514 research outputs found
New Analytical Formula for Supercritical Accretion Flows
We examine a new family of global analytic solutions for optically thick
accretion disks, which includes the supercritical accretion regime. We found
that the ratio of the advection cooling rate, , to the viscous
heating rate, , i.e., , can be
represented by an analytical form dependent on the radius and the mass
accretion rate. The new analytic solutions can be characterized by the
photon-trapping radius, \rtrap, inside which the accretion time is less than
the photon diffusion time in the vertical direction; the nature of the
solutions changes significantly as this radius is crossed. Inside the trapping
radius,
approaches , which corresponds to the advection-dominated
limit (), whereas outside the trapping radius, the radial dependence
of changes to , which corresponds to the
radiative-cooling-dominated limit. The analytical formula for derived here
smoothly connects these two regimes. The set of new analytic solutions
reproduces well the global disk structure obtained by numerical integration
over a wide range of mass accretion rates, including the supercritical
accretion regime. In particular, the effective temperature profiles for our new
solutions are in good agreement with those obtained from numerical solutions.
Therefore, the new solutions will provide a useful tool not only for evaluating
the observational properties of accretion flows, but also for investigating the
mass evolution of black holes in the presence of supercritical accretion flows.Comment: 14 pages, 7 figures, accepted for publication in the Astrophysical
Journa
Does the Slim-Disk Model Correctly Consider Photon-Trapping Effects?
We investigate the photon-trapping effects in the super-critical black hole
accretion flows by solving radiation transfer as well as the energy equations
of radiation and gas. It is found that the slim-disk model generally
overestimates the luminosity of the disk at around the Eddington luminosity
(L_E) and is not accurate in describing the effective temperature profile,
since it neglects time delay between energy generation at deeper inside the
disk and energy release at the surface. Especially, the photon-trapping effects
are appreciable even below L ~ L_E, while they appear above ~ 3L_E according to
the slim disk. Through the photon-trapping effects, the luminosity is reduced
and the effective temperature profile becomes flatter than r^{-3/4} as in the
standard disk. In the case that the viscous heating is effective only around
the equatorial plane, the luminosity is kept around the Eddington luminosity
even at very large mass accretion rate, Mdot>>L_E/c^2. The effective
temperature profile is almost flat, and the maximum temperature decreases in
accordance with rise in the mass accretion rate. Thus, the most luminous radius
shifts to the outer region when Mdot/(L_E/c^2) >> 10^2. In the case that the
energy is dissipated equally at any heights, the resultant luminosity is
somewhat larger than in the former case, but the energy-conversion efficiency
still decreases with increase of the mass accretion rate, as well. The most
luminous radius stays around the inner edge of the disk in the latter case.
Hence, the effective temperature profile is sensitive to the vertical
distribution of energy production rates, so is the spectral shape. Future
observations of high L/L_E objects will be able to test our model.Comment: 10 pages, 7 figures, accepted for publication in Ap
Coevolution of Supermassive Black Holes and Circumnuclear Disks
We propose a new evolutionary model of a supermassive black hole (SMBH) and a
circumnuclear disk (CND), taking into account the mass-supply from a host
galaxy and the physical states of CND. In the model, two distinct accretion
modes depending on gravitational stability of the CND play a key role on
accreting gas to a SMBH. (i) If the CMD is gravitationally unstable, energy
feedback from supernovae (SNe) supports a geometrically thick, turbulent gas
disk. The accretion in this mode is dominated by turbulent viscosity, and it is
significantly larger than that in the mode (ii), i.e., the CMD is supported by
gas pressure. Once the gas supply from the host is stopped, the high accretion
phase () changes to the low one (mode
(ii), ), but there is a delay with yr. Through this evolution, the gas-rich CND turns into the gas poor
stellar disk. We found that not all the gas supplied from the host galaxy
accrete onto the SMBH even in the high accretion phase (mode (i)), because the
part of gas is used to form stars. As a result, the final SMBH mass () is not proportional to the total gas mass supplied from the host
galaxy (); decreases with .This would indicate that it is difficult to form a SMBH with observed at high- QSOs. The evolution of the SMBH and CND would
