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text:
\section{Introduction}

Since the discovery of the first pulsating white dwarf in an accreting
close binary cataclysmic variable (GW Lib; Warner \& van Zyl 1998, van
Zyl et al. 2000, 2004), photometry
of systems with similar orbital periods and optical spectra has revealed
at least 10 more (Warner \& Woudt 2004, Woudt \& Warner 2004,
Araujo-Betancor et al. 2005, Vanlandingham et al. 2005,
Patterson et al. 2005a,b, Mukadam et al. 2006,
G\"ansicke et al. 2006, Nilsson et al.
2006).
 Seven of these pulsating accreting white dwarfs were found by followup work on
cataclysmic variables (CVs) that were discovered in the Sloan Digital Sky Survey
(SDSS; York et al. 2000) by Szkody et al. (2002b,2003,2004,2005,2006).
The optical clue for candidate pulsating white
dwarfs is the
presence of broad absorption lines (originating from the white dwarf)
flanking the Balmer emission lines (originating from the disk). In order
to be able to view the white dwarf, the accretion disk contribution to
the optical light has to be small, a situation that occurs at very low
mass transfer rates, and hence short
orbital periods (near 80 min). Since the SDSS provides spectra that
are about 2 magnitudes fainter than previous surveys, up to 25\% of
SDSS discovered CVs show the white dwarf presence (Szkody et al. 2005).
As the analysis of pulsation frequencies can lead to mass determination
and other aspects of the internal structure of the white dwarf
via the technique of asteroseismology, the compilation of a significant number of
pulsating CVs
provides a valuable database for probing the effects of mass transfer and
accretion on the long term evolution of white dwarfs as well as the effect
of external heat input, He enriched envelopes and fast rotation on the
location of the instability strip.

Non-interacting hydrogen atmosphere (DA) pulsating white dwarfs (DAVs or ZZ
Ceti stars)
 show typical non-radial g-mode pulsations with periods of 50-1400s
and have temperatures in the narrow range of 10800-12,300K and log g$\sim$8
(Bergeron et al. 1995,2004, Koester \& Allard 2000, Mukadam et al. 2004, Gianninas et al. 2005). While the pulsation frequencies
and amplitudes of CV pulsators appear to be similar to those of ZZ Ceti systems (van Zyl et
al. 2004, Warner \& Woudt 2004, Woudt \& Warner 2004, Mukadam
et al. 2006), the temperatures of the underlying white dwarfs may be
quite different. UV observation of GW Lib (Szkody et al. 2002a) with the
Space Telescope Imaging Spectrograph (STIS) revealed a white dwarf with
a temperature of 14,700K (or a best fit with 63\% of the white dwarf
having a temperature of 13,300K and the remainder at 17,100K),
temperatures far outside the empirical instability strip for non-interacting
ZZ Ceti stars. Townsley, Arras \& Bildsten (2004) could match the pulsation periods
and high temperature if they assumed ${\ell }$=1 g-modes and a 1M$_{\odot}$
white dwarf with an accreted H-rich layer of 3$\times$10$^{-5}$M$_{\odot}$.
On the other hand, Araujo-Betancor et al. (2005) used a snapshot STIS
spectrum to show that the CV pulsator HS2331+3905 could be fit with a
10,500K, 0.6M$_{\odot}$ white dwarf, within the range of normal ZZ Ceti stars.
Of course, pulsating CV white dwarfs are rotating very rapidly compared to
non-interacting ZZ Ceti stars and the thermal profiles are quite different
because the surface layer is heated from above by compression and
irradiation due
to accretion. Although the accretion rates for the CV pulsating white
dwarfs are small ($\sim10^{-13}\,{\mathrm{M}}_{\odot}$ yr$^{-1}$), the thermal
profiles may still be altered and
the effective temperature
might not be the best parameter to locate the instability strip.
This
does not imply that the temperature in the driving regions is not important
 in locating the instability strip, but only that the effective
temperature may not
be reflecting the temperature in the driving regions due to accretion
heating
in the surface layers.
Arras et al.
(2006) show that the temperature in the driving zone, log g and the He
abundance are all important for accreting white dwarfs.

In order to explore the physical parameter space occupied by
 accreting pulsators (Arras et al. 2006),
 and to attempt mode identification
through comparison of UV to optical amplitudes (Robinson et al. 1995),
we proposed further study of
three additional known pulsators with STIS.
 After the proposal was
accepted, STIS was taken out of service but we were able to switch our program
to the Solar Blind Channel (SBC) which has the same wavelength coverage,
albeit much lower resolution and no TIME-TAG mode of photon counting. The
three objects are SDSSJ013132.39-090122.3 (Szkody et al. 2003; Warner \&
Woudt 2004), SDSS J161033.64-010223.3 (Szkody et al. 2002; Woudt \& Warner
2004) and SDSS J220553.98+115553.7 (Szkody et al. 2003; Warner \& Woudt 2004).
Throughout the rest of this paper, we will refer to these objects as
SDSSJ0131, SDSSJ1610 and SDSSJ2205. A summary of the orbital periods,
visual brightness and optical pulsation periods is provided for these
3 systems in Table 1. The SDSS spectra are shown in Figure 1.

\section{Observations and Reductions}
\subsection{HST Ultraviolet Observations}

The HST UV data were acquired using the prism
PR110L and the Solar Blind Channel on the Advanced Camera for
Surveys (ACS) to provide
UV spectra from approximately 1245 to 1800\AA. Due to the prism,
the dispersion varied from about 1.5\AA\ pxl$^{-1}$ at the far UV end to about
25\AA\ pxl$^{-1}$
at the longest wavelengths.
Each system was observed for 5 HST orbits using 61s integrations in ACCUM mode. The
dead time between observations was 40s so the time resolution of the spectra
are 101s. The first orbit had 26 integrations (due to the initial overhead
of setting up on a target) and the remaining 4 orbits contained 29 integrations.
Thus, the total time on each source consisted of 142 integrations of 61s
each or 8662s.

