28 research outputs found
Evidence for Resonance Line Scattering in the Suzaku X-ray Spectrum of the Cygnus Loop
We present an analysis of the Suzaku observation of the northeastern rim of
the Cygnus Loop supernova remnant. The high detection efficiency together with
the high spectral resolution of the Suzaku X-ray CCD camera enables us to
detect highly-ionized C and N emission lines from the Cygnus Loop. Given the
significant plasma structure within the Suzaku field of view, we selected the
softest region based on ROSAT observations. The Suzaku spectral data are well
characterized by a two-component non-equilibrium ionization model with
different best-fit values for both the electron temperature and ionization
timescale. Abundances of C to Fe are all depleted to typically 0.23 times solar
with the exception of O. The abundance of O is relatively depleted by an
additional factor of two compared with other heavy elements. We found that the
resonance-line-scattering optical depth for the intense resonance lines of O is
significant and, whereas the optical depth for other resonance lines is not as
significant, it still needs to be taken into account for accurate abundance
determination.Comment: 10 pages, 5 figures. accepted for Publications of the Astronomical
Society of Japa
Core Structure of Intracluster Gas: Isothermal Hydrostatic Equilibrium
We investigate core structures of X-ray emitting intracluster gas based on
the so-called beta-model, which is an isothermal hydrostatic model often used
in observational studies. We reconsider the beta-model and find that the virial
temperature T_vir of a cluster may be represented better by beta T_X than T_X,
where beta is the parameter obtained from the X-ray surface brightness and T_X
is the emission-weighted mean temperature of the gas. We investigate 121
clusters observed by ROSAT and ASCA and find that the luminosity-temperature
relation L_X - beta T_X is less steep than L_X - T_X. We classify the clusters
into two core-size groups in order to investigate their properties in detail.
While in the larger core group the core radius is marginally proportional to
the virial radius, no significant relation is found for the smaller core group.
This may suggest that the smaller cores reflect the presence of cD galaxies,
effect of radiative cooling or asymmetry in the surface brightness. We examine
such possibilities, and find that the clusters of smaller cores have shorter
cooling time than the Hubble time, while no significant correlation is found
with cD or asymmetry. We carry out hydrodynamical calculations to simulate the
beta-model, intending to see the behavior of the isothermal gas under the
gravitational potential including the dark matter and galaxies with or without
a central cD galaxy. Calculations show r_c \propto r_vir and T_vir \simeq beta
T consistently with our consideration to the beta-model. Also is found from
calculations that the presence of a large cD galaxy may form a gas core \sim 40
kpc, which seems too small to account for the range of the core sizes, 40--80
kpc, of the smaller core group.Comment: 9 pages, 10 figures; To be published in PASJ vol 57, No. 3 (June
2005
Evolution of Supernova Remnants Expanding out of the Dense Circumstellar Matter into the Rarefied Interstellar Medium
We carry out 3D-hydrodynamical calculations for the interaction of expanding
supernova ejecta with the dense circumstellar matter (CSM) and the rarefied
interstellar medium (ISM) outside. The CSM is composed of the stellar wind
matter from the progenitor in its pre-supernova phase, and assumed to be
axially symmetric: more matter around the equator than in the polar direction
driven by rotation of the progenitor. Because of high density of the CSM, the
ionization state of the shock-heated ejecta quickly becomes equilibrium with
the electron temperature. When the blast wave breaks out of the CSM into the
rarefied ISM, the shocked ejecta cools rapidly due to adiabatic expansion, and
hence an over-ionized/recombining plasma would be left. The ejecta is reheated
by the second reverse shock due to the interaction with the ISM. We calculate
the emission measure of the supernova remnant (SNR) along the line of sight,
and find that the over-ionized plasma appears to be bar-like with wings in the
edge-on (equatorial view), while shell-like in the face-on (polar view)
geometry with respect to the rotation axis. The hot gas heated by the blast
wave exists in the outermost region of the SNR with a nearly complete shell,
but the X-rays therefrom are too faint to be observable. Thus, depending on the
viewing angle, the SNR of the over-ionized plasma would exhibit center-filled
morphology in X-rays, like W49B, a mixed-morphology SNR. The bar-like structure
is swept out by the second reverse shock and disappears eventually, and then
the SNR becomes shell-like in both the equatorial and polar views in the later
phase of the evolution.Comment: 8 pages, 9 figures, accepted for publication in PAS
X-Ray Spectrum of a Peculiar Supernova Remnant G359.1-0.5
We present the Suzaku results of a supernova remnant (SNR), G359.1-0.5 in the
