15,638 research outputs found
X-ray outbursts of low-mass X-ray binary transients observed in the RXTE era
We have performed a statistical study of the properties of 110 bright X-ray
outbursts in 36 low-mass X-ray binary transients (LMXBTs) seen with the All-Sky
Monitor (2--12 keV) on board the {\it Rossi X-ray Timing Explorer} ({\it RXTE})
in 1996--2011. We have measured a number of outburst properties, including peak
X-ray luminosity, rate of change of luminosity on a daily timescale,
-folding rise and decay timescales, outburst duration, and total radiated
energy. We found that the average properties such as peak X-ray luminosity,
rise and decay timescales, outburst duration, and total radiated energy of
black hole LMXBTs, are at least two times larger than those of neutron star
LMXBTs, implying that the measurements of these properties may provide
preliminary clues as to the nature of the compact object of a newly discovered
LMXBT. We also found that the outburst peak X-ray luminosity is correlated with
the rate of change of X-ray luminosity in both the rise and the decay phases,
which is consistent with our previous studies. Positive correlations between
total radiated energy and peak X-ray luminosity, and between total radiated
energy and the -folding rise or decay timescale, are also found in the
outbursts. These correlations suggest that the mass stored in the disk before
an outburst is the primary initial condition that sets up the outburst
properties seen later. We also found that the outbursts of two transient
stellar-mass ULXs in M31 also roughly follow the correlations, which indicate
that the same outburst mechanism works for the brighter outbursts of these two
sources in M31 that reached the Eddington luminosity.Comment: Accepted to Ap
Note on neutron star equation of state in the light of GW170817
From the very first multimessenger event of GW170817, clean robust
constraints can be obtained for the tidal deformabilities of the two stars
involved in the merger, which provides us unique opportunity to study the
equation of states (EOSs) of dense stellar matter. In this contribution, we
employ a model from the quark level, describing consistently a nucleon and
many-body nucleonic system from a quark potential. We check that our sets of
EOSs are consistent with available experimental and observational constraints
at both sub-nuclear saturation densities and higher densities. The agreements
with ab-initio calculations are also good. Especially, we tune the density
dependence of the symmetry energy (characterized by its slope at nuclear
saturation ) and study its influence on the tidal deformability. The
so-called EOS is named after the case of , and it gives
and , for a
star. The tidal signals are demonstrated to be insensitive to
the uncertain crust-core matching, despite the good correlation between the
symmetry energy slope and the radius of the star.Comment: 8 pages, 6 figures, Submitted to the AIP Proceedings of the
Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era
of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, Chin
The analysis of the charmonium-like states ,, , and according to its strong decay behaviors
Inspired by the newly observed state , we analyze the strong
decay behaviors of some charmonium-like states ,,
, and by the model. We carry out our
work based on the hypothesis that these states are all being the charmonium
systems. Our analysis indicates that charmonium state can be a good
candidate for and state is the possible assignment for
. Considering as the state, the decay behavior of
is inconsistent with the experimental data. So, we can not assign
as the charmonium state by present work. Besides, our
analysis imply that it is reasonable to assign and to be
the same state, . However, combining our analysis with that of
Zhou~\cite{ZhouZY}, we speculate that / might not be a pure
systems
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