The UV data were analyzed using tools available under STSDAS and
pyraf (aXe14). The primary target was extracted using a variety of extraction
widths to optimize the S/N of the resulting spectra and light curves. For
the spectra, a wide extraction of 17 pixels was used and the resulting
142 spectra were co-added to produce a final spectrum. For the light curves,
a smaller extraction width produced the optimum (largest) pulse signal.  This
optimum extraction width was determined to be 9, 12 and 4 pixels for SDSSJ0131, 1610 and
2205 respectively. The fluxes were then added across
wavelength for each
individual spectrum to produce photometric points
throughout the 5 orbits for a light curve that could be analyzed
for periodicity using Discrete Fourier transforms. For the 2 brightest
systems (SDSSJ0131 and 1610), the spectra at the peaks
and troughs of the resulting light curves were then individually combined
into
peak and trough summed spectra, as any difference in temperature between
these spectra would help constrain the change in temperature during a
pulsation cycle of the dominant mode.

\subsection{Optical Observations}

In order to prevent excessive UV light from entering the ACS detectors,
STScI required continual ground observations prior to and during the
HST observations to insure that the objects were not going into a dwarf
nova outburst. These monitoring observations were kindly provided by a large
group of worldwide amateurs and professionals (from AAVSO and
ROTSE and scientists at observatories for other programs). All 3 systems
remained at quiesence throughout the planning and execution of the
observations.

Coordinated simultaneous optical observations were achieved for
SDSSJ1610 in order to obtain the amplitude and period of the optical
pulsations. The 3.5m telescope at Apache Point Observatory (APO)
was used with a B filter on the CCD camera SPIcam
along with the Nordic Optical Telescope (NOT) 2.56m telescope and B filter on
the Faint Object Spectrograph and Camera (ALFOSC) on the night of
June 30/July 01. APO used an integration time of 20s while NOT used 14.1s.
Additional data were obtained on the 2m Himalayan Chandra Telescope (HCT)
on the nights preceding and following the HST observation. These observations
were accomplished with no filter and 30s integeration times.

To check the stability of periods for SDSSJ0131, additional APO data
were obtained on 2005 Dec 1 and 5 and also on 2006 Jan 30, using the imaging CCD on the
Dual Imaging Spectrograph (DIS) with no filters.
DIS utilizes a dichroic that splits the light at 5550\AA\ so that the blue
and red portions of the beam are then incident on two distinct CCD cameras. The
light curves obtained using the blue CCD camera are used in this paper, sensitive
in the wavelength range 3500-5550\AA. Windowing was used to read a small portion of the
CCD in order to reduce the read out time and obtain a suitable time resolution.
A standard IRAF\footnote{{IRAF (Image
 Reduction and Analysis
Facility) is distributed by the National Optical Astronomy Observatories, which
are operated by AURA,
Inc., under cooperative agreement with the National Science Foundation.}}
reduction to extract sky-subtracted light curves from the CCD frames using weighted
circular aperture photometry (O'Donoghue et al. 2000) was employed.
The optical light curve of the target star was divided by a sum of one or more brighter comparison
stars and converted to the same fractional
amplitude scale and the times converted to Barycentric
Coordinated Time (Standish 1998). A Discrete Fourier
Transform (DFT) was then computed for all the optical light curves up to the Nyquist frequency.

Additional optical data for SDSSJ0131 over a longer timescale were obtained
from the 1.9m Radcliffe telescope at the Sutherland site of the South African
Astronomical Observatory (SAAO), using the University of Cape Town
CCD Photometer (UCTCCD; O'Donohue 1995) with no filter. Data were acquired during
several nights in 2003 July, August and September; 2004 September and November
and 2006 August. Fourier transforms were computed for each
night of data, as well as combined FTs for each month.

A summary of the HST and ground-based observations is given in Table 2.

\section{Light Curves and Pulsations}

The summed photometry from each HST spectrum was analyzed in a similar manner
as the DIS data.
Figure 2 shows a light curve for a single HST orbit for each
system; the pulsation is apparent in each case. The combined data from all
5 orbits were then
analyzed with DFT routines to obtain the quantitative periods and amplitudes.
Figure 3 shows the amplitude plots and Table 3 summarizes the resulting periods
and amplitudes. The APO, NOT, and HCT data were analyzed in the same way and
the results shown in Table 3 and Figure 4.

The optimum dataset exists for SDSSJ1610 since we can compare periods and
amplitudes from simultaneous UV and
optical data observations.
Figure 2 shows that the UV pulse is most clearly resolved for this system.
Table 3 shows that the observed UV and optical
periods are identical, while the UV amplitudes are
increased by 2-6 times over those of the optical. Our optical results are
consistent in period and amplitude with the 2 independent periods
that were evident in the
past data of Woudt \& Warner (2004) as listed in Table 1. The observed
304s period is a harmonic of the 608s period.

For pulsating white dwarfs, the identification of the excited
non-radial g-modes
can provide the total mass of the star as well as the
mass of the H layer (Kawaler \& Hansen 1989).
Each of the eigenmodes that can be excited in the star is described by a set of indices:
 $k$ is the radial quantum number that gives the number of nodes between the
surface and the center of the star,
 $\ell $ is the azimuthal quantum number that gives the number of nodes on the surface,
 and $m$ is the number of nodes along the meridian; it is used to describe the
 frequency if the spherical symmetry is lost due to rotation or a magnetic field.
 We use spherical harmonics (${{\mathrm{Y}}^{\ell }}_m$) to describe these eigenmodes.
 This identification
of the quantum numbers $k$, $\ell $,
and $m$ for each observed period
is not easy, as it involves matching observed periods with predictions from
models (with many free parameters). Robinson et al. (1995)
pioneered a method of determining the $\ell $ value
based on the change in amplitude as a function of wavelength
due to limb darkening and the modified geometric cancellation (Robinson,
Kepler \& Nather 1982).
 Limb darkening effectively reduces the viewing area of the stellar disk,
 and this reduction in area depends on wavelength.
 At UV wavelengths, the increased limb darkening
 decreases the contribution of zones near
the limb, and modes of $\ell $=3 are canceled less effectively in the UV
compared to $\ell $=1 or 2.
However, this does not hold true for $\ell $=4 modes, which do not show a significant
change in amplitude as a function of wavelength.

