19,968 research outputs found
Formation of the Double Neutron Star System PSR J19301852
The spin period (185 ms) and period derivative () of the double neutron star (DNS) system PSR J19301852 recently
discovered indicate that the pulsar was mildly recycled through the process of
Roche-lobe overflow. This system has the longest orbital period (45 days) of
the known DNS systems, and can be formed from a helium star-NS binary if the
initial mass of the helium star was ; otherwise the
helium star would never fill its Roche-lobe \citep{t15}. At the moment of the
supernova explosion, the mass of the helium star was .
We find that the probability distribution of the velocity kick imparted to the
new-born neutron star has a maximum at about (and a tail
up to ), indicating that this NS most probably received
a low kick velocity at birth.Comment: 9 pages, 4 figures, accepted for publication in Ap
On the formation of Be stars through binary interaction
Be stars are rapidly rotating B type stars. The origin of their rapid
rotation is not certain, but binary interaction remains to be a possibility. In
this work we investigate the formation of Be stars resulting from mass transfer
in binaries in the Galaxy. We calculate the binary evolution with both stars
evolving simultaneously and consider different possible mass accretion
histories for the accretor. From the calculated results we obtain the critical
mass ratios that determine the stability of mass transfer. We also
numerically calculate the parameter in common envelope evolution, and
then incorporate both and into the population synthesis
calculations. We present the predicted numbers and characteristics of Be stars
in binary systems with different types of companions, including helium stars,
white dwarfs, neutron stars, and black holes. We find that in Be/neutron star
binaries the Be stars can have a lower limit of mass if
they are formed by stable (i.e., without the occurrence of common envelope
evolution) and nonconservative mass transfer. We demonstrate that isolated Be
stars may originate from both mergers of two main-sequence stars and disrupted
Be binaries during the supernova explosions of the primary stars, but mergers
seem to play a much more important role. Finally the fraction of Be stars which
have involved binary interactions in all B type stars can be as high as , implying that most of Be stars may result from binary interaction.Comment: 38 pages, 14 figures, 1 table, accepted for publication in Ap
Formation and Evolution of Galactic Intermediate/Low-Mass X-ray Binaries
We investigate the formation and evolutionary sequences of Galactic
intermediate- and low-mass X-ray binaries (I/LMXBs) by combining binary
population synthesis (BPS) and detailed stellar evolutionary calculations.
Using an updated BPS code we compute the evolution of massive binaries that
leads to the formation of incipient I/LMXBs, and present their distribution in
the initial donor mass vs. initial orbital period diagram. We then follow the
evolution of I/LMXBs until the formation of binary millisecond pulsars (BMSPs).
We find that the birthrate of the I/LMXB population is in the range of , compatible with that of
BMSPs which are thought to descend from I/LMXBs. We show that during the
evolution of I/LMXBs they are likely to be observed as relatively compact
binaries with orbital periods 1 day and donor masses . The resultant BMSPs have orbital periods ranging from less than 1
day to a few hundred days. These features are consistent with observations of
LMXBs and BMSPs. We also confirm the discrepancies between theoretical
predications and observations mentioned in the literature, that is, the
theoretical average mass transfer rates (\,yr) of LMXBs are considerably lower than observed, and the number of
BMSPs with orbital periods day is severely underestimated. These
discrepancies imply that something is missing in the modeling of LMXBs, which
is likely to be related to the mechanisms of the orbital angular momentum loss.Comment: 30 pages, 13 figure
A Population of Ultraluminous X-ray Sources with An Accreting Neutron Star
Most ultraluminous X-ray sources (ULXs) are believed to be X-ray binary
systems, but previous observational and theoretical studies tend to prefer a
black hole rather than a neutron star accretor. The recent discovery of 1.37 s
pulsations from the ULX M82 X-2 has established its nature as a magnetized
neutron star. In this work we model the formation history of neutron star ULXs
in an M82- or Milky Way-like galaxy, by use of both binary population synthesis
and detailed binary evolution calculations. We find that the birthrate is
around for the incipient X-ray binaries in both cases.
We demonstrate the distribution of the ULX population in the donor mass -
orbital period plane. Our results suggest that, compared with black hole X-ray
binaries, neutron star X-ray binaries may significantly contribute to the ULX
population, and high-mass and intermediate-mass X-ray binaries dominate the
neutron star ULX population in M82- and Milky Way-like galaxies, respectively.Comment: 13 pages, 5 figures, accepted for publication in Ap
On the role of supernova kicks in the formation of Galactic double neutron star systems
In this work we focus on a group of Galactic double neutron star (DNS)
systems with long orbital periods of day and low eccentricities of
. The feature of these orbital parameters is used to constrain
the evolutionary processes of progenitor binaries and the supernova (SN) kicks
of the second born NSs. Adopting that the mass transfer during primordial
binary evolution is highly non-conservative (rotation-dependent), the formation
of DNS systems involves a double helium star binary phase, the common envelope
(CE) evolution initiates before the first NS formation. During the CE evolution
the binary orbital energy is obviously larger when using a helium star rather
than a NS to expel the donor envelope, this can help explain the formation of
DNS systems with long periods. SN kicks at NS birth can lead to eccentric
orbits and even the disruption of binary systems, the low eccentricities
require that the DNSs receive a small natal kick at the second collapse.
