268 research outputs found
Scenarios for ultrafast gamma-ray variability in AGN
We analyze three scenarios to address the challenge of ultrafast gamma-ray
variability reported from active galactic nuclei. We focus on the energy
requirements imposed by these scenarios: (i) external cloud in the jet, (ii)
relativistic blob propagating through the jet material, and (iii) production of
high-energy gamma rays in the magnetosphere gaps. We show that while the first
two scenarios are not constrained by the flare luminosity, there is a robust
upper limit on the luminosity of flares generated in the black hole
magnetosphere. This limit depends weakly on the mass of the central black hole
and is determined by the accretion disk magnetization, viewing angle, and the
pair multiplicity. For the most favorable values of these parameters, the
luminosity for 5-minute flares is limited by ,
which excludes a black hole magnetosphere origin of the flare detected from
IC310. In the scopes of scenarios (i) and (ii), the jet power, which is
required to explain the IC310 flare, exceeds the jet power estimated based on
the radio data. To resolve this discrepancy in the framework of the scenario
(ii), it is sufficient to assume that the relativistic blobs are not
distributed isotropically in the jet reference frame. A realization of scenario
(i) demands that the jet power during the flare exceeds by a factor the
power of the radio jet relevant to a timescale of years.Comment: 15 pages, accepted by Ap
Star-Jet Interactions and Gamma-Ray Outbursts from 3C454.3
We propose a model to explain the ultra-bright GeV gamma-ray flares observed
from the blazar 3C454.3. The model is based on the concept of a relativistic
jet interacting with compact gas condensations produced when a star (red giant)
crosses the jet close to the central black hole. The study includes an
analytical treatment of the evolution of the envelop lost by the star within
the jet, and calculations of the related high-energy radiation. The model
readily explains the day-long, variable on timescales of hours, GeV gamma-ray
flare from 3C454.3, observed during November 2010 on top of a weeks-long
plateau. In the proposed scenario, the plateau state is caused by a strong wind
generated by the heating of the star atmosphere by nonthermal particles
accelerated at the jet-star interaction region. The flare itself could be
produced by a few clouds of matter lost by the red giant after the initial
impact of the jet. In the framework of the proposed scenario, the observations
constrain the key model parameters of the source, including the mass of the
central black hole: , the total jet power:
, and the Doppler factor of the
gamma-ray emitting clouds, . Whereas we do not specify the
particle acceleration mechanisms, the potential gamma-ray production processes
are discussed and compared in the context of the proposed model. We argue that
synchrotron radiation of protons has certain advantages compared to other
radiation channels of directly accelerated electrons.Comment: 16 pages, 5 figures, submitted to Ap
Post-Periastron Gamma Ray Flare from PSR B1259-63/LS 2883 as a Result of Comptonization of the Cold Pulsar Wind
We argue that the bright flare of the binary pulsar \object{PSR
B125963/LS2883} detected by the {\it Fermi} Large Area Telescope (LAT), is
due to the inverse Compton (IC) scattering of the unshocked electron-positron
pulsar wind with a Lorentz factor . The combination of
two effects both linked to the circumstellar disk (CD), is a key element in the
proposed model. The first effect is related to the impact of the surrounding
medium on the termination of the pulsar wind. Inside the disk, the "early"
termination of the wind results in suppression of its gamma-ray luminosity.
When the pulsar escapes the disk, the conditions for termination of the wind
undergo significant changes. This would lead to a dramatic increase of the
pulsar wind zone, and thus to the proportional increase of the gamma-ray flux.
On the other hand, if the parts of the CD disturbed by the pulsar can supply
infrared photons of density high enough for efficient Comptonization of the
wind, almost the entire kinetic energy of the pulsar wind would be converted to
radiation, thus the gamma-ray luminosity of the wind could approach to the
level of the pulsar's spin-down luminosity as reported by the {\it Fermi}
collaboration.Comment: 14 pages, 4 figure
Hydrodynamics of interaction of pulsar and stellar winds and its impact on the high energy radiation of binary pulsar systems
The hydrodynamics of the interaction of pulsar and stellar winds in binary
systems harboring a pulsar and its impact on the nonthermal radiation of the
binary pulsar PSR B1259-63/SS2883 is discussed. The collision of an
ultrarelativistic pulsar wind with a nonrelativistic stellar outflow results in
significant bulk acceleration of the shocked material from the pulsar wind.
Already at distances comparable to the size of the binary system, the Lorentz
factor of the shocked flow can be as large as ~4. This results in
significant anisotropy of the inverse Compton radiation of accelerated
electrons. Because of the Doppler boosting of the produced radiation, one
should expect a variable gamma-ray signal from the system. In particular, this
effect may naturally explain the reported tendency of a decrease of TeV
gamma-ray flux close to the periastron. The modeling of the interaction of
pulsar and stellar winds allows self-consistent calculations of adiabatic
losses. Our results show that adiabatic losses dominate over the radiative
losses. These results have direct impact on the orbital variability of radio,
X-ray and gamma-ray signals detected from the binary pulsar PSR 1259-63/SS2883.Comment: 4 pages, 4 figures; based on poster presentation at "High Energy
Phenomena in Relativistic Outflows", Dublin, Sept. 2007; accepted for
publication in International Journal of Modern Physics
Simulations of stellar/pulsar wind interaction along one full orbit
The winds from a non-accreting pulsar and a massive star in a binary system
collide forming a bow-shaped shock structure. The Coriolis force induced by
orbital motion deflects the shocked flows, strongly affecting their dynamics.
