arXiv subjects

T. Kato

Publications and source records attributed to T. Kato.

At least 127 records · Page 7Linked to original sources

arXiv2002

IW And is a Z Cam-Type Dwarf Nova

IW And was discovered as a unique blue variable, which spends 72% of time in "inactive" state, and was only occasionally observed in bright or faint states. Although the past spectroscopy confirmed that the object is a cataclysmic variable (CV), the object has been regarded as significantly different from the known subclasses of CVs. We observed IW And on 55 nights between 2001 December 6 and 2002 March 25. These observations clearly indicate that the object is a Z Cam-type dwarf nova. The duty cycle of standstill in IW And is exceptionally high among Z Cam stars. IW And is apparently the first object to fill the gap between classical Z Cam stars and novalike (NL) stars.

astro-ph↗

arXiv2002

Recurrent Nova IM Normae

We detected the second historical outburst of the 1920 nova IM Nor. Accurate astrometry of the outbursting object revealed the true quiescent counterpart having a magnitude of R=17.0 mag and B=18.0 mag. We show that the quiescent counterpart shows a noticeable variation. From the comparison of light curves and spectroscopic signatures, we propose that IM Nor and CI Aql comprise a new class of recurrent novae bearing some characteristics similar to those of classical novae. We interpret that the noticeable quiescent variation can be a result of either high orbital inclination, which may be also responsible for the low quiescent brightness, or the presence of high/low states. If the second possibility is confirmed by future observations, IM Nor becomes the first recurrent nova showing state changes in quiescence. Such state changes may provide a missing link between recurrent novae and supersoft X-ray sources.

astro-ph↗

arXiv2002

V2540 Oph (Nova Oph 2002): Large-Amplitude Slow Nova with Strong Post-Outburst Oscillations

V2540 Oph (Nova Oph 2002) is a classical nova discovered by Katsumi Haseda and Yuji Nakamura on 2002 January 24. The light curve of this nova shows strong post-outburst oscillations as were observed in V1178 Sco and V4361 Sgr. Accurate astrometry of the nova yeilded an upper limit of 21 mag for the nova precursor. In combination with the observed decline rate, We propose that the nova should have either a short orbital period or a high inclination. We suggest that V2540 Oph may be analogous to V2214 Oph, a presumed magnetic nova inside the period gap.

astro-ph↗

arXiv2002

Unusual Outbursting State of a Z Cam-Type Star HL CMa

HL CMa is a Z Cam-type dwarf nova which was discovered as an Einstein X-ray source. In addition to normal outbursts and standstills, we noticed the presence of "the third" outbursting state. During this period, the star showed weak outbursts with a long outburst cycle length. We propose that this phenomenon is caused by a heating on the accretion disk. The presence of strong P Cyg feature in the ultraviolet and the unusual presence of high-excitation optical lines could be interpreted as an emerging signature of strong irradiation field. Since the object is still in this unusual state in 2002 March, we encourage X-ray and spectroscopic observations to detect further signatures of high-energy photons and irradiation.

astro-ph↗

arXiv2002

Kilo-Second Quasi-Periodic Oscillations in the Cataclysmic Variable DW Cancri

Our photometric monitoring revealed that DW Cnc, which was originally classified as a dwarf nova (V=15--17.5), remained at a bright state of Rc=14.68+/-0.07 for 61 days. In conjunction with optical spectra lacking a strong He II emission line, we propose that the object is not a dwarf nova, but a non-magnetic nova-like variable. Throughout our monitoring, the object showed strong quasi-periodic oscillations (QPOs) with amplitudes reaching about 0.3 mag. Our period analysis yielded a power spectrum with two peaks of QPOs, whose center periods are 37.5+/-0.1 and 73.4+/-0.4 min and, furthermore, with a significant power in frequencies lower than the QPOs. DW Cnc is a unique cataclysmic variable in which kilo-second QPOs were continuously detected for 61 days. We propose two possible interpretations of DW Cnc: (i) A permanent superhumper below the period minimum of hydrogen-rich cataclysmic variables. (ii) A nova-like variable having an orbital period over 3 hours. In this case, the QPOs may be caused by trapped disk oscillations.

astro-ph↗

arXiv2002

Discovery of a Dwarf Nova Breaking the Standard Sequence of Compact Binary Evolution

We revealed that the dwarf nova 1RXS J232953.9+062814 is an SU UMa-type system with a superhump period of 66.774+/-0.010 min. The short period strongly indicates that the orbital period of this object is below the period minimum of cataclysmic variables. The superhump period is 4.04+/-0.02 % longer than the photometric period during quiescence (64.184+/-0.003 min), which is probably associated with the orbital period. Although the standard evolutionary scenario of cataclysmic variables predicts lower mass-transfer rates in systems with shorter orbital periods, we revealed firm evidence of a relatively high mass-transfer rate from its large proper motion and bright apparent magnitude. Its proximity indicates that we have overlooked a number of objects in this new class. With the analogous system of V485 Cen, these objects establish the first subpopulation in hydrogen-rich cataclysmic variables below the period minimum.

