1,256 research outputs found
Astrophysics with High Energy Gamma Rays
Recent results, the present status and the perspectives of high energy
gamma-ray astronomy are described. Since the satellite observations by the
Compton Gamma Ray Observatory and its precursor missions have been reviewed
extensively, emphasis is on the results from the ground-based gamma-ray
telescopes. They concern the physics of Pulsar Nebulae, Supernova Remnants in
their assumed role as the Galactic sources of Cosmic Rays, Jets from Active
Galactic Nuclei, and the Extragalactic Background radiation field due to stars
and dust in galaxies. Since the gamma-ray emission is nonthermal, this kind of
astronomy deals with the pervasive high-energy nonequilibrium states in the
Universe. The present build-up of larger and more sensitive instruments, both
on the ground and in space, gives fascinating prospects also for observational
cosmology and astroparticle physics. Through realistically possible further
observational developments at high mountain altitudes a rapid extension of the
field is to be expected.Comment: 23 pages, 11 figures. To appear in "Astronomy, Cosmology and
Fundamental Physics", ed. P. A. Shaver, L. Di Lella, and A. Gimenez, Proc.
ESA-CERN-ESO Symposium, Garching, March 2002. Springer-Verlag, Berlin,
Heidelberg, series "ESO Astrophysics Symposia
Cosmic ray acceleration parameters from multi-wavelength observations. The case of SN 1006
The properties of the Galactic supernova remnant SN 1006 are theoretically
reanalysed. Nonlinear kinetic theory is used to determine the acceleration
efficiency of cosmic rays (CRs) in the supernova remnant SN 1006. The known
range of astronomical parameters and the existing measurements of nonthermal
emission are examined in order to define the values of the relevant physical
parameters which determine the CR acceleration efficiency. It is shown that the
parameter values -- proton injection rate, electron to proton ratio and
downstream magnetic field strength -- are determined with the appropriate
accuracy. In particular also the observed azimuthal variations in the gamma-ray
morphology agree with the theoretical expectation. These parameter values,
together with the reduction of the gamma-ray flux relative to a spherically
symmetric acceleration geometry, allow a good fit to the existing data,
including the recently detected TeV emission by H.E.S.S. SN 1006 represents the
first example where a high efficiency of nuclear CR production, required for
the Galactic CR sources, is consistently established.Comment: 10 pages, 6 figures, accepted for publication in A&
The Galactic Centre - A Laboratory for Starburst Galaxies (?)
The Galactic centre - as the closest galactic nucleus - holds both intrinsic
interest and possibly represents a useful analogue to star-burst nuclei which
we can observe with orders of magnitude finer detail than these external
systems. The environmental conditions in the GC - here taken to mean the inner
200 pc in diameter of the Milky Way - are extreme with respect to those
typically encountered in the Galactic disk. The energy densities of the various
GC ISM components are typically ~two orders of magnitude larger than those
found locally and the star-formation rate density ~three orders of magnitude
larger. Unusually within the Galaxy, the Galactic centre exhibits
hard-spectrum, diffuse TeV (=10^12 eV) gamma-ray emission spatially coincident
with the region's molecular gas. Recently the nuclei of local star-burst
galaxies NGC 253 and M82 have also been detected in gamma-rays of such
energies. We have embarked on an extended campaign of modelling the broadband
(radio continuum to TeV gamma-ray), non- thermal signals received from the
inner 200 pc of the Galaxy. On the basis of this modelling we find that
star-formation and associated supernova activity is the ultimate driver of the
region's non-thermal activity. This activity drives a large-scale wind of hot
plasma and cosmic rays out of the GC. The wind advects the locally-accelerated
cosmic rays quickly, before they can lose much energy in situ or penetrate into
the densest molecular gas cores where star-formation occurs. The cosmic rays
can, however, heat/ionize the lower density/warm H2 phase enveloping the cores.
