1,141 research outputs found
Stimulated Raman scattering of water maser lines in astrophysical plasmas
Radiative transfer equations are derived and solved for the stimulated Raman
scattering of water maser lines in the astrophysical plasmas with electron
density of about 10^6 - 10^7 cm-3. In stimulated Raman scattering, the energy
of water maser line is transferred to the side band modes: Stokes mode and
anti-Stokes mode. The Stokes mode is easily produced by backward Raman
scattering while the anti-Stokes mode is created by the interacting
intersecting masers in the plasma. The intensity of the Stokes mode is higher
than that of the anti-Stokes mode. These side band modes are proposed as
explanation for the extreme velocity features observed in the galaxy NGC 4258.
The threshold value of the brightness temperature for the Raman scattering is
about 10^16 - 10^19 K, and it is satisfied in the case of NGC 4258.Comment: 12 pages, 4 Postscript figures. Accepted for Physics of Plasma
Fredholm conditions for invariant operators: finite abelian groups and boundary value problems
We answer the question of when an invariant pseudodifferential operator is Fredholm on a fixed, given isotypical component. More precisely, let be a compact group acting on a smooth, compact, manifold without boundary and let be a -invariant, classical, pseudodifferential operator acting between sections of two -equivariant vector bundles and . Let be an irreducible representation of the group . Then induces by restriction a map between the -isotypical components of the corresponding Sobolev spaces of sections. We study in this paper conditions on the map to be Fredholm. It turns out that the discrete and non-discrete cases are quite different. Additionally, the discrete abelian case, which provides some of the most interesting applications, presents some special features and is much easier than the general case. We thus concentrate in this paper on the case when is finite abelian. We prove then that the restriction is Fredholm if, and only if, is "-elliptic", a condition defined in terms of the principal symbol of . If is elliptic, then is also -elliptic, but the converse is not true in general. However, if acts freely on a dense open subset of , then is -elliptic for the given fixed if, and only if, it is elliptic. The proofs are based on the study of the structure of the algebra of classical, -invariant pseudodifferential operators acting on sections of the vector bundle and of the structure of its restrictions to the isotypical components of . These structures are described in terms of the isotropy groups of the action of the group on
Particle Acceleration in three dimensional Reconnection Regions: A New Test Particle Approach
Magnetic Reconnection is an efficient and fast acceleration mechanism by
means of direct electric field acceleration parallel to the magnetic field.
Thus, acceleration of particles in reconnection regions is a very important
topic in plasma astrophysics. This paper shows that the conventional analytical
models and numerical test particle investigations can be misleading concerning
the energy distribution of the accelerated particles, since they oversimplify
the electric field structure by the assumption that the field is homogeneous.
These investigations of the acceleration of charged test particles are extended
by considering three-dimensional field configurations characterized by
localized field-aligned electric fields. Moreover, effects of radiative losses
are discussed. The comparison between homogeneous and inhomogeneous electric
field acceleration in reconnection regions shows dramatic differences
concerning both, the maximum particle energy and the form of the energy
distribution.Comment: 11 pages, 21 figure
Influence of the Lower Hybrid Drift Instability on the onset of Magnetic Reconnection
Two-dimensional and three-dimensional kinetic simulation results reveal the
importance of the Lower-Hybrid Drift Instability LHDI to the onset of magnetic
reconnection. Both explicit and implicit kinetic simulations show that the LHDI
heats electrons anisotropically and increases the peak current density. Linear
theory predicts these modifications can increase the growth rate of the tearing
instability by almost two orders of magnitude and shift the fastest growing
modes to significantly shorter wavelengths. These predictions are confirmed by
nonlinear kinetic simulations in which the growth and coalescence of small
scale magnetic islands leads to a rapid onset of large scale reconnection
Non-thermal Processes in Black-Hole-Jet Magnetospheres
The environs of supermassive black holes are among the universe's most
extreme phenomena. Understanding the physical processes occurring in the
vicinity of black holes may provide the key to answer a number of fundamental
astrophysical questions including the detectability of strong gravity effects,
the formation and propagation of relativistic jets, the origin of the highest
energy gamma-rays and cosmic-rays, and the nature and evolution of the central
engine in Active Galactic Nuclei (AGN). As a step towards this direction, this
paper reviews some of the progress achieved in the field based on observations
in the very high energy domain. It particularly focuses on non-thermal particle
acceleration and emission processes that may occur in the rotating
magnetospheres originating from accreting, supermassive black hole systems.