be related to the evolutionary tracks of different type of AGNs.Comment: 11 pages, 11 figures, accepted for publication in Ap
Evidence of a Warm Absorber that Varies with QPO Phase in the AGN RE J1034+396
A recent observation of the nearby (z=0.042) narrow-line Seyfert 1 galaxy RE
J1034+396 on 2007 May 31 showed strong quasi-periodic oscillations (QPOs) in
the 0.3-10 keV X-ray flux. We present phase-resolved spectroscopy of this
observation, using data obtained by the EPIC PN detector onboard XMM. The "low"
phase spectrum, associated with the troughs in the light curve, shows (at >4
sigma confidence level) an absorption edge at 0.86+/-0.05 keV with an
absorption depth of 0.3+/-0.1. Ionized oxygen edges are hallmarks of X-ray warm
absorbers in Seyfert active galactic nuclei (AGN); the observed edge is
consistent with H-like O VIII and implies a column density of
N_{OVIII}~3x10^{18} cm^{-2}. The edge is not seen in the "high" phase spectrum
associated with the crests in the light curve, suggesting the presence of a
warm absorber in the immediate vicinity of the supermassive black hole which
periodically obscures the continuum emission. If the QPO arises due to
Keplerian orbital motion around the central black hole, the periodic appearance
of the O VIII edge would imply a radius of ~9.4(M/[4x10^6 Msun])^{-2/3}(P/[1
hr])^{2/3} r_g for the size of the warm absorber.Comment: Accepted for publication in ApJ (tentatively scheduled for the July
2010 v717 issue). 5 figures and 19 pages (in aastex preprint format
Super-critical Accretion Flows around Black Holes: Two-dimensional, Radiation-pressure-dominated Disks with Photon-trapping
The quasi-steady structure of super-critical accretion flows around a black
hole is studied based on the two-dimensional radiation-hydrodynamical (2D-RHD)
simulations. The super-critical flow is composed of two parts: the disk region
and the outflow regions above and below the disk. Within the disk region the
circular motion as well as the patchy density structure are observed, which is
caused by Kelvin-Helmholtz instability and probably by convection. The
mass-accretion rate decreases inward, roughly in proportion to the radius, and
the remaining part of the disk material leaves the disk to form outflow because
of strong radiation pressure force. We confirm that photon trapping plays an
important role within the disk. Thus, matter can fall onto the black hole at a
rate exceeding the Eddington rate. The emission is highly anisotropic and
moderately collimated so that the apparent luminosity can exceed the Eddington
luminosity by a factor of a few in the face-on view. The mass-accretion rate
onto the black hole increases with increase of the absorption opacity
(metalicity) of the accreting matter. This implies that the black hole tends to
grow up faster in the metal rich regions as in starburst galaxies or
star-forming regions.Comment: 16 pages, 12 figures, accepted for publication in ApJ (Volume 628,
July 20, 2005 issue
The X-ray Luminosity Function of "The Antennae" Galaxies (NGC4038/39) and the Nature of Ultra-Luminous X-ray Sources
We derive the X-ray luminosity function (XLF) of the X-ray source population
detected in the Chandra observation of NGC4038/39 (the Antennae).
We explicitly include photon counting and spectral parameter uncertainties in
our calculations. The cumulative XLF is well represented by a flat power law
(), similar to those describing the XLFs of other star-forming
systems (e.g. M82, the disk of M81), but different from those of early type
galaxies. This result associates the X-ray source population in the Antennae
with young High Mass X-ray Binaries. In comparison with less actively
star-forming galaxies, the XLF of the Antennae has a highly significant excess
of sources with luminosities above 10^{39} erg\s (Ultra Luminous Sources;
ULXs). We discuss the nature of these sources, based on the XLF and on their
general spectral properties, as well as their optical counterparts discussed in
Paper III. We conclude that the majority of the ULXs cannot be intermediate
mass black-holes (M > 10-1000 \msun) binaries, unless they are linked to the
remnants of massive Population III stars (the Madau & Rees model). Instead,
their spatial and multiwavelength properties can be well explained by beamed
emission as a consequence of supercritical accretion.
Binaries with a neutron star or moderate mass black-hole (up to 20\msun), and
B2 to A type star companions would be consistent with our data. In the beaming
scenario, the XLF should exibit caracteristic breaks that will be visible in
future deeper observations of the Antennae.Comment: 15 pages, submitted to Ap
Why Is Supercritical Disk Accretion Feasible?