 Robinson et al. (1995), Nitta et al. (2000) and Kepler et al. (2000)
 calculated
amplitudes in the UV for different values of $\ell $.  To attempt to
constrain the $\ell $ value for the 608s period observed in SDSSJ1610, we
determined the amplitudes for this period
for four different wavelength regions: 1245-1360\AA,
1360-1500\AA, 1500-1640\AA, and 1640-1800\AA. The effective wavelengths
of these regions were computed using the best-fit white dwarf model
(section 4). We also computed the amplitudes for 20 individual wavelength bins
but the
resulting error bars were too large to be useful. Figure 5 shows the
observed pulse amplitude ratios for our four wavelength regions
 along with the theoretical
amplitude ratio for single DA white dwarf stars using Koester's atmosphere
models (Finley, Koester \& Basri 1997). The top panel shows the model
calculations for $\ell $=1 to 4 modes for log g=8, T$_{eff}$=14,500K (top) and 12,500K
(bottom).
 While neither plot can
fit all the wavelengths, the $\ell $=1 mode with T$_{eff}$=12,500K is a
good fit to all but the shortest wavelength and it appears that high
order modes ($\ell $=3,4) can be ruled out.
However, since
the temperatures for accreting white dwarfs are quite different than for DAVs
(see below), the simple non-interacting DA
model may not be applicable. In addition, since the disk may
cast a shadow on the equatorial regions of the white dwarf, the limb
darkening and geometric cancellation may be different than that for single
white
dwarfs.

It is also interesting that the peaks in the FT of SDSSJ1610 show
no splitting (Figure 4), even though the resolution is $\sim$10$^{-5}$ Hz
(vsini$\sim$0.5 km s$^{-1}$),
whereas fitting of line widths in HST spectra
have shown velocities about 50-100 km s$^{-1}$ (Sion et al. 1994) for accreting
white dwarfs. However, there may be some process that is suppressing some of the modes.
Long
term monitoring of GW Lib (van Zyl et al. 2004) showed  clusters of
periods separated only by about 1 $\mu$Hz whose origin is not clear. It
will take a much longer combined run on SDSSJ1610 to tell if this is also
the case in this system.

For the other two objects, where simultaneous optical light curves could not be
obtained, we can only compare the observed UV periods and amplitudes with
available optical values. For SDSSJ2205, the single observed
UV period of 576s matches one of the  previously observed optical periods
noted by Warner
\& Woudt (2004), and the UV amplitude is about 6 times the optical value. The
strongest period (330s) observed in the optical by Warner \& Woudt is
not visible in the UV.

The brightest system (SDSSJ0131) shows no UV pulsation at the
highest amplitude period (595s) previously evident in the optical
data published in  Warner \& Woudt
(2004). Their other 2 optical periods (260s and 335s) are also not
apparent in the SBC data.
Instead, a shorter period of 213 s near the Nyquist frequencey
is evident in the HST data
with an amplitude near 80 mma.
The 213s period
is obvious, although just barely resolved, in the SBC light curve (Figure 2).
This is the shortest period yet seen in an accreting pulsator.
Our extended optical coverage on this object with APO in the months following the HST
observation and with SAAO in the years preceding and following the HST
(Table 2) provides a handle on the stability of the observed periods.
Figure 6 shows the DFT of the 2006 January data while Figure 7 shows all
the monthly combined runs from the SAAO (Table 4 lists the observed
frequencies and periods from the SAAO runs). It is clear that the pulsation
spectra are highly variable, with longer periods most prominent in the
runs of 2003 (Warner \& Woudt 2004 use data from 2003 September), while
the 2004 runs show only the short period seen in the 2005 HST data.  Then, in
2006 January (Figure 6) both the long period (near 600s) and the short (213s)
period are evident, and in 2006 August (Figure 7), these are both still
present, along with an even longer period (1130s) that is similar to one
seen in 2003 Aug.
While
changes in pulsation spectra are common in cool non-interacting ZZ Ceti
stars on timescales of months and even days,
it is not obvious what is to be
expected with these hotter pulsators. Long term monitoring of GW Lib
(van Zyl et al. 2004) does show that its pulsation amplitudes are unstable
as well. The 2 periods near 650 and 370s remain visible
in all runs (including the HST data), while other periods appear and become
invisible in other runs.
In SDSSJ0131, it appears that
all periods show large amplitude variations. Comparing the amplitude of the 213s period in
the UV with that seen in the optical gives a ratio of about 6, similar to
that of SDSSJ1610 and 2205.