On very large scales (~10 kpc) the non-thermal signature of the escaping GC
cosmic rays has probably been detected recently as the spectacular 'Fermi
bubbles' and corresponding 'WMAP haze'.Comment: Invited talk to appear in Proceedings of IAU Symposium No. 284, 2011
(R.J. Tuffs & C.C. Popescu, eds.) `The Spectral Energy Distribution of
Galaxies
Cosmic Ray Acceleration by Spiral Shocks in the Galactic Wind
Cosmic ray acceleration by shocks related with Slipping Interaction Regions
(SIRs) in the Galactic Wind is considered. SIRs are similar to Solar Wind
Corotating Interaction Regions. The spiral structure of our Galaxy results in a
strong nonuniformity of the Galactic Wind flow and in SIR formation at
distances of 50 to 100 kpc. SIRs are not corotating with the gas and magnetic
field because the angular velocity of the spiral pattern differs from that of
the Galactic rotation. It is shown that the collective reacceleration of the
cosmic ray particles with charge in the resulting shock ensemble can
explain the observable cosmic ray spectrum beyond the "knee" up to energies of
the order of eV. For the reaccelerated particles the Galactic Wind
termination shock acts as a reflecting boundary.Comment: LATEX, 14 pages, 7 figures, accepted to A&
Cosmic-Ray Induced Diffuse Emissions from the Milky Way and Local Group Galaxies
Cosmic rays fill up the entire volume of galaxies, providing an important
source of heating and ionisation of the interstellar medium, and may play a
significant role in the regulation of star formation and galactic evolution.
Diffuse emissions from radio to high-energy gamma rays (> 100 MeV) arising from
various interactions between cosmic rays and the interstellar medium,
interstellar radiation field, and magnetic field, are currently the best way to
trace the intensities and spectra of cosmic rays in the Milky Way and other
galaxies. In this contribution, I describe our recent work to model the full
spectral energy distribution of galaxies like the Milky Way from radio to
gamma-ray energies. The application to other galaxies, in particular the
Magellanic Clouds and M31 that are detected in high-energy gamma-rays by the
Fermi-LAT, is also discussed.Comment: Contribution to "The Spectral Energy Distribution of Galaxies"
Proceedings IAU Symposium No. 284, 2011, eds. R.J. Tuffs & C.C.Popescu. 4
pages with 4 figure
Magnetic Field Amplification in Tycho and other Shell-type Supernova Remnants
It is shown that amplification of the magnetic field in supernova remnants
(SNRs) occurs in all six objects where morphological measurements are presently
available in the hard X-ray continuum at several keV. For the three
archetypical objects (SN 1006, Cas A and Tycho's SNR) to which nonlinear
time-dependent acceleration theory has been successfully applied up to now, the
global theoretical and the local observational field strengths agree very well,
suggesting in addition that all young SNRs exhibit the amplification effect as
a result of very efficient acceleration of nuclear cosmic rays (CRs) at the
outer shock. Since this appears to be empirically the case, we may reverse the
argument and consider field amplification as a measure of nuclear CR
acceleration and it has indeed been argued that acceleration in the amplified
fields allows the CR spectrum from SNRs to reach the knee in the spectrum or,
in special objects, even beyond. The above results are furthermore used to
investigate the time evolution of field amplification in young SNRs. Although
the uncertainties in the data do not allow precise conclusions regarding this
point, they rather clearly show that the ratio of the magnetic field energy
density and the kinetic energy density of gas flow into the shock is of the
order of a few percent if the shock speed is high enough V_s > 10^3 km/s, and
this ratio remains nearly constant during the SNR evolution. The escape of the
highest energy nuclear particles from their sources becomes progressively
important with age, reducing also the cutoff in the \pi^0 -decay gamma-ray
emission spectrum with time after the end of the sweep-up phase. Simultaneously
the leptonic gamma-ray channels will gain in relative importance with
increasing age of the sources.Comment: 13 pages, 8 figures, accepted for publication in A&
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