1,386 research outputs found
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Hereditariness, strongness and relationship between Brown-McCoy and Behrens radicals
In this paper we explore the properties of being hereditary and being strong among the radicals of associative rings, and prove certain results such as a relationship between Brown-McCoy and Behrens radicals
The Corrected Log N-Log Fluence Distribution of Cosmological Gamma-Ray Bursts
Recent analysis of relativistically expanding shells of cosmological
gamma-ray bursts has shown that if the bursts are cosmological, then most
likely total energy (E_0) is standard and not peak luminosity (L_0). Assuming a
flat Friedmann cosmology (q_o = 1/2, Lambda = 0) and constant rate density
(rho_0) of bursting sources, we fit a standard candle energy to a uniformly
selected log N-log S in the BATSE 3B catalog correcting for fluence efficiency
and averaging over 48 observed spectral shapes. We find the data consistent
with E_0 = 7.3^{+0.7}_{-1.0} X 10^{51} ergs and discuss implications of this
energy for cosmological models of gamma-ray bursts.Comment: A five page LateX file that uses the Revtex conference proceedings
macro aipbook.sty, and includes three postscript figures using psfig. To Be
published in the Proceedings of the Third Hunstville Symposium on Gamma-Ray
Bursts, eds. C. Kouveliotou, M.S. Briggs and G.J. Fishman (New York:AIP).
Postscript version availible at http://nis-www.lanl.gov/~jsbloom/LOG_S.p
A closer look at the X-ray transient XTE J1908+094: identification of two new near-infrared candidate counterparts
We had reported in Chaty, Mignani, Israel (2002) on the near-infrared (NIR)
identification of a possible counterpart to the black hole candidate XTE
J1908+094 obtained with the ESO/NTT. Here, we present new, follow-up, CFHT
adaptive optics observations of the XTE J1908+094 field, which resolved the
previously proposed counterpart in two objects separated by about 0.8".
Assuming that both objects are potential candidate counterparts, we derive that
the binary system is a low-mass system with a companion star which could be
either an intermediate/late type (A-K) main sequence star at a distance of 3-10
kpc, or a late-type (K) main sequence star at a distance of 1-3 kpc.
However, we show that the brighter of the two objects (J ~ 20.1, H ~ 18.7, K' ~
17.8) is more likely to be the real counterpart of the X-ray source. Its
position is more compatible with our astrometric solution, and colours and
magnitudes of the other object are not consistent with the lower limit of 3 kpc
derived independently from the peak bolometric flux of XTE J1908+094. Further
multi-wavelength observations of both candidate counterparts are crucial in
order to solve the pending identification.Comment: accepted for publication in MNRAS, 5 pages, 3 figure
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Nitrite formulations and their use as nitric oxide prodrugs
Compositions comprising from about 40 weight parts to about 1000 weight parts of a botanical nitrate source; from about 20 weight parts to about 500 weight parts of a botanical source of nitrite reduction activity; and from about 4 weight parts to about 100 weight parts of a nitrite salt. Use of the composition in methods of reducing triglycerides or reducing C-reactive protein levels are also provided.Board of Regents, University of Texas Syste
Unveiling the environment surrounding LMXB SAX J1808.4-3658
Low-mass X-ray binaries (LMXBs) are a natural workbench to study accretion
disk phenomena and optimal background sources to measure elemental abundances
in the Interstellar medium (ISM). In high-resolution XMM-Newton spectra, the
LMXB SAX J1808.4-3658 showed in the past a neon column density significantly
higher than expected given its small distance, presumably due to additional
absorption from a neon-rich circumstellar medium (CSM). It is possible to
detect intrinsic absorption from the CSM by evidence of Keplerian motions or
outflows. For this purpose, we use a recent, deep (100 ks long),
high-resolution Chandra/LETGS spectrum of SAX J1808.4-3658 in combination with
archival data. We estimated the column densities of the different absorbers
through the study of their absorption lines. We used both empirical and
physical models involving photo- and collisional-ionization in order to
determine the nature of the absorbers. The abundances of the cold interstellar
gas match the solar values as expected given the proximity of the X-ray source.
