1,536 research outputs found
Off-axis emission from relativistic plasma flows
We show that there is no universal law describing how the spectra and
luminosity of synchrotron and inverse Compton radiation from relativistic jets
change with increasing observation angle. Instead, the physics of particle
acceleration leaves pronounced imprints in the observed spectra and allows for
a freedom in numerous modifications of them. The impact of these effects is the
largest for high-energy radiation and depends on the details of particle
acceleration mechanism(s), what can be used to discriminate between different
models. Generally, the beam patterns of relativistic jets in GeV-TeV spectral
domain are much wider than the inverse Lorentz factor. The off-axis emission in
this energy range appear to be brighter, have much harder spectra and a much
higher cut-off frequency compared to the values derived from Doppler boosting
considerations alone.
The implications include the possibility to explain high-latitude
unidentified EGRET sources as off-axis but otherwise typical relativistic-jet
sources, such as blazars, and the prediction of GeV-TeV afterglow from
transient jet sources, such as Gamma-Ray Bursts. We also discuss the phenomenon
of beam-pattern broadening in application to neutrino emission.Comment: Submitted to the Astrophysical Journa
High-energy emission from off-axis relativistic jets
We analyze how the spectrum of synchrotron and inverse Compton radiation from
a narrow relativistic jet changes with the observation angle. It is shown that
diversity of acceleration mechanisms (in particular, taking the converter
mechanism (Derishev et al. 2003) into account) allows for numerous
modifications of the observed spectrum. In general, the off-axis emission in
GeV-TeV energy range appears to be brighter, has a much harder spectrum and a
much higher cut-off frequency compared to the values derived from Doppler
boosting considerations alone. The magnitude of these effects depends on the
details of particle acceleration mechanisms, what can be used to discriminate
between different models.
One of the implications is the possibility to explain high-latitude
unidentified EGRET sources as off-axis but otherwise typical relativistic-jet
sources, such as blazars. We also discuss the broadening of beam pattern in
application to bright transient jet sources, such as Gamma-Ray Bursts.Comment: 6 pages, Proceedings of the International Symposium "High Energy
Gamma-Ray Astronomy", 26-30 July 2004, Heidelberg, German
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
Potential Neutrino Signals from Galactic Gamma-Ray Sources
The recent progress made in Galactic gamma-ray astronomy using the High
Energy Stereoskopic System (H.E.S.S.) instrument provides for the first time a
population of Galactic TeV gamma-rays, and hence potential neutrino sources,
for which the neutrino flux can be estimated. Using the energy spectra and
source morphologies measured by H.E.S.S., together with new parameterisations
of pion production and decay in hadronic interactions, we estimate the signal
and background rates expected for these sources in a first-generation water
Cherenkov detector (ANTARES) and a next-generation neutrino telescope in the
Mediterranean Sea, KM3NeT, with an instrumented volume of 1 km^3. We find that
the brightest gamma-ray sources produce neutrino rates above 1 TeV, comparable
to the background from atmospheric neutrinos. The expected event rates of the
brightest sources in the ANTARES detector make a detection unlikely. However,
for a 1 km^3 KM3NeT detector, event rates of a few neutrinos per year from
these sources are expected, and the detection of individual sources seems
possible. Although generally these estimates should be taken as flux upper
limits, we discuss the conditions and type of gamma-ray sources for which the
neutrino flux predictions can be considered robust.Comment: 20 pages, 4 figures; v2: ERROR in energy scale of KM3NeT effective
neutrino area corrected which resulted in event rates being about a factor 3
too low; v3: grammatical changes and update of references after receiving
proof
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
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
Electromagnetic radiation initiated by hadronic jets from microquasars in the ISM
Microquasars are potential candidates to produce a non-negligible fraction of
the observed galactic cosmic rays. The protons accelerated at the jet
termination shock interact with the interstellar medium and may produce
detectable fluxes of extended emission at different energy bands: high-energy
and very high-energy gamma-rays produced by neutral pion-decay, synchrotron and