Although the occurrence of steady supercritical disk accretion onto a black
hole has been speculated about since the 1970s, it has not been accurately
verified so far. For the first time, we previously demonstrated it through
two-dimensional, long-term radiation-hydrodynamic simulations. To clarify why
this accretion is possible, we quantitatively investigate the dynamics of a
simulated supercritical accretion flow with a mass accretion rate of ~10^2
L_E/c^2 (with L_E and c being, respectively, the Eddington luminosity and the
speed of light). We confirm two important mechanisms underlying supercritical
disk accretion flow, as previously claimed, one of which is the radiation
anisotropy arising from the anisotropic density distribution of very optically
thick material. We qualitatively show that despite a very large radiation
energy density, E_0>10^2L_E/(4 pi r^2 c) (with r being the distance from the
black hole), the radiative flux F_0 cE_0/tau could be small due to a large
optical depth, typically tau 10^3, in the disk. Another mechanism is photon
trapping, quantified by vE_0, where v is the flow velocity. With a large |v|
and E_0, this term significantly reduces the radiative flux and even makes it
negative (inward) at r<70r_S, where r_S is the Schwarzschild radius. Due to the
combination of these effects, the radiative force in the direction along the
disk plane is largely attenuated so that the gravitational force barely exceeds
the sum of the radiative force and the centrifugal force. As a result, matter
can slowly fall onto the central black hole mainly along the disk plane with
velocity much less than the free-fall velocity, even though the disk luminosity
exceeds the Eddington luminosity. Along the disk rotation axis, in contrast,
the strong radiative force drives strong gas outflows.Comment: 8 pages, 7 figures, accepted for publication in Ap
Observations of Rapid Disk-Jet Interaction in the Microquasar GRS 1915+105
We present evidence that ~ 30 minute episodes of jet formation in the
Galactic microquasar GRS 1915+105 may sometimes entirely be a superposition of
smaller, faster phenomena. We base this conclusion on simultaneous X-ray and
infrared observations in July 2002, using the Rossi X-ray Timing Explorer and
the Palomar 5 meter telescope. On two nights, we observed quasi-periodic
infrared flares from GRS 1915+105, each accompanied by a set of fast
oscillations in the X-ray light curve (indicating an interaction between the
jet and accretion disk). In contrast to similar observations in 1997, we find
that the duration of each X-ray cycle matches the duration of its accompanying
infrared flare, and we observed one instance in which an isolated X-ray
oscillation occurred at the same time as a faint infrared "subflare" (of
duration ~ 150 seconds) superimposed on one of the main flares. From these
data, we are able to conclude that each X-ray oscillation had an associated
faint infrared flare and that these flares blend together to form, and entirely
comprise, the ~ 30 minute events we observed. Part of the infrared emission in
1997 also appears to be due to superimposed small flares, but it was
overshadowed by infrared-bright ejections associated with the appearance of a
sharp "trigger" spike in each X-ray cycle that were not present in 2002. We
also study the evolution of the X-ray spectrum and find significant differences
in the high energy power law component, which was strongly variable in 1997 but
not in 2002. Taken together, these observations reveal the diversity of ways in
which the accretion disk and jet in black hole systems are capable of
interacting and solidify the importance of the trigger spike for large
ejections to occur on ~ 30 minute timescales in GRS 1915+105.Comment: 17 pages, 9 figures; accepted for publication in The Astrophysical
Journa
Shapes and Positions of Black Hole Shadows in Accretion Disks and Spin Parameters of Black Holes
Can we determine a spin parameter of a black hole by observation of a black
hole shadow in an accretion disk? In order to answer this question, we make a
qualitative analysis and a quantitative analysis of a shape and a position of a
black hole shadow casted by a rotating black hole on an optically thick
accretion disk and its dependence on an angular momentum of a black hole. We
have found black hole shadows with a quite similar size and a shape for largely
different black hole spin parameters and a same black hole mass. Thus, it is
practically difficult to determine a spin parameter of a black hole from a size
and a shape of a black hole shadow in an accretion disk. We newly introduce a
bisector axis of a black hole shadow named a shadow axis. For a rotating black
hole a shape and a position of a black hole shadow are not symmetric with
respect to a rotation axis of a black hole shadow. So, in this case the minimum
interval between a mass center of a black hole and a shadow axis is finite. An
extent of this minimum interval is roughly proportional to a spin parameter of
a black hole for a fixed inclination angle between a rotation axis of a black
hole and a direction of an observer. In order to measure a spin parameter of a
black hole, if a shadow axis is determined observationally, it is crucially
important to determine a position of a mass center of a black hole in a region
of a black hole shadow.Comment: 13 pages, 6 figures, accepted for publication in Ap
Anti-correlation between the mass of a supermassive black hole and the mass accretion rate in type I ultraluminous infrared galaxies and nearby QSOs
We discovered a significant anti-correlation between the mass of a
supermassive black hole (SMBH), , and the luminosity ratio of
infrared to active galactic nuclei (AGN) Eddington luminosity, , over four orders of magnitude for ultraluminous infrared
galaxies with type I Seyfert nuclei (type I ULIRGs) and nearby QSOs. This
anti-correlation ( vs. ) can be interpreted
as the anti-correlation between the mass of a SMBH and the rate of mass
accretion onto a SMBH normalized by the AGN Eddington rate, . In other words, the mass accretion rate is not proportional to that of the central BH mass. Thus, this
anti-correlation indicates that BH growth is determined by the external mass
supply process, and not the AGN Eddington-limited mechanism. Moreover, we found
an interesting tendency for type I ULIRGs to favor a super-Eddington accretion
flow, whereas QSOs tended to show a sub-Eddington flow. On the basis of our
findings, we suggest that a central SMBH grows by changing its mass accretion
rate from super-Eddington to sub-Eddington. According to a coevolution scenario
of ULIRGs and QSOs based on the radiation drag process, it has been predicted
that a self-gravitating massive torus, whose mass is larger than a central BH,
exists in the early phase of BH growth (type I ULIRG phase) but not in the
final phase of BH growth (QSO phase). At the same time, if one considers the
mass accretion rate onto a central SMBH via a turbulent viscosity, the
anti-correlation ( vs. ) is well explained
by the positive correlation between the mass accretion rate
and the mass ratio of a massive torus to a SMBH.Comment: 29 pages, 4 figures, accepted for publication in Ap
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