astro-ph↗

arXiv2002

Magnetic Excitations of the Spin Gap System TlCuCl$_3$

TlCuCl$_3$ has a singlet ground state with the excitation gap $Δ=0.65$ meV. The magnetic excitations in TlCuCl$_3$ have been investigated by means of neutron inelastic scattering experiments. The constant-$\it{\pmb Q}$ energy scan profiles were collected in the $a^*-c^*$ plane. A well-defined single magnetic excitation mode was observed. The dispersion relations along four different directions were determined. The lowest excitation occurs at ${\it{\pmb Q}}=(h, 0, l)$ with integer $h$ and odd $l$, as observed in KCuCl$_3$. A cluster series expansion up to the sixth order was applied to analyze the dispersion relations, and the individual exchange interactions were evaluated. It was demonstrated that TlCuCl$_3$ is a strongly coupled spin-dimer system.

cond-mat.str-el↗

arXiv2002

V893 Sco Is Not an ER UMa-Type Star

V893 Sco is a recently rediscovered bright eclipsing dwarf nova below the period gap. Most recently, Mason et al. (2001) proposed an idea that V893 Sco is an ER UMa-type dwarf nova. From the analysis of our CCD observations and reports to VSNET, we show that V893 Sco bears no similar characters with ER UMa stars. We propose that the arguments in Mason et al. (2001), including the evolutionary status of ER UMa star as inferred from the observation of V893 Sco, need to be reconsidered.

astro-ph↗

arXiv2002

BL Lacertae: complex spectral variability and rapid synchrotron flare detected with BeppoSAX

We report on two BeppoSAX observations of BL Lac (2200+420) performed respectively in June and December 1999, as part of a ToO program to monitor blazars in high states of activity. During both runs the source has been detected up to 100 keV, but it showed quite different spectra: in June it was concave with a very hard component above 5-6 keV (alpha_1 ~ 1.6; alpha_2 ~ 0.15); in December it was well fitted by a single power law (alpha ~ 0.6). During the first BeppoSAX observation BL Lac showed an astonishing variability episode: the 0.3 - 2 keV flux doubled in ~ 20 minutes, while the flux above 4 keV was almost constant. This frequency-dependent event is one of the shortest ever recordered for BL Lac objects and places lower limits on the dimension and the magnetic field of the emitting region and on the energy of the synchrotron radiating electrons. A similar but less extreme behaviour is detected also in optical light curves, that display non-simultaneous, smaller fluctuations of ~ 20% in 20 min. We fit the spectral energy distributions with a homogeneous, one-zone model to constrain the emission region in a very simple but effective SSC + external Compton scenario, highlightning the importance of the location of the emitting region with respect to the Broad Line Region and the relative spectral shape dependence. We compare our data with historical radio to gamma-ray Spectral Energy Distributions.

astro-ph↗

arXiv2002

On the Origin of Early Superhumps in WZ Sge-Type Stars

The origin of early superhumps, which are double-wave periodic modulations seen only during the earliest stage of WZ Sge-type outburst, has not been well understood. Based on recent discovery of two-armed arch-like patterns on Doppler tomograms in conjunction with early superhumps, we propose a new interpretation on the origin of early superhumps, following the new interpretation by Smak (2001) and Ogilvie (2001) of the two-armed pattern seen in IP Peg. If we consider irradiation of the elevated surface of the accretion disk caused by vertical tidal deformation, we can consistently explain the observed features on Doppler tomograms and photometric waves at the same time. We interpret that a combination of low mass-ratios (q) and low mass-transfer rates, necessary to give rise to these tidal effects, discriminate WZ Sge-type stars from other SU UMa-type dwarf novae. Based on recent fluid calculations, such an effect would be observable in higher q systems. We interpret that RZ Leo is an example of such objects.

astro-ph↗

arXiv2001

Field-Induced Two-Step Phase Transitions in the Singlet Ground State Triangular Antiferromagnet CsFeBr$_3$

The ground state of the stacked triangular antiferromagnet CsFeBr$_3$ is a spin singlet due to the large single ion anisotropy $D(S^z)^2$. The field-induced magnetic ordering in this compound was investigated by the magnetic susceptibility, the magnetization process and specific heat measurements for an external field parallel to the $c$-axis. Unexpectedly, two phase transitions were observed in the magnetic field $H$ higher than 3 T. The phase diagram for temperature versus magnetic field was obtained. The mechanism leading to the successive phase transitions is discussed.

cond-mat.str-el↗

arXiv2001

Observation of Field-Induced Transverse Néel Ordering in the Spin Gap System TlCuCl$_3$

Neutron elastic scattering experiments have been performed on the spin gap system TlCuCl$_3$ in magnetic fields parallel to the $b$-axis. The magnetic Bragg peaks which indicate the field-induced Néel ordering were observed for magnetic field higher than the gap field $H_{\rm g}\approx 5.5$ T at $Q=(h, 0, l)$ with odd $l$ in the $a^*-c^*$ plane. The spin structure in the ordered phase was determined. The temperature and field dependence of the Bragg peak intensities and the phase boundary obtained were discussed in connection with a recent theory which describes the field-induced Néel ordering as a Bose-Einstein condensation of magnons.

