486 research outputs found
Analytic Model for Advection-Dominated Accretion Flows in a Global Magnetic Field
A model for advection-dominated accretion flows (ADAFs) in a global magnetic
field is proposed. In contrast to the well known ADAF models in which the
viscosity of a fluid determines both angular momentum transfer and energy
dissipation in the flow, the magnetic field and the electric resistivity,
respectively, control them in this model. A manageable set of analytic
solutions for the flow and the magnetic field is obtained to vertically
non-integrated basic equations. This set describes mathematically a fully
advective accretion flow and, in physically plausible situations for most AGNs,
it is also confirmed that the radiation cooling estimated on this solution is
really negligible compared with the internal energy of the flow.Comment: 27pages, 1 figure, to appear in ApJ vol 529, Feb.1, 200
Global Operation of Resistive, Radiation-Inefficient, Accretion Flows in Preparing Jet-Driving Circumstances
In our recent paper, we have obtained a model solution to the problem of
radiation-inefficient accretion flows (RIAFs) in a global magnetic field (so
called, resistive RIAF model), which is asymptotically exact in outer regions
of such flows forming accretion disks. When extrapolated inwardly, the model
predicts a local enhancement of the vertical Poynting flux within a small
radius that may be regarded as the disk inner-edge. This fact has been
interpreted as the origin of power source for the astrophysical jets
observationally well-known to be ejected from this type of accretion disks.
Since the accuracy of the solution may become rather poor in such inner
regions, however, the ground of this assertion may not seem to be so firm. In
the present paper, we develop a sophisticated discussion for the appearance of
jet-driving circumstances, based on a much more firm ground by deriving a
global solution in the same situation. Although the new solution still has an
approximate nature, it becomes exact in the limits not only of large radius but
also of small radius. The analytic results clarify that the electrodynamic
power is gathered by the Poynting flux, from outer main-disk region to feed the
innermost part of an accretion disk. The injected power largely exceeds the
local supply of work by the fluid motion.Comment: 10 pages, 3 figures, accepted for publication in PAS
Two Types of Magnetohydrodynamic Sheath Jets
Recent observations of astrophysical jets emanating from various galactic
nuclei strongly suggest that a double layered structure, or a spine-sheath
structure, is likely to be their common feature. We propose that such a sheath
jet structure can be formed magnetohydrodynamically within a valley of the
magnetic pressures, which is formed between the peaks due to the poloidal and
toroidal components, with the centrifugal force acting on the rotating sheath
plasma is balanced by the hoop stress of the toroidal field. The poloidal field
concentrated near the polar axis is maintained by a converging plasma flow
toward the jet region, and the toroidal field is developed outside the jet cone
owing to the poloidal current circulating through the jet. Under such
situations, the set of magnetohydrodynamic (MHD) equations allows two main
types of solutions, at least, in the region far from the footpoint. The first
type solution describes the jets of marginally bound nature. This type is
realized when the jet temperature decreases like viral one, and neither the
pressure-gradient nor the MHD forces, which are both determined consistently,
cannot completely overcome the gravity even at infinity. The second type is
realized under an isothermal situation, and the gravity is cancelled exactly by
the pressure-gradient force. Hence, the jets of this type are accelerated
purely by the MHD force. It is suggested also that these two types correspond,
respectively, to the jets from type I and II radio galaxies in the
Fanaroff-Riley classification.Comment: 12 pages, 1 figure, to appear in PASJ, Vol.61, No.
Criterion for Generation of Winds from Magnetized Accretion Disks
An analytic model is proposed for non-radiating accretion flows accompanied
by up or down winds in a global magnetic field. Physical quantities in this
model solution are written in variable-separated forms, and their radial parts
are simple power law functions including one parameter for wind strength.
