569 research outputs found
XMM-Newton study of the ULIRG NGC 6240
A recently performed XMM-Newton observation of the ULIRG NGC 6240 clearly
indicates the presence of an AGN contribution to its X-ray spectrum. In the 5.0
- 7.0 keV energy range there is a clear signature of the fluorescent Fe K lines
at 6.4, 6.7 and 6.9 keV, respectively.
The line strength of the 6.4 keV line cannot be produced by a thermal
component. The 0.3 - 10.0 keV spectral energy distribution is characterized by
the following components: (I) two hot thermal components (the starburst), (II)
one direct component (heavily absorbed; AGN is hidden), (III) one reflection
component (the AGN), (IV) three narrow Fe lines. The model parameters for the
broad-band spectral energy distribution are consistent with the results of
previously works.Comment: 2 pages incl. 2 figures, to appear in the proceedings of the "New
Century of X-ray Astronomy" symposium held in Yokohama, Japan (March 6-8,
2001), eds. H. Kunieda and H. Inoue, ASP pres
Supernova Neutrino Spectra and Applications to Flavor Oscillations
We study the flavor-dependent neutrino spectra formation in the core of a
supernova (SN) by means of Monte Carlo simulations. A high-statistics neutrino
signal from a galactic SN may contain information that severely constrains the
parameter space for neutrino oscillations. Therefore, reliable predictions for
flavor-dependent fluxes and spectra are urgently needed. In all traditional
hydrodynamic simulations the nu_mu,tau and nu_mu,tau-bar interactions commonly
included are rather schematic. With our Monte Carlo simulations we find that
the most relevant sources for nu_mu,tau and nu_mu,tau-bar are traditionally not
included. In comparing our numerical results for all flavors we find the
standard hierarchy of mean energies nu_e < nu_e-bar < nu_mu,tau, with, however,
very similar values for nu_mu,tau and nu_e-bar. The luminosities of nu_mu,tau
and nu_mu,tau-bar can differ by up to a factor of 2 from L_nue-bar and L_nue,
the latter two are very similar. The Garching Group obtains similar results
from their self-consistent simulation with the full set of interactions. These
results are almost orthogonal to the previous standard picture of exactly equal
luminosities of all flavors and differences in mean energies of up to a factor
of 2. Existing concepts for identifying oscillation effects in a SN neutrino
signal need to be revised. We present two methods for detecting the
earth-matter effect that are rather independent of predictions from SN
simulations.Comment: 138pp, Dissertation, Technische Universitaet Muenche
Identifying Earth matter effects on supernova neutrinos at a single detector
The neutrino oscillations in Earth matter introduce modulations in the
supernova neutrino spectra. These modulations can be exploited to identify the
presence of Earth effects on the spectra, which would enable us to put a limit
on the value of the neutrino mixing angle and to identify whether
the mass hierarchy is normal or inverted. We demonstrate how the Earth effects
can be identified at a single detector without prior assumptions about the
flavor-dependent source spectra, using the Fourier transform of the
``inverse-energy'' spectrum of the signal. We explore the factors affecting the
efficiency of this method, and find that the energy resolution of the detector
is the most crucial one. In particular, whereas water Cherenkov detectors may
need a few ten thousand events to identify the Earth effects, a few thousand
may be enough at scintillation detectors, which generically have a much better
energy resolution. A successful identification of the Earth effects through
this method can also provide to a good accuracy. The
relative strength of the detected Earth effects as a function of time provides
a test for supernova models.Comment: 18 pages, 10 figures, JCAP format. Final version to be published in
JCAP. References and some minor clarifications added to the original versio
Ledoux-Convection in Protoneutron Stars --- a Clue to Supernova Nucleosynthesis?