cond-mat.str-el↗

arXiv2000

Oblique triangular antiferromagnetic phase in CsCu$_{1-x}$Co$_x$Cl$_3$

The spin-1/2 stacked triangular antiferromagnet CsCu$_{1-x}$Co$_x$Cl$_3$ with $0.015<x<0.032$ undergoes two phase transitions at zero field. The low-temperature phase is produced by the small amount of Co$^{2+}$ doping. In order to investigate the magnetic structures of the two ordered phases, the neutron elastic scattering experiments have been carried out for the sample with $x\approx 0.03$. It is found that the intermediate phase is identical to the ordered phase of CsCuCl$_3$, and that the low-temperature phase is an oblique triangular antiferromagnetic phase in which the spins form a triangular structure in a plane tilted from the basal plane. The tilting angle which is 42$^{\circ}$ at $T=1.6$ K decreases with increasing temperature, and becomes zero at $T_{\rm N2} =7.2$ K. An off-diagonal exchange term is proposed as the origin of the oblique phase.

cond-mat.str-el↗

arXiv2000

Development of the 50-Mev DTL for the Jaeri/Kek Joint Project

An Alvaretz-type DTL, to accelerate the H- ion beam from 3 to 50 MeV, is being constructed as the injector for the JAERI/KEK Joint Project. The following components of the DTL have been developed: (1) a cylindrical tank, made by copper electroforming; (2) rf contactors; (3) a pulse-excited quadrupole magnet with a hollow coil made by copper electroforming; (4) a switching-regulator-type pulsed-power supply for the quadrupole magnet. High-power tests of the components have been conducted using a short-model tank. Moreover a breakdown experiment of the copper electrodes has been carried out in order to study the properties of several kinds of copper materials.

physics.acc-ph↗

arXiv2000

Development of a DTL Quadrupole Magnet with a New Electroformed Hollow Coil for the Jaeri/Kek Joint Project

Quadrupole electromagnets have been developed with a hollow coil produced using an improved periodic reverse electroforming. These will be installed in each of the drift tubes of the DTL (324 MHz) as part of the JAERI/KEK Joint Project at the high-intensity proton accelerator facility. Measurements of the magnets' properties were found to be consistent with computer-calculated estimated. The details of the design, the fabrication process, and the measurement results for the quadrupole magnet are described.

physics.acc-ph↗

arXiv2000

Discovery and Photometric Observation of the Optical Counterpart in a Possible Galactic Halo X-ray Transient, XTE J1118+480

We discovered the optical counterpart about 13 mag of a soft X-ray transient, XTE J1118+480 on 2000 March 30. We perform astrometry and provide the accurate position as R.A. = 11h18m10s.85, Decl. = +48o02'12".9. The outbursting object is identified with a 18.8 mag star in USNO catalog. Our pre-discovery data shows another outburst during 2000 January, again coinciding with an outburst detected in X-rays. Through the CCD time-series photometry, we found the presence of a periodic variation with the amplitude of 0.055 mag and the period of 0.17078(0.00004)d which we consider as promising candidate of orbital period. Because of the high galactic latitude and faint quiescence magnitude of 18.8, XTE J1118+480 is the possible first firmly identified black hole candidate (BHC) X-ray transient in the galactic halo.

astro-ph↗

arXiv2000

Magnetic Excitations in the Spin Gap System TlCuCl$_3$

Single-crystal neutron inelastic scattering was performed in order to investigate the magnetic excitations in the spin gap system TlCuCl$_3$. The constant-${\bf Q}$ energy scan profiles were collected in the $a^*-c^*$ plane. Three excitations are observed for $E{\leq}15$ meV. One of the excitations is identified to be magnetic excitation. The lowest magnetic excitation with $E\sim 0.5$ meV occurs at ${\bf Q}=(1, 0, 1)$, as observed in KCuCl$_3$. The dispersion relation of the magnetic excitation can be fitted to the dispersion formula derived from the weakly coupled dimer model. The intradimer interaction is evaluated as $J=5.23$ meV, which coincides with the value estimated from the susceptibility data. However, one of the interdimer interactions obtained is so large that the weakly coupled dimer model is broken down.

cond-mat↗

arXiv2000

Discovery of a New Deeply Eclipsing SU UMa-Type Dwarf Nova, IY UMa (= TmzV85)

We discovered a new deeply eclipsing SU UMa-type dwarf nova, IY UMa, which experienced a superoutburst in 2000 January. Our monitoring revealed two distinct outbursts, which suggest a superoutburst interval of ~800 d, or its half, and an outburst amplitude of 5.4 mag. From time-series photometry during the superoutburst, we determined a superhump and orbital period of 0.07588 d and 0.0739132 d, respectively.

astro-ph↗