For the first time in this source, we detected neon and oxygen blueshifted
absorption lines that can be well modeled with outflowing photoionized gas. The
wind is neon rich (Ne/O>3) and may originate from processed, ionized gas near
the accretion disk or its corona. The kinematics (v=500-1000 km/s) are indeed
similar to those seen in other accretion disks. We also discovered a system of
emission lines with very high Doppler velocities (v~24000 km/s) originating
presumably closer to the compact object. Additional observations and UV
coverage are needed to accurately determine the wind abundances and its
ionization structure.Comment: 12 pages, 10 figures, accepted for publication on A&
IGR J17254-3257, a new bursting neutron star
The study of the observational properties of uncommonly long bursts from low
luminosity sources with extended decay times up to several tens of minutes is
important when investigating the transition from a hydrogen-rich bursting
regime to a pure helium regime and from helium burning to carbon burning as
predicted by current burst theories. IGR J17254-3257 is a recently discovered
X-ray burster of which only two bursts have been recorded: an ordinary short
type I X-ray burst, and a 15 min long burst. An upper limit to its distance is
estimated to about 14.5 kpc. The broad-band spectrum of the persistent emission
in the 0.3-100 keV energy band obtained using contemporaneous INTEGRAL and
XMM-Newton data indicates a bolometric flux of 1.1x10^-10 erg/cm2/s
corresponding, at the canonical distance of 8 kpc, to a luminosity about
8.4x10^35 erg/s between 0.1-100 keV, which translates to a mean accretion rate
of about 7x10^-11 solar masses per year. The low X-ray persistent luminosity of
IGR J17254-3257 seems to indicate the source may be in a state of low accretion
rate usually associated with a hard spectrum in the X-ray range. The nuclear
burning regime may be intermediate between pure He and mixed H/He burning. The
long burst is the result of the accumulation of a thick He layer, while the
short one is a prematurate H-triggered He burning burst at a slightly lower
accretion rate.Comment: 4 pages, 4 figures, 1 table; accepted for publication in A&A Letters.
1 reference (Cooper & Narayan, 2007) correcte
Discovery of an eccentric 30 days period in the supergiant X-ray binary SAX J1818.6-1703 with INTEGRAL
SAX J1818.6-1703 is a flaring transient X-ray source serendipitously
discovered by BeppoSAX in 1998 during an observation of the Galactic centre.
The source was identified as a High-Mass X-ray Binary with an OB SuperGiant
companion. Displaying short and bright flares and an unusually very-low
quiescent level implying intensity dynamical range as large as 1e3-4, the
source was classified as a Supergiant Fast X-ray Transient. The mechanism
triggering the different temporal behaviour observed between the classical
SGXBs and the recently discovered class of SFXTs is still debated. The
discovery of long orbits (>15 d) should help to discriminate between emission
models and bring constraints.
We analysed archival INTEGRAL data on SAX J1818.6-1703. We built short- and
long-term light curves and performed timing analysis in order to study the
temporal behaviour of SAX J1818.6-1703 on different time scales. INTEGRAL
revealed an unusually long orbital period of 30.0+/-0.2 d and an elapsed
accretion phase of ~6 d in the transient SGXB SAX J1818.6-1703. This implies an
elliptical orbit and constraints the possible supergiant spectral type between
B0.5-1I with eccentricities e~0.3-0.4 (for average fundamental parameters of
supergiant stars). During the accretion phase, the source behaved like
classical SGXBs. The huge variations of the observed X-ray flux can be
explained through accretion of macro-clumps formed within the stellar wind. Our
analysis strengthens the model which predicts that SFXTs behave as SGXBs but
with different orbital parameters, thus different temporal behaviour.Comment: 4 pages, 3 figures, A&A Letter in press (subm. 17/10/2008 - accept.
15/11/2008
An age-dependent branching process model for the analysis of CFSE-labeling experiments
<p>Abstract</p> <p>Background</p> <p>Over the past decade, flow cytometric CFSE-labeling experiments have gained considerable popularity among experimentalists, especially immunologists and hematologists, for studying the processes of cell proliferation and cell death. Several mathematical models have been presented in the literature to describe cell kinetics during these experiments.</p> <p>Results</p> <p>We propose a multi-type age-dependent branching process to model the temporal development of populations of cells subject to division and death during CFSE-labeling experiments. We discuss practical implementation of the proposed model; we investigate a competing risk version of the process; and we identify the classes of cellular dependencies that may influence the expectation of the process and those that do not. An application is presented where we study the proliferation of human CD8+ T lymphocytes using our model and a competing risk branching process.</p> <p>Conclusions</p> <p>The proposed model offers a widely applicable approach to the analysis of CFSE-labeling experiments. The model fitted very well our experimental data. It provided reasonable estimates of cell kinetics parameters as well as meaningful insights into the processes of cell division and cell death. In contrast, the competing risk branching process could not describe the kinetics of CD8+ T cells. This suggested that the decision of cell division or cell death may be made early in the cell cycle if not in preceding generations. Also, we show that analyses based on the proposed model are robust with respect to cross-sectional dependencies and to dependencies between fates of linearly filiated cells.</p> <p>Reviewers</p> <p>This article was reviewed by Marek Kimmel, Wai-Yuan Tan and Peter Olofsson.</p
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