731 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
Photometric Study of KR Aurigae during the High State in 2001
We photometrically observed the VY Scl-type cataclysmic variable KR Aurigae
after its final rise from the fading episode in 2000-2001. Time-resolved
observation revealed that the light curve is dominated by persistent short-term
variation with time-scales of minutes to tens of minutes. On some nights,
quasi-periodic variations with periods of 10--15 min were observed. No coherent
variation was detected. The power spectral density of the variation has a power
law component (f^(-1.63)). The temporal properties of the short-term variations
in KR Aur present additional support for the possibility that flickering in CVs
may be better understood as a result of self-organized critical state as in
black-hole candidates. The light curve lacks "superhump"-type signals, which
are relatively frequently seen in VY Scl-type systems and which are suggested
to arise from tidal instability of the accretion disk induced by changing
mass-transfer rates. The present observation suggests a borderline of superhump
excitation in VY Scl-type stars between mass ratios q=0.43 (MV Lyr) and q=0.60
(KR Aur).Comment: 8 pages, 6 figures, to appear in Publ. Astron. Soc. Japa
Numerical scheme based on the spectral method for calculating nonlinear hyperbolic evolution equations
High-precision numerical scheme for nonlinear hyperbolic evolution equations
is proposed based on the spectral method. The detail discretization processes
are discussed in case of one-dimensional Klein-Gordon equations. In conclusion,
a numerical scheme with the order of total calculation cost is
proposed. As benchmark results, the relation between the numerical precision
and the discretization unit size are demonstrated.Comment: To appear in the proceedings of ICCM2020. Figure is modified from the
original versio
Superhumps of CC Cancri Revisited
We observed the 2001 November superoutburst of CC Cnc. This observation makes
the first detailed coverage of a superoutburst of this object. The
best-determined mean superhump period is 0.075518 +/- 0.000018 d, which is 2.7%
longer than the reported orbital period. This fractional superhump excess is a
quite typical value for a normal SU UMa-type dwarf nova, excluding the
previously raised possibility that CC Cnc may have an anomalously large
fractional superhump excess. During the superoutburst plateau, the object
showed a decrease of the superhump period at dot(P)/P = -10.2(1.3) x 10^(-5),
which is one of the largest negative period derivative known in all SU UMa-type
dwarf novae.Comment: 5 pages, 5 figures, to appear in Publ. Astron. Soc. Japa
Chiral charge-density-waves
We discovered the chirality of charge density waves (CDW) in 1T-TiSe by
using scanning tunnelling microscopy (STM) and optical ellipsometry. We found
that the CDW intensity becomes , where (i =1, 2, 3) is the amplitude of the tunnelling current
contributed by the CDWs. There were two states, in which the three intensity
peaks of the CDW decrease \textit{clockwise} and \textit{anticlockwise} when we
index each nesting vector in order of intensity in the Fourier transformation
of the STM images. The chirality in CDW results in the three-fold symmetry
breaking. Macroscopically, two-fold symmetry was indeed observed in optical
measurement. We propose the new generalized CDW chirality H_{CDW} \equiv
{\boldmath q_1} \cdot ({\boldmath q_2}\times {\boldmath q_3}), where
{\boldmath q_i} are the nesting vectors, which is independent of the
symmetry of components. The nonzero - the triple-{\boldmath q}
vectors do not exist in an identical plane in the reciprocal space - should
induce a real-space chirality in CDW system.Comment: 12 pages, 4 figure
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.Comment: 6 pages, 4 figures, PASJ in pres
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.Comment: 5 pages, 2 figures, PASJ in pres
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