Two-dimensional hydrodynamical simulations of the deleptonization of a newly
formed neutron star were performed. Driven by negative lepton fraction and
entropy gradients, convection starts near the neutrinosphere about 20-30 ms
after core bounce, but moves deeper into the protoneutron star, and after about
one second the whole protoneutron star is convective. The deleptonization of
the star proceeds much faster than in the corresponding spherically symmetrical
model because the lepton flux and the neutrino luminosities increase by up to a
factor of two. The convection below the neutrinosphere raises the
neutrinospheric temperatures and mean energies of the emitted neutrinos by
10-20%. This can have important implications for the supernova explosion
mechanism and changes the detectable neutrino signal from the Kelvin-Helmholtz
cooling of the protoneutron star. In particular, the enhanced electron neutrino
flux relative to the electron antineutrino flux during the early post-bounce
evolution might solve the overproduction problem of certain elements in the
neutrino-heated ejecta in models of type-II supernova explosions.Comment: 17 pages, LaTeX, 8 postscript figures, uses epsf.sty. To appear in
ApJ 473 (Letters), 1996 December 1
Supernova neutrinos: Flavor-dependent fluxes and spectra
Transporting nu_mu and nu_tau in a supernova (SN) core involves several
processes that have been neglected in traditional simulations. Based on a Monte
Carlo study we find that the flavor-dependent spectral differences are much
smaller than is often stated in the literature. A full-scale SN simulation
using a Boltzmann solver and including all relevant neutrino reactions confirms
these results. The flavor-dependent flux differences are largest during the
initial accretion phase.Comment: Proceedings NOON 03, Kanazawa, 10-14 Feb 200
XMM-Newton observation of the ULIRG NGC 6240: The physical nature of the complex Fe K line emission
We report on an XMM-Newton observation of the ultraluminous infrared galaxy
NGC 6240. The 0.3-10 keV spectrum can be successfully modelled with: (i) three
collisionally ionized plasma components with temperatures of about 0.7, 1.4,
and 5.5 keV; (ii) a highly absorbed direct power-law component; and (iii) a
neutral Fe K_alpha and K_beta line. We detect a significant neutral column
density gradient which is correlated with the temperature of the three plasma
components. Combining the XMM-Newton spectral model with the high spatial
resolution Chandra image we find that the temperatures and the column densities
increase towards the center.
With high significance, the Fe K line complex is resolved into three distinct
narrow lines: (i) the neutral Fe K_alpha line at 6.4 keV; (ii) an ionized line
at about 6.7 keV; and (iii) a higher ionized line at 7.0 keV (a blend of the Fe
XXVI and the Fe K_beta line). While the neutral Fe K line is most probably due
to reflection from optically thick material, the Fe XXV and Fe XXVI emission
arises from the highest temperature ionized plasma component.
We have compared the plasma parameters of the ultraluminous infrared galaxy
NGC 6240 with those found in the local starburst galaxy NGC 253. We find a
striking similarity in the plasma temperatures and column density gradients,
suggesting a similar underlying physical process at work in both galaxies.Comment: 8 pages including 9 figures. Accepted for publication in A&
XMM-Newton discovery of a sharp spectral feature at ~7 keV in the Narrow-Line Seyfert 1 galaxy 1H 0707-495
We report the first detection of a sharp spectral feature in a Narrow-Line
Seyfert 1 galaxy. Using XMM-Newton we have observed 1H0707-495 and find a drop
in flux by a factor of more than 2 at a rest-frame energy of ~7 keV without any
detectable narrow Fe K alpha line emission. The energy of this feature suggests
a connection with the neutral iron K photoelectric edge, but the lack of any
obvious absorption in the spectrum at lower energies makes the interpretation
challenging. We explore two alternative explanations for this unusual spectral
feature: (i) partial covering absorption by clouds of neutral material and (ii)
ionised disc reflection with lines and edges from different ionisation stages
of iron blurred together by relativistic effects. We note that both models
require an iron overabundance to explain the depth of the feature. The X-ray
light curve shows strong and rapid variability, changing by a factor of four
during the observation. The source displays modest spectral variability which
is uncorrelated with flux.Comment: 5 pages incl. 6 figures, accepted for publication in MNRA
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