130 research outputs found
Soft-excess in ULX spectra: the chilled-disk scenario
Soft X-ray spectra of ULXs show small deviations from a power-law model, that
can be attributed to reprocessing in a fast, ionized outflow, or to thermal
emission from a cool disk. If it is thermal emission, the cool peak temperature
can be explained by an inner disk that radiates only a small fraction of the
gravitational power, transferring the rest to an upscattering medium which is
then responsible for the dominant power-law component. This scenario does not
require intermediate-mass black holes: we use a phenomenological model to show
that the observed X-ray luminosities and spectra of ULXs are consistent with
typical masses ~ 50-100 Msun.Comment: To appear in the proceedings of "The Multicoloured Landscape of
Compact Objects and their Explosive Progenitors: Theory vs Observations",
Cefalu', Sicily, June 11-24, 2006 (AIP
On the origin of radio core emission in radio-quiet quasars
We present a model for the radio emission from radio-quiet quasar nuclei. We
show that a thermal origin for the high brightness temperature, flat spectrum
point sources (known as radio ``cores'') is possible provided the emitting
region is hot and optically-thin. We hence demonstrate that optically-thin
bremsstrahlung from a slow, dense disk wind can make a significant contribution
to the observed levels of radio core emission. This is a much more satisfactory
explanation, particularly for sources where there is no evidence of a jet, than
a sequence of self-absorbed synchrotron components which collectively conspire
to give a flat spectrum. Furthermore, such core phenomena are already observed
directly via milli-arcsecond radio imaging of the Galactic microquasar SS433
and the active galaxy NGC1068. We contend that radio-emitting disk winds must
be operating at some level in radio-loud quasars and radio galaxies as well
(although in these cases, observations of the radio cores are frequently
contaminated/dominated by synchrotron emission from jet knots). This
interpretation of radio core emission mandates mass accretion rates that are
substantially higher than Eddington. Moreover, acknowledgment of this mass-loss
mechanism as an AGN feedback process has important implications for the input
of energy and hot gas into the inter-galactic medium (IGM) since it is
considerably less directional than that from jets.Comment: to appear in ApJ Letters (4 pages
New Global 3D MHD Simulations of Black Hole Disk Accretion and Outflows
It is widely accepted that quasars and other active galactic nuclei (AGN) are
powered by accretion of matter onto a central supermassive black hole. While
numerical simulations have demonstrated the importance of magnetic fields in
generating the turbulence believed necessary for accretion, so far they have
not produced the high mass accretion rates required to explain the most
powerful sources. We describe new global 3D simulations we are developing to
assess the importance of radiation and non-ideal MHD in generating magnetized
outflows that can enhance the overall rates of angular momentum transport and
mass accretion.Comment: 2 pages, including 1 colour figure. To appear in proceedings of IAU
Symposium 259: "Cosmic Magnetic Fields: From Planets, To Stars and Galaxies",
Tenerife, Nov 200
X-ray polarization from accreting white dwarfs and associated systems
We present our results of Monte-Carlo simulations of polarized Compton X-rays
from magnetic cataclysmic variables, with realistic density, temperature and
velocity structures in the accretion flow. Our study has shown that the X-ray
linear polarization may reach about 8% for systems with high accretion rates
viewed at a high viewing inclination angle. This value is roughly twice the
maximum value obtained by previous studies which assumed a cold, static
emission region with a uniform density. We also investigate the X-ray
polarization properties of ultra-compact double-degenerate binaries for the
unipolar-inductor and direct-impact accretor models. Our study has shown
negligible X-ray polarization for the unipolar-induction model. However, the
direct-impact accretor model may give X-ray polarization levels similar to that
predicted for the magnetic cataclysmic variables.Comment: to appear in "X-ray Polarimetry: A New Window in Astrophysics",
edited by R. Bellazzini, E. Costa, G. Matt and G. Tagliaferr
Enhanced MHD transport in astrophysical accretion flows: turbulence, winds and jets
Astrophysical accretion is arguably the most prevalent physical process in
the Universe; it occurs during the birth and death of individual stars and
plays a pivotal role in the evolution of entire galaxies. Accretion onto a
black hole, in particular, is also the most efficient mechanism known in
nature, converting up to 40% of accreting rest mass energy into spectacular
forms such as high-energy (X-ray and gamma-ray) emission and relativistic jets.
Whilst magnetic fields are thought to be ultimately responsible for these
phenomena, our understanding of the microphysics of MHD turbulence in accretion
flows as well as large-scale MHD outflows remains far from complete. We present
a new theoretical model for astrophysical disk accretion which considers
enhanced vertical transport of momentum and energy by MHD winds and jets, as
well as transport resulting from MHD turbulence. We also describe new global,
3D simulations that we are currently developing to investigate the extent to
which non-ideal MHD effects may explain how small-scale, turbulent fields
(generated by the magnetorotational instability -- MRI) might evolve into
large-scale, ordered fields that produce a magnetized corona and/or jets where
the highest energy phenomena necessarily originate.Comment: 8 pages, 2 figures. Minor revision, published version: Proc 14th
International Congress on Plasma Physics, Fukuoka, Japan, Sep 200
Black hole masses and accretion states in ULXs
We summarize indirect empirical arguments used for estimating black hole (BH)
masses in ultraluminous X-ray sources (ULXs). The interpretation of the X-ray
data is still too model-dependent to provide tight constraints, but masses <~
100 Msun seem the most likely. It is getting clearer that ULXs do not show the
same evolutionary sequence between canonical spectral states as stellar-mass
BHs, nor the same timescale for state transitions. Most ULX spectra are
consistent either with a power-law-dominated state (apparently identical to the
canonical low/hard state), or with a very high state (or slim-disk state).
Despite often showing luminosity variability, there is little evidence of ULXs
settling into a canonical high/soft state, dominated by a standard disk
(disk-blackbody spectrum). It is possible that the mass accretion rate (but not
necessarily the luminosity) is always higher than Eddington; but there may be
additional physical differences between stellar-mass BHs and ULXs, which
disfavour transitions to the standard-disk, radio-quiet state in the latter
class. We speculate that the hard state in ULXs is associated with jet or
magnetic processes rather than an ADAF, can persist up to accretion rates ~
Eddington, and can lead directly to the very high state.Comment: 8 pages; to appear in the proceedings of the conference
"Observational Evidence of Black Holes", Kolkata, February 200
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