\section{Spectral Fits}

The UV spectra of low mass transfer rate CVs are a combination of
the underlying white dwarf, the accretion disk and a source of emission
lines (likely an accretion disk chromosphere). To model the observed
SBC spectra, we employed a procedure similar to our analysis of STIS
data on similar systems (e.g. G\"ansicke et al. 2005). This involved using
Hubeny white dwarf LTE models TLUSTY195 and SYNSPEC46 (Hubeny \& Lanz 1995)
in a grid
of temperatures, gravities and abundances to create a best fit to the
spectrum. Due to the low resolution of the SBC and the past results which were
all consistent with log g=8, we fixed the log g at this value and used 0.01
solar abundance to fit the best temperature white dwarf. The constraints on
the fit include that the white
dwarf must provide the best match to the UV continuum shape, especially the broad
Ly$\alpha$ line, and its optical flux must fall below the observed optical
fluxes. Figure 8
shows the model results for a range of white dwarf temperatures (10,000K to
20,000K) compared to the observed HST and SDSS spectra of the brightest
system SDSSJ0131. It is immediately clear that the temperature typical
of non-interacting
ZZ Cet pulsators ($\sim$12000K) is too cool to fit the UV spectrum. A temperature
of 14,500K is derived from the best fit. This temperature white dwarf extrapolated to
optical wavelengths produces a $\it g$ magnitude of 19.2, well below the
observed SDSS $\it g$
mag of 18.3. In addition to the white dwarf, there is some continuum source
(the disk) that produces about 30\% of the light across the spectrum. This
is especially evident in the core of Ly$\alpha$ which should be zero for
a high gravity white dwarf.
As there is no good model of a non-steady
state disk at these low mass transfer rates, we added this continuum
component as a simple black body (power laws were tried with similar results),
used simple Gaussians to fill in the emission lines and redid the fits with
the two components. The resulting best fit for SDSSJ0131 is shown in Figure
9 and the results summarized in Table 5. A similar procedure produced the
best fits for SDSSJ1610 and SDSSJ2205 (Figures 10 and 11 and Table 5).

The spectra that produced the largest amplitude pulse were also added and fit
with
this procedure. These spectra had higher S/N but less overall flux. Thus,
the shape of the spectrum may be better defined but the total fluxes are
not correct for distances, etc. We also list these temperature fits as
T$_{optext}$ in Table 5
as a measure of the error of our temperature fits.

We also attempted to fit the difference between the peaks of the
pulsations and the troughs for the two brightest sources SDSSJ0131 and
SDSSJ1610. The spectra of the peak points in the light curves were summed
to produce one total peak spectrum
and then the troughs were summed to produce a total trough spectrum.
The resulting fits to the peak and trough spectra showed
no change in the white dwarf temperatures in either case,
which is not surprising
given that the uncertainties of our fits are on the order of
1000K.

The temperatures of the white dwarf in all 3 systems are similar,
close to 15,000K and much hotter than the temperatures of the DAV
pulsators. These temperatures are also very similar to that derived for
GW Lib (Szkody et al. 2002). Because we had used a two-temperature white dwarf
fit for GW Lib, rather than a white dwarf + BB, we redid the
fits to the STIS data of GW Lib using the approach here. The result
produces a best fit with T$_{wd}$=15,400K and T$_{BB}$=12,000K but
this fit is not as good as our past fit with 2 white dwarf components of
13,300K and 17,100 covering 63\% and 37\% respectively
of the white dwarf surface. Further confirmation that the two temperature white dwarf
is correct for GW Lib comes from inspection of its STIS spectrum. This
shows that the core
of Ly$\alpha$ does go down to zero flux, indicating that the white dwarf, rather
than a second component such as the disk, contributes all the UV flux. A
comparison of the single temperature white dwarf fit (14,700K) with that of
the WD+BB also shows that adding in a second component only changes the
derived temperature of the white dwarf by less than 1000K.

Thus, we now have secure results that four of the accreting ZZ Ceti stars
in CVs are hotter than single pulsators. On the other hand, HS2331+3905
is also secure in having a white dwarf temperature of 10,500K (see
Fig. 13 in Araujo-Betancor et al. 2005). While the UV emission lines in
HS2331+3905 are much stronger than in the four objects that have hot white
dwarfs (likely partly due to the weak white dwarf continuum), and
there are continuum variations which might imply a higher
inclination, the fact remains that the white dwarf pulsations are visible
in HS2331+3905 so the white dwarf light is prominent and it is cool.
In contrast to our three SDSS sources, all of which have UV fluxes greater
than the optical as in Figure 8, HS2331 has larger optical than UV fluxes,
and a distinct rise in flux longward of 1600\AA\ which pins down the
white dwarf temperature to its cool value.

Since accreting white dwarfs are known to show UV absorption lines of
Si, C and other metals, it is clear they do not have pure H atmospheres
(Sion 1999). Thus, perhaps it is not unexpected that the instability strip
is not the same as for ZZ Ceti stars. For accreting model white dwarfs
with a high He abundance ($>$0.38), Arras, Townsley \& Bildsten (2006)
find an additional hotter instability strip at $\sim$15,000K for low mass
white dwarfs due to \ion{He}{2} ionization.
 Thus, they
infer that HS2331+3905 has a low mass white dwarf while GW Lib (and hence
SDSSJ0131, SDSSJ1610 and SDSSJ2205) should have highly evolved donor stars and more massive
white dwarfs.

\section{Conclusions}

Our low resolution light curves throughout five HST orbits for our
three white dwarf accreting pulsators all have increased pulsation amplitudes
in the UV compared to the optical, consistent with $\ell $=1 modes.
The simultaneous optical/UV data
for SDSSJ1610 showed identical periods in both wavelength regions, while
SDSSJ0131 and SDSSJ2205 showed one of three periods evident in the optical
at other times. The long term monitoring of SDS0131 shows that all pulsation
periods come and go, indicating a high level of instability for this system.

