Article

# Large-Scale, Decelerating, Relativistic X-ray Jets from the Microquasar XTE J1550-654

[more]
Utrecht University, Utrecht, Utrecht, Netherlands
(Impact Factor: 31.48). 11/2002; 298(5591):196-9. DOI: 10.1126/science.1075857
Source: PubMed

ABSTRACT We have detected, at x-ray and radio wavelengths, large-scale moving jets from the microquasar XTE J1550-564. Plasma ejected from near the black hole traveled at relativistic velocities for at least 4 years. We present direct evidence for gradual deceleration in a relativistic jet. The broadband spectrum of the jets is consistent with synchrotron emission from high-energy (up to 10 tera-electron volts) particles that were accelerated in the shock waves formed within the relativistic ejecta or by the interaction of the jets with the interstellar medium. XTE J1550-564 offers a rare opportunity to study the dynamical evolution of relativistic jets on time scales inaccessible for active galactic nuclei jets, with implications for our understanding of relativistic jets from Galactic x-ray binaries and active galactic nuclei.

### Full-text

Available from: Jerome A. Orosz, Jun 19, 2015
0 Followers
·
107 Views
• Source
##### Article: On the radio properties of the intermediate-mass black hole candidate ESO 243-49 HLX-1
[Hide abstract]
ABSTRACT: We present follow-up radio observations of ESO 243-49 HLX-1 from 2012 using the Australia Telescope Compact Array (ATCA) and the Karl G. Jansky Very Large Array (VLA). We report the detection of radio emission at the location of HLX-1 during its hard X-ray state using the ATCA. Assuming that the `Fundamental Plane' of accreting black holes is applicable, we provide an independent estimate of the black hole mass of $M_{\rm{BH}}\leq2.8^{+7.5}_{-2.1} \times 10^{6}$ M$_{\odot}$ at 90% confidence. However, we argue that the detected radio emission is likely to be Doppler-boosted and our mass estimate is an upper limit. We discuss other possible origins of the radio emission such as being due to a radio nebula, star formation, or later interaction of the flares with the large-scale environment. None of these were found adequate. The VLA observations were carried out during the X-ray outburst. However, no new radio flare was detected, possibly due to a sparse time sampling. The deepest, combined VLA data suggests a variable radio source and we briefly discuss the properties of the previously detected flares and compare them with microquasars and active galactic nuclei.
Monthly Notices of the Royal Astronomical Society 11/2014; 446(4). DOI:10.1093/mnras/stu2363 · 5.23 Impact Factor
• Source
##### Article: Black hole-like hysteresis and accretion states in neutron star low mass X-ray binaries
[Hide abstract]
ABSTRACT: We have systematically studied a large sample of the neutron star low mass X-ray binaries (LMXBs) monitored by the Rossi X-ray Timing Explorer (50 sources; 10000+ observations). We find that the hysteresis patterns between Compton dominated and thermal dominated states, typically observed in black hole LMXBs, are also common in neutron star systems. These patterns, which also sample intermediate states, are found when looking at the evolution of both X-ray colour and fast variability of ten systems accreting below ~ 30 % of the Eddington Luminosity. We show that hysteresis does not require large changes in luminosity and it is the natural form that state transitions take at these luminosities. At higher accretion rates neutron stars do not show hysteresis, and they remain in a thermal dominated, low variability state, characterized by flaring behaviour and fast colour changes. Only at luminosities close to the Eddington Luminosity, are high variability levels seen again, in correspondence to an increase in the fractional contribution of the Comptonization component. We compare this behaviour with that observed in LMXBs harbouring black holes, showing that the spectral, timing and multi-wavelength properties of a given source can be determined by its location in the fast variability-luminosity diagram, which, therefore, provides a common framework for neutron star and black hole accretion states.
Monthly Notices of the Royal Astronomical Society 07/2014; 443(4). DOI:10.1093/mnras/stu1334 · 5.23 Impact Factor
• Source
##### Article: Technical Report: Synchrotron Radiation from Outer Space and the Chandra X-ray Observatory
[Hide abstract]
ABSTRACT: The Chandra X-ray Observatory began its journey into space on July 23, 1999, using the Space Shuttle Columbia for the initial ascent. An upper stage and integral propulsion then placed the observatory into an elliptical orbit with an initial apogee of 140,000 km (1/3 of the distance to the moon) and an initial perigee 10,000 km (about two earth radii). In this orbit, the satellite (Figure 1) is above the radiation belts for more than 75% of the 63.5 hour orbital period, allowing for uninterrupted observations up to more than two days.
Synchrotron Radiation News 10/2006; 19(5):29-35. DOI:10.1080/08940880600978747