Several, mathematically equivalent but physically different expressions of the
criterion for wind generation are obtained. It is suggested also that the
generation of wind is a consequence of the intervention of some mechanism that
redistributes the locally available gravitational energy, and that the
Bernoulli sum can be a good indicator of the existence of such mechanisms.Comment: 24 pages, 0 figures, ApJ accepte
Radiation Spectra from Advection-Dominated Accretion Flows in a Global Magnetic Field
We calculate the radiation spectra from advection-dominated accretion flows
(ADAFs), taking into account the effects of a global magnetic field.
Calculation is based on the analytic model for magnetized ADAFs proposed by
Kaburaki, where a large-scale magnetic field controls the accretion process.
Adjusting a few parameters, we find that our model can well reproduce the
observed spectrum of Sagittarius A. The result is discussed in comparison
with those of well-known ADAF models, where the turbulent viscosity controls
the accretion process.Comment: Accepted for publication in Ap
What Kinds of Accretion Disks Are There in the Nuclei of Radio Galaxies?
It seems to be a widely accepted opinion that the types of accretion disks
(or flows) generally realized in the nuclei of radio galaxies and in further
lower mass-accretion rate nuclei are inner, hot, optically thin, radiatively
inefficient accretion flows (RIAFs) surrounded by outer, cool, optically thick,
standard type accretion disks. However, observational evidence for the
existence of such outer cool disks in these nuclei is rather poor. Instead,
recent observations sometimes suggest the existence of inner cool disks of
non-standard type, which develop in the region very close to their central
black holes. Taking NGC 4261 as a typical example of such light eating nuclei,
for which both flux data ranging from radio to X-ray and data for the
counterjet occultation are available, we examine the plausibility of such a
picture for the accretion states as mentioned above, based on model
predictions. It is shown that the explanation of the gap seen in the counterjet
emission in terms of the free-free absorption by an outer standard disk is
unrealistic, and moreover, the existence itself of such an outer standard disk
seems very implausible. Instead, the model of RIAF in an ordered magnetic field
(so called resistive RIAF model) can well serve to explain the emission gap in
terms of the synchrotron absorption, as well as to reproduce the observed
features of the overall spectral energy distribution (SED). This model also
predicts that the RIAF state starts directly from an interstellar hot gas phase
at around the Bondi radius and terminates at the inner edge whose radius is
about 100 times the Schwartzschild radii. Therefore, there is a good
possibility for a cool disk to develop within this innermost region.Comment: 8 pages, 3 figures, to appear in PASJ, Vol.62, No.
Appearance of Jet-Driving Poynting Flux in Hot, Tenuous Accretion Disks Threaded by an Ordered Magnetic Field
In a series of our previous works, a model of radiatively inefficient
accretion flows (RIAFs) in a global magnetic field (so called resistive RIAF
model) has proved its ability to account for many physical processes taking
place in such accretion flows as realized in the nuclei of the galaxies
believed to be accreting at a very small fraction of each Eddinton accretion
rate. Within the present status of this model, however, the model cannot
describe the launch of a self-confined bipolar jet from the vicinity of disk's
inner edge, although it allows the existence of a thermal wind widely
distributed over the disk surfaces. This is because the electric field (and
hence the Poynting flux) vanishes everywhere in the disk, whereas such a jet in
a globally ordered magnetic field is most likely to be accelerated
electrodynamically. We show in the present paper that this defect can be
overcome naturally if we reformulate the problem so as to admit a
quasi-stationary change of the magnetic field (and hence the appearance of a
non-irrotational electric field), and also restore all the terms of order
epsilon ~ (v_r/v_{varphi})^2 < 1 (where v_r and v_{varphi} denote radial and
azimuthal components, respectively, of the fluid velocity) which have been
neglected altogether in the previous treatments. The restored effects are the
inertial and magnetic draggings on the infalling matter. As an illustrative
example, a model solution which is correct up to the first order in epsilon is
derived under a set of plausible restrictions. The new solution predicts the
appearance of a localized Poynting flux in a region near the disk inner edge,
suggesting strongly that a jet is launched from this region. Another
interesting prediction is the appearance of a rapid change of the magnetic
field also localized to this region.Comment: 13 pages, 1 figure, accepted for publication in PAS
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