The summed UV spectra reveal hot white dwarfs in all three systems, similar
to past results on GW Lib but contrary to the lone cool accreting white dwarf
pulsator HS2331+3905. Based on just these five systems with well-determined
white dwarf temperatures from the UV, it appears that there is a wide
range in the instability strip for accreting systems, with most accreting
pulsators in a
regime that is hotter than for non-accreting ZZ Ceti stars. Whether this is due to
a difference in the white dwarf mass and/or He composition provided by an
evolved donor as proposed by
Arras, Townsley \& Bildsten 2006 can be confirmed if the white dwarf
masses and/or the
composition of the donor can be determined. As there is no evidence of
a donor star out to 9000\AA\ in the SDSS spectra and the systems are
generally faint, the donor will be difficult to characterize. Since the
absorption lines of the white dwarf are difficult to measure in the optical
with the contaminating Balmer emission, the best approach may be the use of
high resolution UV (the Cosmic Origins Spectrograph) time-resolved data
in the future to obtain the mass of the white dwarf, although the unknown inclinations will
create some uncertainty.

\acknowledgments

We are very grateful to the many observers who monitored our objects
to insure the safety of the UV detectors and allow our
observations to take place, including Ms. Bama, Dick Campbell, Dean Chandler, Katy Garmany
(and TLRBSE teachers), Bill Goff, Bernard Heathcote, Arne
Henden, Santosh Joshi, Seung-Lee Kim, Mercedes Lopez-Morales, David Mary,
John W. McAnally, Aaron Price, Chuck Pullen, ROTSE observers,
Patrick Schmeer, and D. E. Winget. We also kindly acknowledge Denise Dale and Ewald
Zietsman for the observations of SDSS J0131 taken at the SAAO.
This research was supported by NASA grant GO-10233.01A and through the
Hubble Fellowship grant HST-HF-01175.01-A, both awarded from the Space
Telescope Science Institute which is operated
 by the Association of Universities for Research in Astronomy, Inc., for NASA,
 under contract NAS 5-26555.
BTG was supported by a PPARC Advanced Fellowship.
The NOT data were taken using the ALFOSC, which is owned by
the Institute de Astrofisica de Andelucia (IAA) and operated by the Nordic
Optical Telescope under agreement between IAA and the NBIfAFG of the
Astronomical Observatory of Copenhagen.

redpajama_set_name: RedPajamaArXiv


LOS ANGELES (AP) — A reward for information that solves the fatal shooting of a camper in Southern California"s Malibu Creek State Park has grown to $15,000.
City News Service reports the Los Angeles County Board of Supervisors added $10,000 on Tuesday.
The city of Malibu previously posted a $5,000 reward in the case of 35-year-old Tristan Thomas Beaudette, who was shot in the head June 22 while camping with his two young daughters. The pharmaceutical scientist was inside a tent at the time.
The park sprawls over a large area of wilderness in the Santa Monica Mountains north of the city of Malibu. A spate of unsolved shootings have occurred in the area dating back to 2016.


Usually a new firmware being made available a good thing. New features are added and bugs are fixed. But this is not the case when you cannot get the firmware update to apply and this message is continually displayed every time I turned on the TV and came up again every 20 minutes while watching TV. It was extremely annoying to constantly be interrupted by a useless message.
This wouldn't normally be that big of an issue, but this message displayed every time I turned on the TV and came up again every 20 minutes while watching TV. It was extremely annoying to constantly be interrupted by a useless message.
I disabled firmware updates in the support menu, but the message was continuously displayed.
I permanently disconnected the network connection, but the message still continuously displayed.
I did a full reset of all settings.
I called LG tech support for help, and they provided no solution, other than for me to pay for a technician to come to my house and look at the TV, although they didn't know what the technician could do to fix it.
Having tried every reasonable solution to solve this issue, I was desperate for a solution. It finally dawned on me…the message doesn't specifically say "LG TV Firmware Update Available"…this may not be an LG TV message. I have a Roku streaming box that's connected to a Denon AVR3312CI receiver that's connected to a LG TV. All three of these devices produce video overlays. All three of them have update-able firmware.
Sure enough, going through the Denon menus, there was a firmware update available. Problem solved.
Or even better, it would have automatically applied the firmware update itself without putting the bourdon of firmware maintenance on me.
It's a lesson learned for me – never assume your perception of context is the only one possible, when troubleshooting or when creating something new.


