926 research outputs found
Enhanced mass transfer during dwarf nova outbursts by irradiation of the secondary?
One of the remaining issues in the problems of dwarf novae is whether or not
enhanced mass transfer due to irradiation of the secondary stars could occur
during outbursts. In a previous paper (Osaki and Meyer 2003), we presented a
theoretical analysis that shows no appreciable enhancement of the mass outflow
rate. This conclusion is challenged by Smak (2004) who claims that equations
used in our analysis were incorrect and that in systems with short orbital
periods substantial enhancement could occur. In this letter, we examine the
origin of such divergent conclusions. We show that Smak's solutions are
unacceptable from the standpoint of the equation of continuity and that our
analysis is an appropriate one to treat this problem.Comment: 4 pages, accepted by Astronomy &.Astrophysics Letter
Repetitive rebrightening of EG Cancri: evidence for viscosity decay in the quiescent disk?
A WZ Sge-type dwarf nova, EG Cancri, exhibited six consecutive mini-outbursts
with a mean interval of about seven days after the end of the main outburst in
1996/1997. Most unusual was that the star abruptly entered into a deep faint
minimum after such frantic activities. We propose that this peculiar phenomenon
may be understoodin terms of viscosity decay in the cold disk. In this picture,
the viscosity is produced by MHD turbulence due to the magneto-rotational
instability ('Balbus-Hawley instability') and dies down exponentially with time
when the disk becomes cold because the magnetic fields decay due to finite
conductivity in the cold disk (Gammie & Menou 1998). But the viscosity is
refreshed to a high value every time when a mini-outburst occurs (i.e., the
disk becomes hot again). It is argued that a sudden cessation of repetitive
mini-outbursts may be brought about by a very small reduction in viscosity or a
small increase in its decay rate, which may in turn be produced most likely by
stochastic fluctuations of magnetic fields. Numerical simulations based on a
simple model reproduce the observed light curve of EG Cancri very well. We
discuss possible causes why the reflares after the main outburst occur mostly
in the WZ Sge-type stars.Comment: 8 pages, 5 figures, accepted for publication in A&
In-the-Gap SU UMa-Type Dwarf Nova, Var73 Dra with a Supercycle of about 60 Days
An intensive photometric-observation campaign of the recently discovered SU
UMa-type dwarf nova, Var73 Dra was conducted from 2002 August to 2003 February.
We caught three superoutbursts in 2002 October, December and 2003 February. The
recurrence cycle of the superoutburst (supercycle) is indicated to be 60
d, the shortest among the values known so far in SU UMa stars and close to
those of ER UMa stars. The superhump periods measured during the first two
superoutbursts were 0.104885(93) d, and 0.10623(16) d, respectively. A
0.10424(3)-d periodicity was detected in quiescence. The change rate of the
superhump period during the second superoutburst was , which
is an order of magnitude larger than the largest value ever known. Outburst
activity has changed from a phase of frequent normal outbursts and infrequent
superoutbursts in 2001 to a phase of infrequent normal outbursts and frequent
superoutbursts in 2002. Our observations are negative to an idea that this star
is an related object to ER UMa stars in terms of the duty cycle of the
superoutburst and the recurrence cycle of the normal outburst. However, to
trace the superhump evolution throughout a superoutburst, and from quiescence
more effectively, may give a fruitful result on this matter.Comment: 9 pages, 8 figures, submitted to A&
Is evidence for enhanced mass transfer during dwarf-nova outbursts well substantiated?
Outburst mechanisms of SU UMa-type dwarf novae are discussed. Two competing
models were proposed; a pure disk instability model called the thermal-tidal
instability model (TTI model) and the enhanced mass transfer model (EMT model).
Observational evidence for enhanced mass transfer from the secondary star
during outbursts is critically examined. It is demonstrated that most evidence
for enhanced mass transfer is not well substantiated. Patterson et al. (2002)
have recently claimed to have found evidence for enhanced mass transfer during
the 2001 outburst of WZ Sge. We show that their evidence is probably due to a
misinterpretation of their observed light curves. Our theoretical analysis also
shows that irradiation during outburst should not affect the mass transfer
rate. A refinement of the TTI model is proposed that can explain why superhumps
appear a few days after the superoutburst maximum in some SU UMa stars. We
present our own interpretation of the overall development of the 2001 outburst
of WZ Sge based on the TTI model that does not require the assumption of an
unproved enhanced mass transfer.Comment: 14 pages, accepted for publication in A&
On the Correlated X-ray and Optical Evolution of SS Cygni
We have analyzed the variability and spectral evolution of the prototype
dwarf nova system SS Cygni using RXTE data and AAVSO observations. A series of
pointed RXTE/PCA observations allow us to trace the evolution of the X-ray
spectrum of SS Cygni in unprecedented detail, while 6 years of optical AAVSO
and RXTE/ASM light curves show long-term patterns. Employing a technique in
which we stack the X-ray flux over multiple outbursts, phased according to the
optical light curve, we investigate the outburst morphology. We find that the
3-12 keV X-ray flux is suppressed during optical outbursts, a behavior seen
previously, but only in a handful of cycles. The several outbursts of SS Cygni
observed with the more sensitive RXTE/PCA also show a depression of the X-rays
during optical outburst. We quantify the time lags between the optical and
X-ray outbursts, and the timescales of the X-ray recovery from outburst. The
optical light curve of SS Cygni exhibits brief anomalous outbursts. During
these events the hard X-rays and optical flux increase together. The long-term
data suggest that the X-rays decline between outburst. Our results are in
general agreement with modified disk instability models (DIM), which invoke a
two-component accretion flow consisting of a cool optically thick accretion
disk truncated at an inner radius, and a quasi-spherical hot corona-like flow
extending to the surface of the white dwarf. We discuss our results in the
framework of one such model, involving the evaporation of the inner part of the
optically thick accretion disk, proposed by Meyer & Meyer-Hofmeister (1994).Comment: 24 pages, 8 figures, 2 tables, accepted for publication in Ap
Changes in the long term intensity variations in Cyg X-2 and LMC X-3
We report the detection of changes in the long-term intensity variations in
two X-ray binaries, Cyg X-2 and LMC X-3. In this work, we have used the
long-term light curves obtained with the All-Sky Monitors (ASMs) of the Rossi
X-Ray Timing Explorer (RXTE), Ginga, Ariel 5, and Vela 5B and the scanning
modulation collimator of HEAO 1. It is found that in the light curves of both
the sources, obtained with these instruments at various times over the last 30
years, more than one periodic or quasi-periodic component is always present.
