2,182 research outputs found
Polarization of high-energy emissions from the Crab pulsar
We investigate polarization of high-energy emissions from the Crab pulsar in
the frame work of the outer gap accelerator, following previous works of Cheng
and coworkers. The recent version of the outer gap, which extends from inside
the null charge surface to the light cylinder, is used for examining the
synchrotron radiations from the secondary and the tertiary pairs, which are
produced outside the gap. We calculate the light curve, the spectrum and the
polarization characteristics, simultaneously, by taking into account gyration
motion of the particles. The polarization position angle curve and the
polarization degree are calculated to compare with the Crab optical data. We
demonstrate that the radiations from inside the null charge surface make
outer-wing and off-pulse emissions in the light curve, and the tertiary pairs
contribute to bridge emissions. The emissions from the secondary pairs explain
the main features of the observed light curve and spectrum.
On the other hand, both emissions from inside the null charge surface and
from the tertiary pairs are required to explain the optical polarization
behavior of the Crab pulsar. The energy dependence of the polarization features
is expected by the present model. For the Crab pulsar, the polarization
position angle curve indicates that the viewing angle of the observer measured
from the rotational axis is greater than .Comment: 32pages, 8 figures. Accepted for publication in Ap
GeV detection of HESS J0632+057
HESS J0632+057 is the only gamma-ray binary that has been detected at TeV
energies, but not at GeV energies yet. Based on nearly nine years of Fermi
Large Area Telescope (LAT) Pass 8 data, we report here on a deep search for the
gamma-ray emission from HESS J0632+057 in the 0.1-300 GeV energy range. We find
a previously unknown gamma-ray source, Fermi J0632.6+0548, spatially coincident
with HESS J0632+057. The measured flux of Fermi J0632.6+0548 is consistent with
the previous flux upper limit on HESS J0632+057 and shows variability that can
be related to the HESS J0632+057 orbital phase. We propose that Fermi
J0632.6+0548 is the GeV counterpart of HESS J0632+057. Considering the Very
High Energy (VHE) spectrum of HESS J0632+057, a possible spectral turnover
above 10 GeV may exist in Fermi J0632.6+0548, as appears to be common in other
established gamma-ray binaries.Comment: 17 pages, 4 figures, 1 table; Accepted for publication in Ap
Monte Carlo direct simulation technique user's manual
User manual for Monte Carlo direct simulation techniqu
Modelling the light curves of PSR B1259-63/LS 2883-II.The effects of anisotropic pulsar wind and Doppler-boosting
PSR B1259-63/LS 2883 is a binary system in which a 48-ms pulsar orbits around
a Be star in a high eccentric orbit with a long orbital period of about 3.4 yr.
It is special for having asymmetric two-peak profiles in both the X-ray and the
TeV light curves. Recently, an unexpected GeV flare was detected by
gamma-ray observatory several weeks after the last periastron passage. In this
paper, we show that this observed GeV flare could be produced by the
Doppler-boosted synchrotron emission in the bow shock tail. An anisotropic
pulsar wind model, which mainly affects the energy flux injection to the
termination shock in different orbital phase, is also used in this paper, and
we find that the anisotropy in the pulsar wind can play a significant role in
producing the asymmetric two-peak profiles in both X-ray and TeV light curves.
The X-ray and TeV photons before periastron are mainly produced by the shocked
electrons around the shock apex and the light curves after periastron are
contributed by the emission from the shock apex and the shock tail together,
which result in the asymmetric two-peak light curves.Comment: 5 Fig, accepted by Ap
Comparison of crystal structures and effects of Co substitution in a new member of Fe-1111 superconductor family AeFeAsF(Ae = Ca and Sr): a possible candidate for higher Tc superconductor
We refined crystal structures of newly found members of the Fe-1111
superconductor family, CaFe\_{1-x}Co\_{x}AsF and SrFe\_{1-x}Co\_{x}AsF (x = 0,
0.06, 0.12) by powder synchrotron X-ray diffraction analysis. The tetragonal to
orthorhombic phase transitions were observed at ~120 K for unsubstituted
CaFeAsF and at ~180 K for unsubstituted SrFeAsF, the transition temperatures
agreeing with kinks observed in temperature-dependent resistivity curves.