text:
Dismantling the AUT64 Automotive Cipher
Christopher Hicks, Flavio D. Garcia, David Oswald
AUT64 is a 64-bit automotive block cipher with a 120-bit secret key used in a number of security sensitive applications such as vehicle immobilisation and remote keyless entry systems. In this paper, we present for the first time full details of AUT64 including a complete specification and analysis of the block cipher, the associated authentication protocol, and its implementation in a widely-used vehicle immobiliser system that we have reverse engineered. Secondly, we reveal a number of cryptographic weaknesses in the block cipher design. Finally, we study the concrete use of AUT64 in a real immobiliser system, and pinpoint severe weaknesses in the key diversification scheme employed by the vehicle manufacturer. We present two key-recovery attacks based on the cryptographic weaknesses that, combined with the implementation flaws, break both the 8 and 24 round configurations of AUT64. Our attack on eight rounds requires only 512 plaintext-ciphertext pairs and, in the worst case, just 237.3 offline encryptions. In most cases, the attack can be executed within milliseconds on a standard laptop. Our attack on 24 rounds requires 2 plaintext-ciphertext pairs and 248.3 encryptions to recover the 120-bit secret key in the worst case. We have strong indications that a large part of the key is kept constant across vehicles, which would enable an attack using a single communication with the transponder and negligible offline computation.
IACR Transactions on Cryptographic Hardware and Embedded Systems
https://doi.org/10.13154/tches.v2018.i2.46-69
Conference on Cryptographic Hardware and Embedded Systems 2018 - Amsterdam, Netherlands
Duration: 9 Sep 2018 → 12 Sep 2018
Hardware and software reverse engineering
10.13154/tches.v2018.i2.46-69Licence: Creative Commons: Attribution (CC BY)
Hicks_et_al_Dismantling_AUT64_Automative_CipherFinal published version, 987 KBLicence: Creative Commons: Attribution (CC BY)
Dive into the research topics of 'Dismantling the AUT64 Automotive Cipher'. Together they form a unique fingerprint.
Cryptography Engineering & Materials Science 100%
Transponders Engineering & Materials Science 73%
Authentication Engineering & Materials Science 52%
Recovery Engineering & Materials Science 41%
Communication Engineering & Materials Science 30%
Hicks, C., Garcia, F. D., & Oswald, D. (2018). Dismantling the AUT64 Automotive Cipher. IACR Transactions on Cryptographic Hardware and Embedded Systems, 2018(2), 46-69. https://doi.org/10.13154/tches.v2018.i2.46-69
Hicks, Christopher ; Garcia, Flavio D. ; Oswald, David. / Dismantling the AUT64 Automotive Cipher. In: IACR Transactions on Cryptographic Hardware and Embedded Systems. 2018 ; Vol. 2018, No. 2. pp. 46-69.
@article{c7b88488513c496188650f9e2fa53077,
title = "Dismantling the AUT64 Automotive Cipher",
abstract = "AUT64 is a 64-bit automotive block cipher with a 120-bit secret key used in a number of security sensitive applications such as vehicle immobilisation and remote keyless entry systems. In this paper, we present for the first time full details of AUT64 including a complete specification and analysis of the block cipher, the associated authentication protocol, and its implementation in a widely-used vehicle immobiliser system that we have reverse engineered. Secondly, we reveal a number of cryptographic weaknesses in the block cipher design. Finally, we study the concrete use of AUT64 in a real immobiliser system, and pinpoint severe weaknesses in the key diversification scheme employed by the vehicle manufacturer. We present two key-recovery attacks based on the cryptographic weaknesses that, combined with the implementation flaws, break both the 8 and 24 round configurations of AUT64. Our attack on eight rounds requires only 512 plaintext-ciphertext pairs and, in the worst case, just 237.3 offline encryptions. In most cases, the attack can be executed within milliseconds on a standard laptop. Our attack on 24 rounds requires 2 plaintext-ciphertext pairs and 248.3 encryptions to recover the 120-bit secret key in the worst case. We have strong indications that a large part of the key is kept constant across vehicles, which would enable an attack using a single communication with the transponder and negligible offline computation. ",
keywords = "Automotive security , Hardware and software reverse engineering ",
author = "Christopher Hicks and Garcia, {Flavio D.} and David Oswald",
doi = "10.13154/tches.v2018.i2.46-69",
journal = "IACR Transactions on Cryptographic Hardware and Embedded Systems",
note = "Conference on Cryptographic Hardware and Embedded Systems 2018 ; Conference date: 09-09-2018 Through 12-09-2018",
Hicks, C, Garcia, FD & Oswald, D 2018, 'Dismantling the AUT64 Automotive Cipher', IACR Transactions on Cryptographic Hardware and Embedded Systems, vol. 2018, no. 2, pp. 46-69. https://doi.org/10.13154/tches.v2018.i2.46-69
Dismantling the AUT64 Automotive Cipher. / Hicks, Christopher; Garcia, Flavio D.; Oswald, David.
In: IACR Transactions on Cryptographic Hardware and Embedded Systems, Vol. 2018, No. 2, 08.05.2018, p. 46-69.
T1 - Dismantling the AUT64 Automotive Cipher
AU - Hicks, Christopher
AU - Garcia, Flavio D.
AU - Oswald, David
N2 - AUT64 is a 64-bit automotive block cipher with a 120-bit secret key used in a number of security sensitive applications such as vehicle immobilisation and remote keyless entry systems. In this paper, we present for the first time full details of AUT64 including a complete specification and analysis of the block cipher, the associated authentication protocol, and its implementation in a widely-used vehicle immobiliser system that we have reverse engineered. Secondly, we reveal a number of cryptographic weaknesses in the block cipher design. Finally, we study the concrete use of AUT64 in a real immobiliser system, and pinpoint severe weaknesses in the key diversification scheme employed by the vehicle manufacturer. We present two key-recovery attacks based on the cryptographic weaknesses that, combined with the implementation flaws, break both the 8 and 24 round configurations of AUT64. Our attack on eight rounds requires only 512 plaintext-ciphertext pairs and, in the worst case, just 237.3 offline encryptions. In most cases, the attack can be executed within milliseconds on a standard laptop. Our attack on 24 rounds requires 2 plaintext-ciphertext pairs and 248.3 encryptions to recover the 120-bit secret key in the worst case. We have strong indications that a large part of the key is kept constant across vehicles, which would enable an attack using a single communication with the transponder and negligible offline computation.
AB - AUT64 is a 64-bit automotive block cipher with a 120-bit secret key used in a number of security sensitive applications such as vehicle immobilisation and remote keyless entry systems. In this paper, we present for the first time full details of AUT64 including a complete specification and analysis of the block cipher, the associated authentication protocol, and its implementation in a widely-used vehicle immobiliser system that we have reverse engineered. Secondly, we reveal a number of cryptographic weaknesses in the block cipher design. Finally, we study the concrete use of AUT64 in a real immobiliser system, and pinpoint severe weaknesses in the key diversification scheme employed by the vehicle manufacturer. We present two key-recovery attacks based on the cryptographic weaknesses that, combined with the implementation flaws, break both the 8 and 24 round configurations of AUT64. Our attack on eight rounds requires only 512 plaintext-ciphertext pairs and, in the worst case, just 237.3 offline encryptions. In most cases, the attack can be executed within milliseconds on a standard laptop. Our attack on 24 rounds requires 2 plaintext-ciphertext pairs and 248.3 encryptions to recover the 120-bit secret key in the worst case. We have strong indications that a large part of the key is kept constant across vehicles, which would enable an attack using a single communication with the transponder and negligible offline computation.
KW - Automotive security
KW - Hardware and software reverse engineering
U2 - 10.13154/tches.v2018.i2.46-69
DO - 10.13154/tches.v2018.i2.46-69
M3 - Conference article
JO - IACR Transactions on Cryptographic Hardware and Embedded Systems
JF - IACR Transactions on Cryptographic Hardware and Embedded Systems
T2 - Conference on Cryptographic Hardware and Embedded Systems 2018
Y2 - 9 September 2018 through 12 September 2018
Hicks C, Garcia FD, Oswald D. Dismantling the AUT64 Automotive Cipher. IACR Transactions on Cryptographic Hardware and Embedded Systems. 2018 May 8;2018(2):46-69. https://doi.org/10.13154/tches.v2018.i2.46-69