The multiple prominent peaks in the periodograms have frequencies unrelated to
each other. In Cyg X-2, RXTE-ASM data show strong peaks at 40.4 and 68.8 days,
and Ginga-ASM data show strong peaks at 53.7 and 61.3 days. Multiple peaks are
also observed in LMC X-3. The various strong peaks in the periodograms of LMC
X-3 appear at 104, 169, and 216 days (observed with RXTE-ASM) and 105, 214, and
328 days (observed with Ginga-ASM). The present results, when compared with the
earlier observations of periodicities in these two systems, demonstrate the
absence of any stable long period. The 78 day periodicity detected earlier in
Cyg X-2 was probably due to the short time base in the RXTE data that were
used, and the periodicity of 198 days in LMC X-3 was due to a relatively short
duration of observation with HEAO 1.Comment: 11 pages, 7 postscript figures include
The Impact of Menthol Cigarettes on Smoking Initiation among Non-Smoking Young Females in Japan
Japan presents an excellent case-study of a nation with low female smoking rates and a negligible menthol market which changed after the cigarette market was opened to foreign competition. Internal tobacco industry documents demonstrate the intent of tobacco manufacturers to increase initiation among young females through development and marketing of menthol brands. Japanese menthol market share rose rapidly from less than 1% in 1980 to 20% in 2008. Menthol brand use was dominated by younger and female smokers, in contrast with non-menthol brands which were used primarily by male smokers. Nationally representative surveys confirm industry surveys of brand use and provide further evidence of the end results of the tobacco industryâs actionsâincreased female smoking in Japan. These findings suggest that female populations may be encouraged to initiate into smoking, particularly in developing nations or where female smoking rates remain low, if the tobacco industry can successfully tailor brands to them. The Japanese experience provides a warning to public health officials who wish to prevent smoking initiation among young females
Contact Discontinuities in Models of Contact Binaries Undergoing Thermal Relaxation Oscillations
In this paper we pursue the suggestion by Shu, Lubow & Anderson (1979) and
Wang (1995) that contact discontinuity (DSC) may exist in the secondary in the
expansion TRO (thermal relaxation oscillation) state. It is demonstrated that
there is a mass exchange instability in some range of mass ratio for the two
components. We show that the assumption of {\it constant} volume of the
secondary should be relaxed in DSC model. For {\it all} mass ratio the
secondary alway satisfies the condition that no mass flow returns to the
primary through the inner Lagrangian point. The secondary will expand in order
to equilibrate the interaction between the common convective envelope and the
secondary. The contact discontinuity in contact binary undergoing thermal
relaxation does not violate the second law of thermodynamics. The maintaining
condition of contact discontinuity is derived in the time-dependent model. It
is desired to improve the TRO model with the advanced contact discontinuity
layer in future detailed calculations.Comment: 5 pages in emulateapj, 1 figur
Cyclic brightening in the short-period WZ Sge-type cataclysmic variable SDSS J080434.20+510349.2
We have observed a new cataclysmic variable (CV) SDSS J080434.20+510349.2 and
study the origin of a long-term variability found in its light curve.
Multi-longitude time-resolved photometric observations were carried out to
analyze the uncommon behavior also found recently in two newly discovered CVs.
This study of SDSS J080434.20+510349.2 mainly concerns the understanding of the
nature of the observed double-humped light curve and its relation to a cyclic
brightening occurring during quiescence. The observations were obtained early
in 2007, when the object was at about V~17.1, 0.4 mag brighter than the
pre-outburst magnitude. The light curve shows a sinusoidal variability with an
amplitude of about 0.07 mag and a periodicity of 42.48 min, which is half of
the orbital period of the system. In addition, we have observed two
"mini-outbursts" of the system up to 0.6 mag, with a duration of about 4 days
each. The "mini-outburst" had a symmetric profile and repeated in about 32
days. Subsequent monitoring of the system shows a cyclical behaviour of such
"mini-outbursts" with a similar recurrence period. The origin of the
double-humped light curve and the periodic brightening is discussed in the
light of the evolutionary state of SDSS J080434.20+510349.2.Comment: 7 pages, 6 figures, Accepted by A&A, typos added, figure correcte
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