Although the transition temperature decreases, the structural phase transitions
were observed below 100 K in both samples of x = 0.06, and finally they were
suppressed in the doping level of x = 0.12. The refined structures reveal that
distortions of the FeAs4 tetrahedron from the regular tetrahedron likely
originate from mismatches in atomic radii among the constituent elements. In
this system, the enlarged FeAs4 tetrahedron resulting from larger radius of Sr
than that of Ca is flattened along a-b plane, whereas the smaller radius of Ca
makes the tetrahedron closer to regular one, and their characteristic shapes
are further enhanced by Co substitution. These results suggest that the CaFeAsF
compound is a promising candidate for higher-Tc superconductor.Comment: 17 pages, 8 figures, 2 tables, Supplementary information is included
at the end of the documen
[OII]3727 Emission from the Companion to the Quasar BR 1202-0725 at z=4.7
Results of a narrow-band imaging for the redshifted [OII]3727 emission around
a quasar at z=4.7 obtained with the Subaru telescope and CISCO (a Cassegrain
near infrared camera) are presented. A significant emission line is detected in
the narrow-band H_2 (v=1-0 S(1)) filter at a location 2.4" northwest from the
quasar, where the presence of a companion has been reported in Lyman alpha
emission and the rest-frame UV continuum. We identify this line as [OII]3727
emission and confirm that the source really is a companion at z=4.7. The
[OII]3727 flux from the companion is estimated to be 2.5 x 10^{-17} erg s^{-1}
cm^{-2}. If the companion is a star forming object, the inferred star formation
rate is as high as 45-230 M_{solar} yr^{-1} even without assuming the
extinction correction. This value is higher than those derived from the Lyman
alpha emission or from the UV continuum. Thus, provided that the difference is
caused by dust extinction, the extinction corrected star formation rate is
calculated to be 45 to 2300 M_{solar} yr^{-1} depending on the assuming
extinction curves.Comment: 15 pages including 3 figures. Accepted for publication in PAS
Theory of Stellar Oscillations
In recent years, astronomers have witnessed major progresses in the field of
stellar physics. This was made possible thanks to the combination of a solid
theoretical understanding of the phenomena of stellar pulsations and the
availability of a tremendous amount of exquisite space-based asteroseismic
data. In this context, this chapter reviews the basic theory of stellar
pulsations, considering small, adiabatic perturbations to a static, spherically
symmetric equilibrium. It starts with a brief discussion of the solar
oscillation spectrum, followed by the setting of the theoretical problem,
including the presentation of the equations of hydrodynamics, their
perturbation, and a discussion of the functional form of the solutions.
Emphasis is put on the physical properties of the different types of modes, in
particular acoustic (p-) and gravity (g-) modes and their propagation cavities.
The surface (f-) mode solutions are also discussed. While not attempting to be
comprehensive, it is hoped that the summary presented in this chapter addresses
the most important theoretical aspects that are required for a solid start in
stellar pulsations research.Comment: Lecture presented at the IVth Azores International Advanced School in
Space Sciences on "Asteroseismology and Exoplanets: Listening to the Stars
and Searching for New Worlds" (arXiv:1709.00645), which took place in Horta,
Azores Islands, Portugal in July 201
Nature of a Strongly-Lensed Submillimeter Galaxy SMM J14011+0252
We have carried out near-infrared JHK spectroscopy of a gravitationally
lensed submillimeter galaxy SMM J14011+0252 at z=2.565, using OHS and CISCO on
the Subaru telescope. This object consists of two optical components, J1 and
J2, which are lensed by the cluster Abell 1835. J1 suffers additional strong
lensing by a foreground galaxy at z=0.25 in the cluster. The rest-optical
H-alpha, H-beta, and [O II]3727 lines are detected in both J1 and J2, and [N
II]6548,6583 lines are also detected in J1. A diagnosis of emission-line ratios
shows that the excitation source of J1 is stellar origin, consistent with
previous X-ray observations. The continua of J1 and J2 show breaks at rest
4000A, indicating relatively young age. Combined with optical photometry, we
have carried out model spectrum fitting of J2 and find that it is a very young
(~50 Myr) galaxy of rather small mass (~10e8 M_sol) which suffers some amount
of dust extinction. A new gravitational lensing model is constructed to assess
both magnification factor and contamination from the lensing galaxy of the
component J1, using HST-F702W image. We have found that J1 suffers strong
lensing with magnification of ~30, and its stellar mass is estimated to be <
10e9 M_sol. These results suggest that SMM J14011+0252 is a major merger system
at high redshift that undergoes intense star formation, but not a formation
site of a giant elliptical. Still having plenty of gas, it will transform most
of the gas into stars and will evolve into a galaxy of < 10e10 M_sol.
Therefore, this system is possibly an ancestor of a less massive galaxy such as
a mid-sized elliptical or a spiral at the present.Comment: 21 pages, 11 figures. Accepted for publication in Astronomical
Journa
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