redpajama_set_name: RedPajamaCommonCrawl


Image Title: Diy Industrial Hand Blown Glass Lighting Energy Saving Art Pertaining To Designs 10. Post Title: Blown Glass Lighting. Filename: diy-industrial-hand-blown-glass-lighting-energy-saving-art-pertaining-to-designs-10.jpg. Image Dimension: 739 x 738 pixels. Images Format: jpg/jpeg. Publisher/Author: Brody Ruecker. Uploaded Date: Wednesday - January 23rd. 2019 00:42:15 AM. Category: Architecture. Image Source: digsdigs.com. KEEP Hand Blown Glass Lighting Regarding Decor 1. Artisan Blown Glass Lighting Hammerton Studio With Remodel 0. Tom Dixon To Launch Hallucinogenic MELT Lamps During Milan Design With Regard Blown Glass Lighting Idea 12. Fontana Arte Bolla Blown Glass Suspension Light 51cm Panik Design Intended For Lighting Inspirations 3. Diy Industrial Hand Blown Glass Lighting Energy Saving Art Pertaining To Designs 10. Photos HGTV Within Blown Glass Lighting Prepare 13. Artisan Blown Glass Lighting Hammerton Studio Inside Remodel 9. 15 Blown Glass Pendant Lighting Ideas For A Modern And Sleek Glow Within Design 4. Tiny Bubbles Glass Pendant Light Artisan Crafted Lighting Pertaining With Regard To Blown Decor 15. Romantic Creative Amber Art Glass Lamp Chihuly LED Handmade Blown With Lighting Plans 11.


The Under Your Spell underwired mini dress is designed in a luxurious metallic fabric embellished with decorative rhinestones. Plus, our sculpted cups shape and enhance your bust for an unforgettable look. What more could you wish for?


This activity focuses on more advanced preschool matching. The objects are not an exact copy of the photo so children need to carefully observe details to match correctly. Children problem solve by looking at distinctive attributes that they can see on both the object and the photo. Usually they will start by color and eliminate pictures that do not share the same color. They can also look at shapes, patterns and details. They might ask themselves "what fish has spots?" or "which fish is long and skinny?". Most likely they will notice more than one fish with spots and have to look at another attribute. Recognizing these little details helps a child grow their category knowledge and learn new vocabulary!
- 12 laminated cards professionally printed on 100# cardstock and laminated with 5 mil lamination. The cards are classroom tough. Cards are 2.6"x 2.5"
12. Bird Match - 7 miniature plastic Safari LTD bird figurines. (approx 2-3" long) and 7 laminated cards professionally printed on 100# cardstock and laminated with 5 mil lamination. The cards are classroom tough. Cards are 2.6"x 2.5"
14. Desert Animals - 11 Animals (2"- 3" Long) Rattlesnake, saguaro cactus, big horn ram, bobcat, road runner, coyote, armadillo, mountain lion, horned lizard, scorpion.


Earn an Associate's Degree in Animal Care plus a Bachelor's Criminal Justice in the same amount of time as a Bachelor's Degree alone!
Describe the administration of justice with specialized knowledge of related content areas including, but not limited to, police, courts, and corrections.
Identify the theories of crime causation, responses to crime, and the implications and application for public policy.
Interpret, analyze, and draw conclusions from qualitative and quantitative data in a social science context and communicate effectively using scholarly sources on topics relating to social problems and criminal justice.


Everyone knows that Santa's workshop is at the North Pole, but did you know that the North Pole isn't in the Arctic? The North Pole along with Santa's Workshop is actually just west of Colorado Springs at the base of Pikes Peak!
Today as a special treat, the grandparents (Gram, Pop Pop, and Grandpa) are taking Ian, Alli, and their cousin. My kids were excited when I told them where they were going. Ian especially was excited to meet Santa.
In operation since 1956, the North Pole has been around for over 60 years! I remember my parents taking me and my brothers here years and years ago. Now I was really excited to see my parents taking my kids back to that same park.
Before they left, I told Ian one of my favorites was the giant peppermint slide. You grab a burlap sack, climb 4 stories, and slide your way down.
Turns out it ended up being one of Ian's favorite rides of the day too. My dad said at one point, he went 6 times in a row, sliding down then sprinting up the stairs to have another go.
The rides here at the North Pole are fairly basic, but the kids couldn't care less. With height requirements that are between 32" and 42", Ian and Alli were able to ride just about everything.
No surprise that she found the pink and purple one.
Ian and Alli's Uncle Patrick on that same ride, circa 1993.
Even better than Autopia back at Disneyland since he can drive all by himself!
Ian's daddy Joe driving a similar car back in 1984.
I would have been around 5 or 6 when my parents brought me here, and I remember loving the Tilt-a-Whirl. It was an early introduction to some of the wildness of the roller coasters I'd end up loving later.
So it was no surprise that my roller coaster loving little boy also had a great time riding the Tilt-a-Whirl.
Alli loves her horses. Add some bells that you can jingle and you've got a winner of a ride.
Their Uncle Jon and their daddy riding the same ride, around 1984.
Their cousin isn't tall enough just yet, but she will be soon enough.
And all those years ago, there were even real ponies you could ride!
When you're visiting the North Pole, you have to make time to visit the big man himself.
Ian and Alli were super excited and ran up to see Santa. He said it made his day seeing how excited they were.
When Santa asked them what they'd like for Christmas, Alli wanted "candy and a present" which Santa agreed he could do. Ian, always the creative one, asked for "candy and a statue of me" which Santa took be a statue of Ian made of candy. That one might be a little more difficult. Santa was really great with both kids and they certainly enjoyed seeing him.
Their cousin... not so much. She'll get there eventually.
After the visit with Santa, a ride on the railroad was in order.
Then a ride on the carrousel.
The two girls are headed home early to get a nap. Ian and Pop Pop stayed a little longer to keep going on rides.
For the Dive Bombers, Ian let other kids go in front of him, just so he could be the first in line on the next ride in order to get this American Flag bomber.
The lines here have been really good. Usually for rides like this, you had to only wait for one cycle and then it was your turn to ride.
Seeing these rides again makes me smile. I remember having a lot of fun on them all those years ago.
Their Uncle Jon and Uncle Patrick riding in 1993.
Uncle Patrick in 1993. I see they've all had a flashy paint job since this picture was taken.
I love how so many things are Christmas themed.
Getting a picture on Santa's sleigh.
And touching the North Pole which is actually frozen!
Ian and Alli both loved their visit to the North Pole! Thanks Gram and Pop Pop!
It was indeed a good day. Loved the pics and commentary. And pictures of you and your brothers growing up.


