499 research outputs found
Once Bitten, Twice Shy: The Supreme Court’s Misguided Doubling Down on the Dual Sovereigns Exception to the Fifth Amendment’s Double Jeopardy Clause
Iron K-alpha Emission from X-ray Reflection: Predictions for Gamma-Ray Burst Models
Recent observations of several gamma-ray burst (GRB) afterglows have shown
evidence for a large amount of X-ray line emitting material, possibly arising
from ionized iron. A significant detection of an X-ray spectral feature, such
as that found in the Chandra observation of GRB 991216, may provide important
constraints on the immediate environment of the burst and hence on progenitor
models. The large Fe K-alpha equivalent widths inferred from the X-ray
observations favor models in which the line is produced when the primary X-ray
emission from the source strikes Thomson-thick material and Compton scatters
into our line of sight. We present such reflection spectra here, computed in a
fully self-consistent manner, and discuss the range of ionization parameters
that may be relevant to different models of GRBs. We argue that the presence of
a strong hydrogen-like K-alpha line is unlikely, because Fe-XXVI photons would
be trapped resonantly and removed from the line core by Compton scattering. In
contrast, a strong narrow emission line from He-like Fe-XXV is prominent in the
model spectra. We briefly discuss how these constraints may affect the line
energy determination in GRB 991216.Comment: 8 pages, 3 figures, Ap.J. Letters accepte
Fe K\alpha emission from photoionized slabs: the impact of the iron abundance
Iron K\alpha emission from photoionized and optically thick material is
observed in a variety of astrophysical environments including X-ray binaries,
active galactic nuclei, and possibly gamma-ray bursts. This paper presents
calculations showing how the equivalent width (EW) of the Fe K line depends on
the iron abundance of the illuminated gas and its ionization state -- two
variables subject to significant cosmic scatter. Reflection spectra from a
constant density slab which is illuminated with a power-law spectrum with
photon-index \Gamma are computed using the code of Ross & Fabian. When the Fe K
EW is measured from the reflection spectra alone, we find that it can reach
values greater than 6 keV if the Fe abundance is about 10 times solar and the
illuminated gas is neutral. EWs of about 1 keV are obtained when the gas is
ionized. In contrast, when the EW is measured from the incident+reflected
spectrum, the largest EWs are ~800 keV and are found when the gas is ionized.
When \Gamma is increased, the Fe K line generally weakens, but significant
emission can persist to larger ionization parameters. The iron abundance has
its greatest impact on the EW when it is less than 5 times solar. When the
abundance is further increased, the line strengthens only marginally.
Therefore, we conclude that Fe K lines with EWs much greater than 800 eV are
unlikely to be produced by gas with a supersolar Fe abundance. These results
should be useful in interpreting Fe K emission whenever it arises from
optically thick fluorescence.Comment: 5 pages, 5 figures, accepted by MNRAS Letter
The response of the Fe K\alpha line to changes in the X-ray illumination of accretion discs
X-ray reflection spectra from photoionized accretion discs in active galaxies
are presented for a wide range of illumination conditions. The energy,
equivalent width (EW) and flux of the Fe K line are shown to depend strongly on
the ratio of illuminating flux to disc flux, Fx/Fdisc, the photon index of the
irradiating power-law, \Gamma, and the incidence angle of the radiation, i.
When Fx/Fdisc \leq 2 a neutral Fe K line is prominent for all but the largest
values of \Gamma. At higher illuminating fluxes a He-like Fe K line at 6.7 keV
dominates the line complex. With a high-energy cutoff of 100 keV, the thermal
ionization instability seems to suppress the ionized Fe K line when \Gamma \leq
1.6. The Fe K line flux correlates with Fx/Fdisc, but the dependence weakens as
iron becomes fully ionized. The EW is roughly constant when Fx/Fdisc is low and
a neutral line dominates, but then declines as the line progresses through
higher ionization stages. There is a strong positive correlation between the Fe
K EW and \Gamma when the line energy is at 6.7 keV, and a slight negative one
when it is at 6.4 keV. This is a potential observational diagnostic of the
ionization state of the disc. Observations of the broad Fe K line which take
into account any narrow component would be able to test these predictions.
Ionized Fe K lines at 6.7 keV are predicted to be common in a simple magnetic
flare geometry. A model which includes multiple ionization gradients on the
disc is postulated to reconcile the results with observations.Comment: 11 pages, 10 figures. Fig. 10 on page 9 in colour. Accepted by MNRA
X-ray Reflection By Photoionized Accretion Discs
We present the results of reflection calculations that treat the relevant
physics with a minimum of assumptions. The temperature and ionization structure
of the top five Thomson depths of an illuminated disc are calculated while also
demanding that the atmosphere is in hydrostatic equilibrium. In agreement with
Nayakshin, Kazanas & Kallman, we find that there is a rapid transition from hot
to cold material in the illuminated layer. However, the transition is usually
not sharp so that often we find a small but finite region in Thomson depth
where there is a stable temperature zone at T \sim 2 x 10^{6} K due to
photoelectric heating from recombining ions. As a result, the reflection
spectra often exhibit strong features from partially-ionized material,
including helium-like Fe K lines and edges. We find that due to the highly
ionized features in the spectra these models have difficulty correctly
parameterizing the new reflection spectra. There is evidence for a spurious
correlation in the ASCA energy range, where is the reflection
fraction for a power-law continuum of index , confirming the suggestion
of Done & Nayakshin that at least part of the R-Gamma correlation reported by
Zdziarski, Lubinski & Smith for Seyfert galaxies and X-ray binaries might be
due to ionization effects. Although many of the reflection spectra show strong
ionized features, these are not typically observed in most Seyfert and quasar
X-ray spectra.Comment: 16 pages, accepted by MNRAS, Fig. 8 is in colour Figures and tables
changed by a code update. Conclusions unchange
X-ray Reflection from Inhomogeneous Accretion Disks: II. Emission Line Variability and Implications for Reverberation Mapping
One of the principal scientific objectives of the upcoming Constellation-X
mission is to attempt to map the inner regions of accretion disks around black
holes in Seyfert galaxies by reverberation mapping of the Fe K fluorescence
line. This area of the disk is likely radiation pressure dominated and subject
to various dynamical instabilities. Here, we show that density inhomogeneities
in the disk atmosphere resulting from the photon bubble instability (PBI) can
cause rapid changes in the X-ray reflection features, even when the
illuminating flux is constant. Using a simulation of the development of the
PBI, we find that, for the disk parameters chosen, the Fe K and O VIII Ly\alpha
lines vary on timescales as short as a few hundredths of an orbital time. In
response to the changes in accretion disk structure, the Fe K equivalent width
(EW) shows variations as large as ~100 eV. The magnitude and direction
(positive or negative) of the changes depends on the ionization state of the
atmosphere. The largest changes are found when the disk is moderately ionized.
The O VIII EW varies by tens of eV, as well as exhibiting plenty of rapid,
low-amplitude changes. This effect provides a natural explanation for some
observed instances of short timescale Fe K variability which was uncorrelated
with the continuum (e.g., Mrk 841). New predictions for Fe K reverberation
mapping should be made which include the effects of this accretion disk driven
line variability and a variable ionization state. Reflection spectra averaged
over the evolution of the instability are well fit by constant density models
in the 2-10 keV region.Comment: 20 pages, 3 figures. Accepted by Ap
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