Topics covered include direct electric field acceleration in the black hole's
magnetosphere, ultra-high energy cosmic ray production, Blandford-Znajek
mechanism, centrifugal acceleration and magnetic reconnection, along with the
relevant efficiency constraints imposed by interactions with matter, radiation
and fields. By way of application, a detailed discussion of well-known sources
(Sgr A*; Cen A; M87; NGC1399) is presented.Comment: invited review for International Journal of Modern Physics D, 49
pages, 15 figures; minor typos corrected to match published versio
Shuffle relations for regularised integrals of symbols
We prove shuffle relations which relate a product of regularised integrals of
classical symbols to regularised nested (Chen) iterated integrals, which hold
if all the symbols involved have non-vanishing residue. This is true in
particular for non-integer order symbols. In general the shuffle relations hold
up to finite parts of corrective terms arising from renormalisation on tensor
products of classical symbols, a procedure adapted from renormalisation
procedures on Feynman diagrams familiar to physicists. We relate the shuffle
relations for regularised integrals of symbols with shuffle relations for
multizeta functions adapting the above constructions to the case of symbols on
the unit circle.Comment: 40 pages,latex. Changes concern sections 4 and 5 : an error in
section 4 has been corrected, and the link between section 5 and the previous
ones has been precise
Random Dirac operators with time-reversal symmetry
Quasi-one-dimensional stochastic Dirac operators with an odd number of
channels, time reversal symmetry but otherwise efficiently coupled randomness
are shown to have one conducting channel and absolutely continuous spectrum of
multiplicity two. This follows by adapting the criteria of Guivarch-Raugi and
Goldsheid-Margulis to the analysis of random products of matrices in the group
SO, and then a version of Kotani theory for these operators. Absence of
singular spectrum can be shown by adapting an argument of Jaksic-Last if the
potential contains random Dirac peaks with absolutely continuous distribution.Comment: parts of introduction made more precise, corrections as follow-up on
referee report
ROSAT Evidence for Intrinsic Oxygen Absorption in Cooling Flow Galaxies and Groups
Using spatially resolved, deprojected ROSAT PSPC spectra of 10 of the
brightest cooling flow galaxies and groups with low Galactic column densities
we have detected intrinsic absorption over energies ~0.4-0.8 keV in half of the
sample. Since no intrinsic absorption is indicated for energies below ~0.4 keV,
the most reasonable model for the absorber is collisionally ionized gas at
temperatures T=10^{5-6} K with most of the absorption arising from ionized
states of oxygen but with a significant contribution from carbon and nitrogen.
The soft X-ray emission of this warm gas can explain the sub-Galactic column
densities of cold gas inferred within the central regions of most of the
systems. Attributing the absorption to ionized gas reconciles the large columns
of cold H and He inferred from EINSTEIN and ASCA with the lack of such columns
inferred from ROSAT. Within the central ~10-20 kpc, where the constraints are
most secure, the estimated mass of the ionized absorber is consistent with most
(perhaps all) of the matter deposited by a cooling flow over the lifetime of
the flow. Since the warm absorber produces no significant H or He absorption
the large absorber masses are consistent with the negligible atomic and
molecular H inferred from HI and CO observations of cooling flows. It is also
found that if T > ~2x10^5 K then the optical and UV emission implied by the
warm gas does not violate published constraints. Finally, we discuss how the
prediction of warm ionized gas as the product of mass drop-out in these and
other cooling flows can be verified with new CHANDRA and XMM observations.
(Abridged)Comment: 17 pages (5 figures), Accepted for publication in ApJ, expanded
discussion of multiphase spectral models, theoretical implications of warm
gas in cooling flows, and the statistical significance of the oxygen
absorptio
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