Compared with the overall distribution of orbital parameters for observed DNS
binaries, we propose that the second born NSs in most DNS systems are subject
to small natal kicks with the Maxwellian dispersion velocity of less than , which can provide some constraints on the SN explosion
processes. The mass distribution of DNS binaries is also briefly discussed. We
suggest that the rotation-dependent mass transfer mode and our results about SN
kicks should be applied to massive binary evolution and population synthesis
studies.Comment: 7 figures, 2 tables, accepted by Ap
Zitterbewegung at the level of quantum field theory
Traditionally, the zitterbewegung (ZB) of the Dirac electron has just been
studied at the level of quantum mechanics. Seeing that the fact that an old
interest in ZB has recently been rekindled by the investigations on spintronic,
graphene, and superconducting systems, etc., in this paper we present a
quantum-field-theory investigation on ZB and obtain the conclusion that, the ZB
of an electron arises from the influence of virtual electron-positron pairs (or
vacuum fluctuations) on the electron.Comment: 10 pages, no figure, to be published in Chinese Physic
Photons inside a waveguide as massive particles
In the paper, we show that there exists a close analogy between the behavior
of de Broglie matter waves and that of electromagnetic waves inside a hollow
waveguide, such that the guided photons can be treated as free massive
particles subject to a relativistic quantum-mechanical equation. Inspired by
the effective rest mass of guided photons and the zitterbewegung phenomenon of
the Dirac electron, at variance with the well-known Higgs mechanism we present
some different heuristic ideas on the origin of mass.Comment: 14 pages, no figur
Radiative decays of the neutral
We study the radiative decays of the in a hadronic molecule
picture, where the is treated as a hadronic
molecule. The partial widths of and
are predicted to be of order 10 keV
and the cross sections for and are of order 0.1 pb at 4.23 GeV, which may be accessible for the
BESIII and forthcoming BelleII.Comment: 8 pages, 11 figures, Phys.Rev.D versio
1-loop Corrections to the \rho Parameter in the Left-Right Twin Higgs Model
We implement a one-loop analysis of the parameter in the Left Right
Twin Higgs model, including the logarithmically enhanced contributions from
both fermion and scalar loops. Numerical results show that the one-loop
contributions are dominant over the tree level corrections in most regions of
parameter space. The experimentally allowed values of -parameter divide
the allowed parameter space into two regions; less than and
larger than roughly, for symmetry breaking scale . Our
numerical analysis significantly reduces the parameter space which are
favorably accessible to the LHC.Comment: Submitted for the SUSY07 proceedings, 4 pages, 3 eps figure
On the close encounters between Plutinos and Neptune Trojans: I. Statistic analysis and theoretical estimations
Close encounters (CEs) between celestial objects may exert significant
influence on their orbits. The influence will be even enhanced when two groups
of celestial objects are confined in stable orbital configurations, e.g. in
adjacent mean motion resonances (MMRs). Plutinos and Neptune Trojans, trapped
in the 2:3 and 1:1 MMRs with Neptune respectively, are such examples.
%Meanwhile, many objects among these two groups have peculiar orbits, seemingly
as the vestige of CEs. As the first part of our investigation, this paper
provides a detailed description of CEs between Plutinos and Trojans and their
potential influences on the Trojans' orbits. Statistical analyses of CE data
from numerical simulations reveal the randomness lying in the CEs between the
two planetesimals. The closest positions of CEs distribute symmetrically inside
the given CE region and no particular bias is found between the positive and
negative effects on the orbital elements of Trojans. Based on the Gaussian
approximation on the distribution of the velocity orientation of Plutino, and
the integral derivatives of Gaussian perturbation equations, a theoretical
method is built to estimate the CE effects. To further verify the randomness of
CEs, a Monte Carlo approach is applied, and it generates distribution features
consistent with the numerical results. In summary, CEs brought by realistic
Plutinos exert impartial effects and tiny total influence on the orbital
elements of Trojans. However, driven by the random walk mechanism, tiny effects
may accumulate to a prominent variation given sufficient CEs, which will be
discussed in the accompanying paper.Comment: 17 pages, 23 figure
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