4,645 research outputs found
Outburst Photometry of the Eclipsing Dwarf Nova GY Cancri
We observed the ROSAT-selected eclipsing dwarf nova GY Cnc (=RX J0909.8+1849)
during the 2001 November outburst. We refined the orbital period to be
0.17544251(5) d. The fading portion of the outburst was indistinguishable from
those of typical dwarf novae with similar orbital periods. However, the
signature of orbital humps (or a hot spot) was far less prominently observed in
the orbital light curves and eclipse profiles than in usual dwarf novae with
similar orbital periods. The combination of low frequency of outbursts and the
apparent lack of slowly rising, long outbursts in GY Cnc is difficult to
reconcile within the standard framework of dwarf novae. We suspect that GY Cnc
may be the first above-the-gap counterpart of unusual eclipsing dwarf novae HT
Cas and IR Com.Comment: 6 pages, 7 figures, to appear in Publ. Astron. Soc. Japa
Reconstruction of the Structure of Accretion Disks in Dwarf Novae from the Multi-Band Light Curves of Early Superhumps
We propose a new method to reconstruct the structure of accretion disks in
dwarf novae using multi-band light curves of early superhumps. Our model
assumes that early superhumps are caused by the rotation effect of
non-axisymmetrically flaring disks. We have developed a Bayesian model for this
reconstruction, in which a smoother disk-structure tends to have a higher prior
probability. We analyzed simultaneous optical and near-infrared photometric
data of early superhumps of the dwarf nova, V455 And using this technique. The
reconstructed disk has two flaring parts in the outermost region of the disk.
These parts are responsible for the primary and secondary maxima of the light
curves. The height-to-radius ratio is h/r=0.20-0.25 in the outermost region. In
addition to the outermost flaring structures, flaring arm-like patterns can be
seen in an inner region of the reconstructed disk. The overall profile of the
reconstructed disk is reminiscent of the disk structure that is deformed by the
tidal effect. However, an inner arm-like pattern, which is responsible for the
secondary minimum in the light curve, cannot be reproduced only by the tidal
effect. It implies the presence of another mechanism that deforms the disk
structure. Alternatively, the temperature distribution of the disk could be
non-axisymmetric. We demonstrate that the disk structure with weaker arm-like
patterns is optimal in the model including the irradiation effect. However, the
strongly irradiated disk gives quite blue colors, which may conflict with the
observation. Our results suggest that the amplitude of early superhumps depends
mainly on the height of the outermost flaring regions of the disk. We predict
that early superhumps can be detected with an amplitude of >0.02 mag in about
90% of WZ Sge stars.Comment: 17 pages, 17 figures, accepted for publication in PAS
Dwarf Novae in the Shortest Orbital Period Regime: II. WZ Sge Stars as the Missing Population near the Period Minimum
WZ Sge-type dwarf novae are characterized by long recurrence times of
outbursts (~10 yr) and short orbital periods (<~ 85 min). A significant part of
WZ Sge stars may remain undiscovered because of low outburst activity.
Recently, the observed orbital period distribution of cataclysmic variables
(CVs) has changed partly because outbursts of new WZ Sge stars have been
discovered routinely. Hence, the estimation of the intrinsic population of WZ
Sge stars is important for the study of the population and evolution of CVs. In
this paper, we present a Bayesian approach to estimate the intrinsic period
distribution of dwarf novae from observed samples. In this Bayesian model, we
assumed a simple relationship between the recurrence time and the orbital
period which is consistent with observations of WZ Sge stars and other dwarf
novae. As a result, the minimum orbital period was estimated to be ~70 min. The
population of WZ Sge stars exhibited a spike-like feature at the shortest
period regime in the orbital period distribution. These features are consistent
with the orbital period distribution previously predicted by population
synthesis studies. We propose that WZ Sge stars and CVs with a low
mass-transfer rate are excellent candidates for the missing population
predicted by the evolution theory of CVs.Comment: 9 pages, 5 figures, accepted for publication in PAS
Abstract and concrete type theories
In this thesis, we study abstract and concrete type theories. We introduce an abstract notion of a type theory to obtain general results in the semantics of type theories, but we also provide a syntactic way of presenting a type theory to allow us a further investigation into a concrete type theory to obtain consistency and independence results
Cubical Assemblies, a Univalent and Impredicative Universe and a Failure of Propositional Resizing
Superconducting Volume Fraction in Overdoped Regime of La_2-x_Sr_x_CuO_4_: Implication for Phase Separation from Magnetic-Susceptibility Measurement
We have grown a single crystal of La_2-x_Sr_x_CuO_4_ in which the Sr
concentration, x, continuously changes from 0.24 to 0.29 in the overdoped
regime and obtained many pieces of single crystals with different x values by
slicing the single crystal. From detailed measurements of the magnetic
susceptibility, chi, of each piece, it has been found that the absolute value
of chi at the measured lowest temperature 2 K, |chi_2K_|, on field cooling
rapidly decreases with increasing x as well as the superconducting (SC)
transition temperature. As the value of |chi_2K_| is regarded as corresponding
to the SC volume fraction in a sample, it has been concluded that a phase
separation into SC and normal-state regions occurs in a sample of
La_2-x_Sr_x_CuO_4_ in the overdoped regime.Comment: 4 pages, 3 figures, ver. 2 has been accepted in J. Phys. Soc. Jp
In-situ growth of superconducting NdFeAs(O,F) thin films by Molecular Beam Epitaxy
The recently discovered high temperature superconductor F-doped LaFeAsO and
related compounds represent a new class of superconductors with the highest
transition temperature (Tc) apart from the cuprates. The studies ongoing
worldwide are revealing that these Fe-based superconductors are forming a
unique class of materials that are interesting from the viewpoint of
applications. To exploit the high potential of the Fe-based superconductors for
device applications, it is indispensable to establish a process that enables
the growth of high quality thin films. Efforts of thin film preparation started
soon after the discovery of Fe-based superconductors, but none of the earlier
attempts had succeeded in an in-situ growth of a superconducting film of
LnFeAs(O,F) (Ln=lanthanide), which exhibits the highest Tc to date among the
Fe-based superconductors. Here, we report on the successful growth of
NdFeAs(O,F) thin films on GaAs substrates, which showed well-defined
superconducting transitions up to 48 K without the need of an ex-situ heat
treatment
Riemann-Hurwitz formula for Morita-Mumford classes and surface symmetries
Let a finite group G act on a compact Riemann surface C in a faithful and orientation preserving way. Then we describe the Morita-Mumford classes en (Ca) E H2n (G;Z) of the homotopy quotient (or the Borel construction) Ca of the action in terms of fixed-point data. This fixed-point formula is deduced from a higher analogue of the classical Riemann-Hurwitz formula based on computations of Miller [Mi] and Morita [Mo]
Magnetic Phase Diagram of the Hole-doped CaNaCuOCl Cuprate Superconductor
We report on the magnetic phase diagram of a hole-doped cuprate
CaNaCuOCl, which is free from buckling of CuO
planes, determined by muon spin rotation and relaxation. It is characterized by
a quasi-static spin glass-like phase over a range of sodium concentration
(), which is held between long range antiferromagnetic
(AF) phase () and superconducting phase where the system is
non-magnetic for . The obtained phase diagram qualitatively agrees
well with that commonly found for hole-doped high-\tc cuprates, strongly
suggesting that the incomplete suppression of the AF order for is an
essential feature of the hole-doped cuprates.Comment: 5 pages, submitted to Phys. Rev. Let
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