964 research outputs found
XMM-Newton observations of Nova Sgr 1998
We report on X-ray observations of Nova Sagittarius 1998 (V4633 Sgr),
performed with XMM-Newton at three different epochs, 934, 1083 and 1265 days
after discovery. The nova was detected with the EPIC cameras at all three
epochs, with emission spanning the whole energy range from 0.2 to 10 keV.
The X-ray spectra do not change significantly at the different epochs, and
are well fitted for the first and third observations with a multi-temperature
optically thin thermal plasma, while lower statistics in the second
observations lead to a poorer fit. The thermal plasma emission is most probably
originated in the shock heated ejecta, with chemical composition similar to
that of a CO nova. However, we can not completely rule out reestablished
accretion as the origin of the emission. We also obtain upper limits for the
temperature and luminosity of a potential white dwarf atmospheric component,
and conclude that hydrogen burning had already turned-off by the time of our
observations.Comment: 18 pages, 3 figures. Accepted in Astrophysical Journa
Mechanisms in endocrinology: Metabolic syndrome through the female life cycle
The normal function of the female reproductive system is closely linked to energy homeostasis with the ultimate scope of fertility and human race perpetuation through the centuries. During a woman's lifetime there are normal events such as puberty, pregnancy and menopause which are related to alterations in energy homeostasis and gonadal steroids levels followed by increase of body fat and insulin resistance, important components of metabolic syndrome (MetS). Pathological conditions such as premature adrenarche, polycystic ovary syndrome and gestational diabetes also present with shifts in gonadal steroid levels and reduced insulin sensitivity. The aim of this review is to discuss these conditions, both normal and pathological, analyzing the changes or abnormalities in ovarian function that coexist with metabolic abnormalities which resemble MetS in relationship with environmental, genetic and epigenetic factors
The supersoft X-ray source in V5116 Sgr I. The high resolution spectra
Classical novae occur on the surface of an accreting white dwarf in a binary
system. After ejection of a fraction of the envelope and when the expanding
shell becomes optically thin to X-rays, a bright source of supersoft X-rays
arises, powered by residual H burning on the surface of the white dwarf. While
the general picture of the nova event is well established, the details and
balance of accretion and ejection processes in classical novae are still full
of unknowns. The long-term balance of accreted matter is of special interest
for massive accreting white dwarfs, which may be promising supernova Ia
progenitor candidates. V5116 Sgr was observed as a bright and variable
supersoft X-ray source by XMM-Newton 610~days after outburst. The light curve
showed a periodicity consistent with the orbital period. During one third of
the orbit the luminosity was a factor of seven brighter than during the other
two thirds of the orbital period. In the present work we aim to disentangle the
X-ray spectral components of V5116 Sgr and their variability. We present the
high resolution spectra obtained with XMM-Newton RGS and Chandra LETGS/HRC-S in
March and August 2007. The grating spectrum during the periods of high-flux
shows a typical hot white dwarf atmosphere dominated by absorption lines of N
VI and N VII. During the low-flux periods, the spectrum is dominated by an
atmosphere with the same temperature as during the high-flux period, but with
several emission features superimposed. Some of the emission lines are well
modeled with an optically thin plasma in collisional equilibrium, rich in C and
N, which also explains some excess in the spectra of the high-flux period. No
velocity shifts are observed in the absorption lines, with an upper limit set
by the spectral resolution of 500 km/s, consistent with the expectation of a
non-expanding atmosphere so late in the evolution of the post-nova.Comment: 12 pages, 15 figures, 4 tables; accepted for publication in Astronomy
and Astrophysic
Measurements and optimization of the light yield of a TeO crystal
Bolometers have proven to be good instruments to search for rare processes
because of their excellent energy resolution and their extremely low intrinsic
background. In this kind of detectors, the capability of discriminating alpha
particles from electrons represents an important aspect for the background
reduction. One possibility for obtaining such a discrimination is provided by
the detection of the Cherenkov light which, at the low energies of the natural
radioactivity, is only emitted by electrons. This paper describes the method
developed to evaluate the amount of light produced by a crystal of TeO when
hit by a 511 keV photon. The experimental measurements and the results of a
detailed simulation of the crystal and the readout system are shown and
compared. A light yield of about 52 Cherenkov photons per deposited MeV was
measured. The effect of wrapping the crystal with a PTFE layer, with the aim of
maximizing the light collection, is also presented
X-ray and UV emission from the recurrent nova RS Ophiuchi in quiescence: Signatures of accretion and shocked gas
RS Ophiuchi is a recurrent nova system that experiences outbursts every ~20
years, implying accretion at a high rate onto a massive white dwarf. However,
previous X-ray observations of the system in quiescence have detected only
faint emission that is difficult to reconcile with the high accretion rate
predicted by nova theory for such frequent outbursts. Here, we use new Chandra
and XMM-Newton observations obtained 537 and 744 days after the 2006 outburst
to constrain both the accretion rate onto the white dwarf and the properties of
the nova ejecta at these times. We detect low level UV variability with the
XMM-Newton Optical Monitor on day 744 that is consistent with accretion disk
flickering, and use this to place a lower limit on the accretion rate. The
X-ray spectra in both observations are well described by a two component
thermal plasma model. The first component originates in the nova shell, which
can emit X-rays for up to a decade after the outburst. The other component
likely arises in the accretion disk boundary layer, and can be equally well fit
by a single temperature plasma or a cooling flow model. Although the flux of
the single temperature model implies an accretion rate that is 40 times lower
than theoretical predictions for RS Oph, the best fit cooling flow model
implies Mdot < 1.2x10^-8 M_sol/yr 537 days after the outburst, which is within
a factor of 2 of the theoretical accretion rate required to power an outburst
every 20 years. Furthermore, we place an upper limit on the accretion rate
through an optically thick region of the boundary layer of 2.0x10^-8 M_sol/yr.
