Making death more acceptable

Smith, Tony

doi:10.1136/bmj.311.7008.815a

Cited by 40 publications

(44 citation statements)

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“…X-ray transient source XTE J1550-564 was discovered with all sky monitor ASM onboard the RXTE observatory on September 7 1998 (Smith, 1998). Soon its optical and radio counterparts were identified by Orosz 1998, Campbell-Wilson et al,1998.…”

Section: Introductionmentioning

confidence: 99%

Broadband X-ray spectrum of XTE J1550-564 during the outburst of 2003

et al. 2004

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Section: Introductionmentioning

confidence: 99%

Broadband X-ray spectrum of XTE J1550-564 during the outburst of 2003

et al. 2004

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“…With the sensitivity of current X-ray missions (in particular Chandra and XMM-Newton), it is now possible to study in more detail the physical processes that take place in this accretion regime. XTE J1550À564 was discovered by the Rossi X-Ray Timing Explorer (RXTE ) All Sky Monitor (ASM ) on 1998 September 7 (Smith 1998). A brief and intense radio/X-ray flare, associated with a massive plasma ejection, was observed two weeks later ( Hannikainen et al 2001).…”

Section: Introductionmentioning

confidence: 99%

On the Origin of Black Hole X‐Ray Emission in Quiescence:ChandraObservations of XTE J1550−564 and H1743−322

Corbel

Tomsick

Kaaret

2006

ApJ

112

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We report the results of observations of the black hole binaries XTE J1550À564 and H1743À322 in their quiescent state using the Chandra X-Ray Observatory. Both sources are detected at their faintest level of X-ray emission ever observed with a 0.5-10 keV unabsorbed luminosity of 2 ; 10 32 (d /5 kpc) 2 ergs s À1 for XTE J1550À564 and 9 ; 10 31 (d /8 kpc) 2 ergs s À1 for H1743À322. These luminosities are in the upper range compared to the faintest levels observed in other black hole systems, possibly related to residual accretion for these sources with frequent outbursts. For XTE J1550À564, the Chandra observations also constrain the X-ray spectrum, as a fit with an absorbed powerlaw model yields a photon index of 2:25 AE 0:08, clearly indicating a softening of the X-ray spectrum at lower luminosities compared to the standard hard state. Similar softening at low luminosity is seen for several black hole transients with orbital periods less than 60 hr. Most of the current models of accreting black holes are able to reproduce such softening in quiescence. In contrast, we find that systems with orbital periods longer than 60 hr appear to have hard spectra in quiescence, and their behavior may be consistent with hardening in quiescence.

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“…In addition, it would also have picked up five new X-ray transients in the past year. For example, a preliminary version of this system detected the bright black hole transient XTE J1550-564 at an intensity of only 70 mCrab, very early in its rise from anonymity on 7 Sep. 1998 (Smith 1998a). The position notices are now automatically transmitted to the GCN within 5 − 60 minutes of the burst arrival time under normal operating conditions.…”

Section: New Rapid Grb Position Gcn Alertsmentioning

confidence: 99%