70 research outputs found
Attenuation of super-soft X-ray sources by circumstellar material
Recent studies have suggested the possibility of significantly obscuring
super-soft X-ray sources in relatively modest amounts of local matter lost from
the binaries themselves. If correct, then this would have explained the paucity
of observed super-soft X-ray sources and would have significance for the search
for single-degenerate type Ia supernova progenitors. We point out that earlier
studies of circumbinary obscuration ignored photo-ionisations of the gas by the
emission from the super-soft X-ray source. We revisit the problem using a full,
self-consistent calculation of the ionisation state of the circumbinary
material photo-ionised by the radiation of the central source. Our results show
that the circumstellar mass-loss rates required for obcuration of super-soft
X-ray sources is about an order of magnitude larger than those reported in
earlier studies, for comparable model parameters. While this does not entrirely
rule out the possibility of circumstellar material obscuring super-soft X-ray
sources, it makes it unlikely that this effect alone can account for the
majority of the missing super-soft X-ray sources. We discuss the observational
appearance of hypothetical obscured nuclear burning white dwarfs and show that
they have signatures making them distinct from photo-ionised nebulae around
super-soft X-ray sources imbedded in the low density ISM.Comment: MNRAS, accepted; 11 pages, 10 figures, 1 tabl
Progenitors of type Ia supernovae in elliptical galaxies
Although there is a nearly universal agreement that type Ia supernovae are
associated with the thermonuclear disruption of a CO white dwarf, the exact
nature of their progenitors is still unknown. The single degenerate scenario
envisages a white dwarf accreting matter from a non-degenerate companion in a
binary system. Nuclear energy of the accreted matter is released in the form of
electromagnetic radiation or gives rise to numerous classical nova explosions
prior to the supernova event. We show that combined X-ray output of supernova
progenitors and statistics of classical novae predicted in the single
degenerate scenario are inconsistent with X-ray and optical observations of
nearby early type galaxies and galaxy bulges. White dwarfs accreting from a
donor star in a binary system and detonating at the Chandrasekhar mass limit
can account for no more than ~5% of type Ia supernovae observed in old stellar
populations.Comment: To be published in Proceedings of "Astrophysics of neutron stars",
Cesme, 201
He II recombination lines as a test of the nature of SN Ia progenitors in elliptical galaxies
To date, the question of which progenitor channel can reproduce the observed
rate of Type Ia supernovae (SNe Ia) remains unresolved, with the single and
double degenerate scenarios remaining the leading contenders. The former
implies a large population of hot accreting white dwarfs with photospheric
temperatures of T ~ 10^5-10^6 K during some part of their accretion history. We
show that in early-type galaxies, a population of accreting white dwarfs large
enough to reproduce the SN Ia rate would contribute significantly to the
ionizing UV radiation expected from the stellar population. For mean stellar
ages < ~5 Gyr, single degenerate progenitors would dominate the ionizing
background produced by stars, increasing the continuum beyond the He
II-ionizing limit more than ten-fold. This opens a new avenue for constraining
the progenitors of SNe Ia, through consideration of the spatially extended
low-ionization emission-line regions now found in many early-type galaxies.
Modelling the expected emission, we show that one can constrain the
contribution of the single degenerate channel to the SN Ia rate in E/S0
galaxies from upper limits on the luminosity of He II recombination lines in
the optical and FUV. We discuss future directions, as well as possible
implications for the evolution of SNe Ia in old stellar populations.Comment: 12 pages, 13 figures, MNRA
X-ray diagnostics of chemical composition of the accretion disk and donor star in ultra-compact X-ray binaries
Non-solar composition of the donor star in ultra-compact X-ray binaries may
have a pronounced effect on the fluorescent lines appearing in their spectra
due to reprocessing of primary radiation by the accretion disk and the white
dwarf surface. We show that the most dramatic and easily observable consequence
of the anomalous C/O abundance, is the significant, by more than an order of
magnitude, attenuation of the Ka line of iron. It is caused by screening of the
presence of iron by oxygen - in the C/O dominated material the main interaction
process for a E ~ 7keV photon is absorption by oxygen rather than by iron,
contrary to the solar composition case. Ionization of oxygen at high mass
accretion rates adds a luminosity dependence to this behavior - the iron line
is significantly suppressed only at low luminosity, log(LX) less than 37-37.5,
and should recover its nominal strength at higher luminosity. The increase of
the EW of the Ka lines of carbon and oxygen, on the other hand, saturates at
rather moderate values. Screening by He is less important, due to its low
ionization threshold and because in the accretion disk it is mostly ionized.
Consequently, in the case of the He-rich donor, the iron line strength remains
close to its nominal value, determined by the iron abundance in the accretion
disk. This opens the possibility of constraining the nature of donor stars in
UCXBs by means of X-ray spectroscopy with moderate energy resolution.Comment: Accepted by MNRA
Is the lack of pulsations in low mass X-Ray binaries due to comptonizing coronae?
The spin periods of the neutron stars in most Low Mass X-ray Binary (LMXB) systems still remain undetected. One of the models to explain the absence of coherent pulsations has been the suppression of the beamed signal by Compton scattering of X-ray photons by electrons in a surrounding corona. We point out that simultaneously with wiping out the pulsation signal, such a corona will upscatter (pulsating or not) X-ray emission originating at and/or near the surface of the neutron star leading to appearance of a hard tail of Comptonized radiation in the source spectrum. We analyze the hard X-ray spectra of a selected set of LMXBs and demonstrate that the optical depth of the corona is not likely to be large enough to cause the pulsations to disappear
Can AGN and galaxy clusters explain the surface brightness fluctuations of the cosmic X-ray background?
Fluctuations of the surface brightness of cosmic X-ray background (CXB) carry
unique information about faint and low luminosity source populations, which is
inaccessible for conventional large-scale structure (LSS) studies based on
resolved sources. We used Chandra data of the XBOOTES field
() to conduct the most accurate measurement to date of
the power spectrum of fluctuations of the unresolved CXB on the angular scales
of arcsec arcmin. We find that at sub-arcmin angular
scales, the power spectrum is consistent with the AGN shot noise, without much
need for any significant contribution from their one-halo term. This is
consistent with the theoretical expectation that low-luminosity AGN reside
alone in their dark matter halos. However, at larger angular scales we detect a
significant LSS signal above the AGN shot noise. Its power spectrum, obtained
after subtracting the AGN shot noise, follows a power law with the slope of
and its amplitude is much larger than what can be plausibly
explained by the two-halo term of AGN. We demonstrate that the detected LSS
signal is produced by unresolved clusters and groups of galaxies. For the flux
limit of the XBOOTES survey, their flux-weighted mean redshift equals
\left\sim0.3, and the mean temperature of their intracluster medium
(ICM), \left\approx 1.4 keV, corresponds to the mass of . The power spectrum of CXB fluctuations
carries information about the redshift distribution of these objects and the
spatial structure of their ICM on the linear scales of up to Mpc, i.e. of
the order of the virial radius.Comment: 25 pages, 20 figures, submitted to MNRAS, comments welcom
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