direction of the Galactic center region. From the SNR, we find prominent
K-shell lines of highly ionized Si and S ions, together with unusual structures
at 2.5-3.0 and 3.1-3.6 keV. No canonical SNR plasma model, in either ionization
equilibrium or under-ionization, can explain the structures. The energies and
shapes of the structures are similar to those of the radiative transitions of
free electrons to the K-shell of He-like Si and S ions (radiative recombination
continuum: RRC). The presence of the strong RRC structures indicates that the
plasma is in over-ionization. In fact, the observed spectrum is well fitted
with an over-ionized plasma model. The best-fit electron temperature of 0.29
keV is far smaller than the ionization temperature of 0.77 keV, which means
that G359.1-0.5 is in extreme condition of over-ionization. We report some
cautions on the physical parameters, and comment possible origins for the
over-ionized plasma.Comment: 7 pages, 5 figures, accepted for publication in PAS
Discovery of Enhanced Radiative Recombination Continua of He-like Iron and Calcium from IC 443 and Its Implications
We present deep observations of the Galactic supernova remnant IC 443 with
the {\it Suzaku X-ray satellite}. We find prominent K-shell lines from iron and
nickel, together with a triangle residual at 8--10~keV, which corresponds to
the energy of the radiative recombination continuum (RRC) of He-like iron. In
addition, the wavy residuals have been seen at 5.1 and 5.5~keV. We
confirm that the residuals show the first enhanced RRCs of He- and H-like
calcium found in supernova remnants. These facts provide robust evidence for
the recombining plasma. We reproduce the plasma in the 3.7--10~keV band using a
recombining plasma model at the electron temperature 0.65~keV. The
recombination parameter ( is electron density and
is elapsed time after formation of a recombining plasma) and abundances of iron
and nickel are strongly correlated, and hence the errors are large. On the
other hand, the ratio of nickel to iron relative to the solar abundances is
well constrained to 11 (1). A possibility is that the large
abundance ratio is a result of an asymmetric explosion of the progenitor star.Comment: 4 pages, 5 figures, published in Ap
Non-Equilibrium Ionization States of GRB Environments
Iron spectral features are thought to be the best tracer of a progenitor of
gamma-ray bursts (GRBs). The detections of spectral features such as an iron
line and/or a Radiative Recombination edge and Continuum (RRC) were reported in
four X-ray afterglows of GRBs. However their properties were different each
other burst by burst. For example, Chandra observation of GRB 991216 reported
both the strong H-like iron line together with its RRC. On the contrary,
Yoshida et al. (2001) report only a detection of the strong RRC in GRB 970828
with ASCA. Since it is difficult to produce the strong RRC, we have to consider
special condition for the line and/or the RRC forming region. In this paper, we
point out a possibility of a ``non-equilibrium ionization state'' for the line
and the RRC forming region.Comment: 10pages, 2figures. Accepted for ApJL. This is a companion paper by
A.Yoshida et. a
L_X-T Relation and Related Properties of Galaxy Clusters
An observational approach is presented to constrain the global structure and
evolution of the intracluster medium based on the ROSAT and ASCA distant
cluster sample. From statistical analysis of the gas density profile and the
connection to the LX-T relation under the beta-model, the scaled gas profile is
nearly universal for the outer region and the LX(>0.2r500) is tightly related
to the temperature through T^3 rather than T^2. On the other hand, a large
density scatter exists in the core region and there is clearly a deviation from
the self-similar scaling for clusters with a small core size. A direct link
between the core size and the radiative cooling timescale suggest that t_cool
is a parameter to control the gas structure and the appearance of small cores
in regular clusters may be much connected with the thermal evolution. We derive
the luminosity-ambient temperature (T') relation, assuming the universal
temperature profile to find the dispersion around the relation significantly
decreases: L_1keV is almost constant for a wide range of t_cool. We further
examined the LX-Tbeta and LX-T'beta relations and showed a trend that merging
clusters segregate from the regular clusters on the planes. A good correlation
between t_cool and the X-ray morphology on the L_1keV-t_cool/t_age plane leads
us to define three phases according to the different level of cooling, and draw
a phenomenological picture: after a cluster collapses and t_cool falls below
t_age, the core cools radiatively with quasi-hydrostatic balancing in the
gravitational potential, and the central density gradually becomes higher to
evolve from an outer-core-dominant cluster to inner-core-dominant cluster.Comment: 39 pages, 37 figures. Accepted for publication in ApJ. Version with
high-quality color figures at
http://cosmic.riken.jp/ota/publications/index.htm