far. In particular, its persistent emission has rarely been detected between consecutive bursts, because of lack of sensitivity or confusion. This caused GRS 1741.9-2853 to be one of the nine "burst-only sources" identified by BeppoSAX a few years ago. The physical properties of GRS 1741.9-2853 bursts are of significant interest beacause we know little about the nuclear regimes of low accretion rate bursters. For the first time we analyze several bursts along with the persistent emission of the source, using INTEGRAL, XMM-Newton, and Swift observations. Methods. We investigate the source flux variability and bursting behavior during its 2005 and 2007 long outbursts. These events were monitored almost entirely by INTEGRAL, both in the soft (3-20 keV) and hard (20-100 keV) X-ray bands, and also partly by XMM-Newton and Swift (2-10 keV) in 2007.Results. In its last activity periods, 2005 and 2007, the persistent luminosity of GRS 1741.9-2853 varied between ∼1.7 and 10.5 × 10 36 erg s −1 , i.e., 0.9−5.3% of the Eddington luminosity. The shape of the spectrum as described by an absorbed power-law remained with a photon index Γ ≈ 2 and a column density N H ≈ 12 × 10 22 cm −2 throughout the outbursts. We discovered 11 type-I bursts with INTEGRAL, and inspected four additional bursts: two recorded by XMM-Newton and two by Swift. From the brightest burst, we derive an upper limit to the source distance of ∼7 kpc. The observed bursts characteristics and source accretion rate infer pure helium explosions igniting at column depths y ign ≈ 0.8 − 4.8 × 10 8 g cm −2 , for typical energy releases of ∼1.2 − 7.4 × 10 39 erg.

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The X‐Ray Binary GRS 1741.9−2853 in Outburst and Quiescence

Cited by 31 publications

References 37 publications

Cataclysmic Variables in Globular Clusters, the Galactic Center, and Local Space

Cataclysmic Variables in Globular Clusters, the Galactic Center, and Local Space

A four-year baselineSwiftstudy of enigmatic X-ray transients located near the Galactic center

Bursting behavior of the Galactic center faint X-ray transient GRS 1741.9–2853

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