bremsstrahlung emission in a wide energy range generated by the secondary
electrons produced by charged pion-decay. We discuss the association between
this scenario and some of the unidentified EGRET sources in the galactic plane.Comment: (1)Universitat de Barcelona (2)Max Planck institute fur kernphysik,
11 pages, 14 figures, accepted for publication in Astronomy & Astrophysic
On the anomalously large extension of the Pulsar Wind Nebula HESS J1825-137
The very high energy (VHE) gamma-ray emission reported from a number of
pulsar wind nebulae (PWNe) is naturally explained by the inverse Compton
scattering of multi-TeV electrons. However, the physical dimensions of some
gamma-ray-emitting PWNe significantly exceed the scales anticipated by the
standard hydrodynamical paradigm of PWN formation. The most "disturbing" case
in this regard is HESS J1825-137, which extends to distances
from the central pulsar PSR J1826-1334. If the gamma-ray
emission is indeed produced inside the PWN, but not by electrons that escaped
the nebula and diffuse in the interstellar medium (ISM), the formation of such
an anomalously extended plerion could be realized, in a diluted environment
with the hydrogen number density . In this
paper, we explore an alternative scenario assuming that the pulsar responsible
for the formation of the nebula initially had a very short rotation period. In
this case, the sizes of both the PWN and the surrounding supernova remnant
depend on the initial pulsar period, the braking index, and the ISM density. To
check the feasibility of this scenario, we study the parameter space that would
reproduce the size of HESS J1825-137. We show that this demand can be achieved
if the braking index is small, and the pulsar birth period is short,
. This scenario can reproduce the wind termination
position, which is expected at , only in a dense
environment with . The requirement of the dense
surrounding gas is supported by the presence of molecular clouds found in the
source vicinity.Comment: 15 pages, 6 figures, ApJ accepte
Gamma-ray flares from red giant/jet interactions in AGN
Non-blazar AGN have been recently established as a class of gamma-ray
sources. M87, a nearby representative of this class, show fast TeV variability
on timescales of a few days. We suggest a scenario of flare gamma-ray emission
in non-blazar AGN based on a red giant interacting with the jet at the base. We
solve the hydrodynamical equations that describe the evolution of the envelope
of a red giant blown by the impact of the jet. If the red giant is at least
slightly tidally disrupted by the supermassive black hole, enough stellar
material will be blown by the jet, expanding quickly until a significant part
of the jet is shocked. This process can render suitable conditions for energy
dissipation and proton acceleration, which could explain the detected day-scale
TeV flares from M87 via proton-proton collisions. Since the produced radiation
would be unbeamed, such an events should be mostly detected from non-blazar
AGN. They may be frequent phenomena, detectable in the GeV-TeV range even up to
distances of Gpc for the most powerful jets. The counterparts at lower
energies are expected to be not too bright.} {M87, and nearby non-blazar AGN in
general, can be fast variable sources of gamma-rays through red giant/jet
interactions.Comment: 8 pages, 4 figure
Broad-band electromagnetic radiation from microquasars interacting with ISM
Microquasars (MQs) are galactic objects with relativistic jets that
constitute a source population which can be responsible for production of a
non-negligible fraction of the observed galactic cosmic rays. These
relativistic protons, associated with the termination of the jet, interact with
the interstellar medium and, at certain surrounding conditions, may lead to
production of detectable fluxes of high-energy and very high-energy gamma-rays.
This radiation is accompanied by the broad-band emission of secondary electrons
from decays of -mesons produced through synchrotron, bremstrahlung and
inverse Compton process. The features of broad-band emission initiated by
proton-proton (pp) interactions in such a scenario is discussed in the context
of the strategy of search for counterparts of high-energy and very high-energy
gamma-ray sources in the galactic plane.Comment: High Energy Gamma-Ray Astronomy: 2nd International Symposium,
Proceedings of the conference held 26-30 July 2004 in Heidelberg (Germany).
Edited by Felix A. Aharonian, Heinz J. Volk, and Dieter Horns. AIP Conference
Proceedings, Volume 745. New York: American Institute of Physics, 2005.,
p.317-32
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