We study the evolution of the shocked stellar and pulsar winds on scales in
which the orbital motion is important. Potential sites of non-thermal activity
are investigated. Relativistic hydrodynamical simulations in two dimensions,
performed with the code PLUTO and using the adaptive mesh refinement technique,
are used to model interacting stellar and pulsar winds on scales ~80 times the
distance between the stars. The hydrodynamical results suggest the suitable
locations of sites for particle acceleration and non-thermal emission. In
addition to the shock formed towards the star, the shocked and unshocked
components of the pulsar wind flowing away from the star terminate by means of
additional strong shocks produced by the orbital motion. Strong instabilities
lead to the development of turbulence and an effective two-wind mixing in both
the leading and trailing sides of the interaction structure, which starts to
merge with itself after one orbit. The adopted moderate pulsar-wind Lorentz
factor already provides a good qualitative description of the phenomena
involved in high-mass binaries with pulsars, and can capture important physical
effects that would not appear in non-relativistic treatments. Simulations show
that shocks, instabilities, and mass-loading yield efficient mass, momentum,
and energy exchanges between the pulsar and the stellar winds. This renders a
rapid increase in the entropy of the shocked structure, which will likely be
disrupted on scales beyond the simulated ones. Several sites of particle
acceleration and low- and high-energy emission can be identified. Doppler
boosting will have significant and complex effects on radiation.Comment: 8 pages, 11 figures, Astronomy and Astrophysics, in press, minor
changes after acceptanc
Clues to unveil the emitter in LS 5039: powerful jets vs colliding winds
LS 5039 is among the most interesting VHE sources in the Galaxy. Two
scenarios have been put forward to explain the observed TeV radiation: jets vs
pulsar winds. The source has been detected during the superior conjunction of
the compact object, when very large gamma-ray opacities are expected. In
addition, electromagnetic cascades, which may make the system more transparent
to gamma-rays, are hardly efficient for realistic magnetic fields in massive
star surroundings. All this makes unlikely the standard pulsar scenario for LS
5039, in which the emitter is the region located between the star and the
compact object, where the opacities are the largest. Otherwise, a jet-like flow
can transport energy to regions where the photon-photon absorption is much
lower and the TeV radiation is not so severely absorbed.Comment: 3 pages, 3 Figures, contribution to the "Fourth Heidelberg
International Symposium on High-Energy Gamma-Ray Astronomy 2008
Modeling interaction of relativistic and nonrelativistic winds in binary system PSR 1259-63/SS2883. I.Hydrodynamical limit
In this paper, we present a detailed hydrodynamical study of the properties
of the flow produced by the collision of a pulsar wind with the surrounding in
a binary system. This work is the first attempt to simulate interaction of the
ultrarelativistic flow (pulsar wind) with the nonrelativistic stellar wind.
Obtained results show that the wind collision could result in the formation of
an "unclosed" (at spatial scales comparable to the binary system size) pulsar
wind termination shock even when the stellar wind ram pressure exceeds
significantly the pulsar wind kinetical pressure. Moreover, the post-shock flow
propagates in a rather narrow region, with very high bulk Lorentz factor
(). This flow acceleration is related to adiabatical losses,
which are purely hydrodynamical effects. Interestingly, in this particular
case, no magnetic field is required for formation of the ultrarelativistic bulk
outflow. The obtained results provide a new interpretation for the orbital
variability of radio, X-ray and gamma-ray signals detected from binary pulsar
system PSR 1259-63/SS2883.Comment: 11 pages, 13 figures, submitted to MNRA
Non-thermal emission from secondary pairs in close TeV binary systems
Massive hot stars produce dense ultraviolet (UV) photon fields in their
surroundings. If a very high-energy (VHE) gamma-ray emitter is located close to
the star, then gamma-rays are absorbed in the stellar photon field, creating
secondary (electron-positron) pairs. We study the broadband emission of these
secondary pairs in the stellar photon and magnetic fields. Under certain
assumptions on the stellar wind and the magnetic field in the surroundings of a
massive hot star, we calculate the steady state energy distribution of
secondary pairs created in the system and its radiation from radio to
gamma-rays. Under the ambient magnetic field, possibly high enough to suppress
electromagnetic (EM) cascading, the energy of secondary pairs is radiated via
synchrotron and single IC scattering producing radio-to-gamma-ray radiation.
The synchrotron spectral energy distribution (SED) is hard, peaks around X-ray
energies, and becomes softer. The IC SED is hard as well and peaks around 10
GeV, becoming also softer at higher energies due to synchrotron loss dominance.
The radio emission from secondary pairs is moderate and detectable as a
point-like and/or extended source. In X-rays, the secondary pair synchrotron
component may be dominant. At energies <10 GeV, the secondary pair IC radiation
may be the dominant primary gamma-ray emission and possibly detectable by the
next generation of instruments.Comment: accepted for publication in Astronomy & Astrophysics, 6 pages, 8
figure
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