Modeling the X-ray contribution of XRB jets

Markoff, Sera; Nowak, Michael A.; Corbel, S.; Fender, Rob; Falcke, H.

doi:10.1016/s1387-6473(03)00078-2

Cited by 23 publications

(19 citation statements)

References 11 publications

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“…In our simulations, the flow originates in the high entropy atmosphere called a corona. Optically thin coronae are an integral part in models of the X-ray features of AGNs (e.g., Mushotzky et al 1993) and μ-Quasars (e.g., Nowak et al 2002;Markoff et al 2003).…”

Section: Accretion Disk Coronaementioning

confidence: 99%

Acceleration and Collimation of Relativistic Magnetohydrodynamic Disk Winds

Porth

Fendt

2010

ApJ

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We perform axisymmetric relativistic magnetohydrodynamic simulations to investigate the acceleration and collimation of jets and outflows from disks around compact objects. Newtonian gravity is added to the relativistic treatment in order to establish the physical boundary condition of an underlying accretion disk in centrifugal and pressure equilibrium. The fiducial disk surface (respectively a slow disk wind) is prescribed as boundary condition for the outflow. We apply this technique for the first time in the context of relativistic jets. The strength of this approach is that it allows us to run a parameter study in order to investigate how the accretion disk conditions govern the outflow formation. Substantial effort has been made to implement a current-free, numerical outflow boundary condition in order to avoid artificial collimation present in the standard outflow conditions. Our simulations using the PLUTO code run for 500 inner disk rotations and on a physical grid size of 100 × 200 inner disk radii. The simulations evolve from an initial state in hydrostatic equilibrium and an initially force-free magnetic field configuration. Two options for the initial field geometries are applied-an hourglass-shaped potential magnetic field and a split monopole field. Most of our parameter runs evolve into a steady state solution which can be further analyzed concerning the physical mechanism at work. In general, we obtain collimated beams of mildly relativistic speed with Lorentz factors up to 6 and mass-weighted half-opening angles of 3-7 deg. The split-monopole initial setup usually results in less collimated outflows. The light surface of the outflow magnetosphere tends to align vertically-implying three relativistically distinct regimes in the flow-an inner subrelativistic domain close to the jet axis, a (rather narrow) relativistic jet and a surrounding subrelativistic outflow launched from the outer disk surface-similar to the spine-sheath structure currently discussed for asymptotic jet propagation and stability. The outer subrelativistic disk-wind is a promising candidate for the X-ray absorption winds that are observed in many radio-quiet active galactic nuclei. The hot winds under investigation acquire only low Lorentz factors due to the rather high plasma-β we have applied in order to provide an initial force-balance in the disk corona. When we increase the outflow Poynting flux by injecting an additional disk toroidal field into the outflow, the jet velocities achieved are higher. These flows gain super-magnetosonic speed and remain Poynting flux dominated.

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Section: Accretion Disk Coronaementioning

confidence: 99%

Acceleration and Collimation of Relativistic Magnetohydrodynamic Disk Winds

Porth

Fendt

2010

ApJ

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“…On the contrary, we adopt a thermal Comptonization field at hard X-rays, possibly originating in a corona around the black hole (e.g. Zdziarski et al 2003), as suggested by the observation of a Compton reflection feature and an iron Kα line in some sources (for an alternative interpretation, see Markoff et al 2003b). In this sense, our treatment is more similar to that of Romero et al (2002).…”

Section: Commentsmentioning

confidence: 99%

High-mass microquasars and low-latitude gamma-ray sources

Bosch‐Ramon¹,

Romero

Paredes³

2004

A&A

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Abstract. Population studies of unidentified EGRET sources suggest that there exist at least three different populations of galactic gamma-ray sources. One of these populations is formed by young objects distributed along the galactic plane with a strong concentration toward the inner spiral arms of the Galaxy. Variability, spectral and correlation analysis indicate that this population is not homogeneous. In particular, there is a subgroup of sources that display clear variability in their gammaray fluxes on timescales from days to months. Following the proposal by Kaufman Bernadó et al. (2002), we suggest that this group of sources might be high-mass microquasars, i.e. accreting black holes or neutron stars with relativistic jets and early-type stellar companions. We present detailed inhomogeneous models for the gamma-ray emission of these systems that include both external and synchrotron self-Compton interactions. We have included effects of interactions between the jet and all external photon fields to which it is exposed: companion star, accretion disk, and hot corona. We make broadband calculations to predict the spectral energy distribution of the emission produced in the inner jet of these objects up to GeV energies. The results and predictions can be tested by present and future gamma-ray instruments like INTEGRAL, AGILE, and GLAST.

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“…This is unlike the LS, where the origin of X-rays is still a matter of debate (e.g., Markoff et al 2003;Zdziarski et al 2004).…”

Section: Introductionmentioning

confidence: 99%

A Panchromatic View of PKS 0558–504: An Ideal Laboratory to Study the Disk-Jet Link

Gliozzi

Papadakis

Grupe

et al. 2010

ApJ

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PKS 0558−504 is the brightest radio-loud Narrow-line Seyfert 1 galaxy (NLS1) at X-ray energies. Here we present results from the radio, optical, UV, and X-ray bands obtained with Swift, XMM-Newton, and the Australia Telescope Compact Array (ATCA) during a ten-day monitoring campaign in 2008 September. The simultaneous coverage at several wavelengths makes it possible to investigate in detail the broadband spectral energy distribution (SED) and the energetics of this source. The main results can be summarized as follows. The ATCA reveals the presence of an extended radio emission in PKS 0558−504 with two lobe-like structures ∼7 from the bright central source. The extended radio structure and the low value of the radio loudness similar to radio-quiet Seyfert galaxies coupled with constraints from higher energy bands argue against a jet-dominated emission in PKS 0558−504. The study of the SED, which is dominated by a nearly constant optical-UV emission, supports the conclusion that PKS 0558−504 is accreting at a super-Eddington rate. This conclusion was reached by assuming M BH = 2.5 × 10 8 M , which was obtained with a new scaling method based on X-ray spectral variability results. A comparison between the accretion luminosity and the kinetic power associated with the jet suggests that in this source, the accretion power dominates in agreement with the results obtained from radiation-magnetohydrodynamic simulations of Galactic black holes (GBHs) accreting at the Eddington rate. The combined findings from this panchromatic investigation strongly suggest that PKS 0558−504 is a largescale analog of GBHs in their highly accreting intermediate state. More importantly, PKS 0558−504 may also be the prototype of the parent population of the very radio-loud NLS1s recently detected at γ -ray energies.

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Modeling the X-ray contribution of XRB jets

Cited by 23 publications

References 11 publications

Acceleration and Collimation of Relativistic Magnetohydrodynamic Disk Winds

Acceleration and Collimation of Relativistic Magnetohydrodynamic Disk Winds

High-mass microquasars and low-latitude gamma-ray sources

A Panchromatic View of PKS 0558–504: An Ideal Laboratory to Study the Disk-Jet Link

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