Thus, the X-ray emission in quiescence is consistent with the accretion rate
expectations of nova theory. Finally, we discuss the possible origins of the
low temperature associated with the accretion component, which is a factor of
10 lower than in T CrB, an otherwise similar recurrent nova.Comment: 16 pages, 6 figures, accepted for publication in Ap
Recent discoveries of supersoft X-ray sources in M 31
Classical novae (CNe) have recently been reported to represent the major
class of supersoft X-ray sources (SSSs) in the central area of our neighbouring
galaxy M 31. This paper presents a review of results from recent X-ray
observations of M 31 with XMM-Newton and Chandra. We carried out a dedicated
optical and X-ray monitoring program of CNe and SSSs in the central area of M
31. We discovered the first SSSs in M 31 globular clusters (GCs) and their
connection to the very first discovered CN in a M 31 GC. This result may have
an impact on the CN rate in GCs. Furthermore, in our optical and X-ray
monitoring data we discovered the CN M31N 2007-11a, which shows a very short
SSS phase of 29 - 52 days. Short SSS states (durations < 100 days) of CNe
indicate massive white dwarfs (WDs) that are candidate progenitors of
supernovae type Ia. In the case of M31N 2007-11a, the optical and X-ray light
curves suggest a binary containing a WD with M_WD > 1.0 M_sun. Finally, we
present the discovery of the SSS counterpart of the CN M31N 2006-04a. The X-ray
light curve of M31N 2006-04a shows short-time variability, which might indicate
an orbital period of about 2 hours.Comment: 4 pages, 1 figure; Proc. of workshop "Supersoft X-ray Sources - New
Developments", ESAC, May 2009; accepted for publication in Astronomische
Nachrichte
TeO bolometers with Cherenkov signal tagging: towards next-generation neutrinoless double beta decay experiments
CUORE, an array of 988 TeO bolometers, is about to be one of the most
sensitive experiments searching for neutrinoless double-beta decay. Its
sensitivity could be further improved by removing the background from
radioactivity. A few years ago it has been pointed out that the signal from
s can be tagged by detecting the emitted Cherenkov light, which is not
produced by s. In this paper we confirm this possibility. For the first
time we measured the Cherenkov light emitted by a CUORE crystal, and found it
to be 100 eV at the -value of the decay. To completely reject the
background, we compute that one needs light detectors with baseline noise below
20 eV RMS, a value which is 3-4 times smaller than the average noise of the
bolometric light detectors we are using. We point out that an improved light
detector technology must be developed to obtain TeO bolometric experiments
able to probe the inverted hierarchy of neutrino masses.Comment: 5 pages, 4 figures. Added referee correction
New experimental limits on the alpha decays of lead isotopes
For the first time a PbWO4 crystal was grown using ancient Roman lead and it
was run as a cryogenic detector. Thanks to the simultaneous and independent
read-out of heat and scintillation light, the detector was able to discriminate
beta/gamma interactions with respect to alpha particles down to low energies.
New more stringent limits on the alpha decays of the lead isotopes are
presented. In particular a limit of T_{1/2} > 1.4*10^20 y at a 90% C.L. was
evaluated for the alpha decay of 204Pb to 200Hg
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