Extreame Savings! Up to 50% off on Bento Boxes at Dining bench, Page 5. Top brands include NutriBox, Yumbox, Bentgo, PlanetBox, & Qualitas Products. Hurry! Limited time offers. Offers valid only while supplies last.


Stretching over a land with deep roots, the 21 hectares of the Longue Tubi estate were bought by the Buisine family in 2001. agronomists, passionate about all aspects of the winegrowing arts for 34 years, they took the plunge by deciding to build a cellar in 2012 and produce their own wine. They take the greatest care of the soil and the plant.
The creation of wines that are suitable for both enlightened wine lovers and those who wish to discover the pleasures of tasting step by step.


text:
Indian Muslims face bleak future
In the aftermath of recent rhetoric offending Islam and Prophet Mohammad (PBUH) by a Bharatiya Janata party spokesperson, and despite a promising and secular constitution guaranteeing the rights and freedoms of all people regardless of religion, clashes between religions are becoming more overt in India. The current economic and sociopolitical climate, under the governance of rightwing Prime Minister Narendra Modi, forecasts a bleak future ahead for Indian Muslims, as they are already living under grueling circumstances and seen as second-class citizens.
Muslims' religious rituals and dietary habits are being attacked and even criminalized; women are banned from wearing hijab in schools, and Friday prayer is prohibited in the city of Gurgaon, along with several issues relating to Muslim personal status law. Hindu extremists are also demanding speakers no longer transmit the Muslim call to prayer.
The homes and businesses of Muslim people are being targeted and sabotaged, and their livelihoods threatened. Demands of changing Muslim names of certain cities and roadways, contesting the use of the word "halal", inflammatory media portrayals of Muslims, as well as Hindutva propaganda alleging that Muslim monuments such as Taj Mahal and Qutab Minar are originally Hindu sites, all contribute to the alienation of the Muslim people.
In addition, journalists and media personnel not adhering to the extremist national policy of Hindutva are persistently being silenced and reprimanded. The response of the Indian government to the recent offensive remarks is seen as a renewal of the image of the country and an attempt to protect its economic interests instead of an actual concrete attempt to better the reality of Muslims in India.
Due to the lack of Muslim political representation or media presence, government bodies are increasingly adopting more anti-Muslim policies. Majoritarian violence is influencing the ebb and flow of the decision-making process as the legislative and executive authorities are taking provocative measures against the Muslim community, including arrests of prominent figures.
On the political front, the Indian Congress Party, which was once on the forefront of Indian independence, is currently in shambles. The party that contributed to the writing of the constitution preformed quite weakly in local and national elections, as it failed to appeal to the masses. Other leftist parties are also restricted to certain states with very limited representation in parliament; therefore, an alternative where political parties answer the pleas of Muslims and repair the systemized political social and economic oppression is unlikely.
Furthermore, many Indian Muslims question the motives and integrity of leftist parties as they either unknowingly or purposely play into rightwing agenda. Despite reports of a number of Muslims subscribing to the rightwing party, a permanent alliance between the two is implausible as the governing party continues to taint the image of Muslim Indians and paint them as successors of violent invaders who killed Hindus and toppled temples, dividing the country.
The image of a peace-loving India that was put in place by Mahatma Gandhi is gradually deteriorating, adversely affecting in the long run hefty economic opportunities in the fields of information technology, imports, exports, health and tourism. Independent journalists are warning of the eruption of a civil war if the government fails to regulate Hindutva, while others are saying India has indeed become a Hindu state. – KUNA


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5/4(Sat) 15:00 Full More dates... More dates available!
5/18(Sat) 15:00 6 spots More dates... More dates available!
5/19(Sun) 11:00 7 spots More dates... More dates available!
いつも明るく楽しい先生のもと、 ブラジルのChristmasのお話しや、Christmasらしいお料理。楽しくておいしかったです。 ブラジルのことも、もっと知りたいと思いました。 Thank you very much. I would like to participate again. I would love to make dessert as well.
Thank you so much for having me today, I really enjoyed myself thoroughly :) I absolutely loved the menu, the way you introduced us into the session and I am sure to be back again!
Thank you for your lesson! You are so kind and anytime helped me. The food was so nice! I want to join your lesson again or I will definitely join when you have "Ouchi Gohan "!
Flavia-san is amazing!! Flavia's kitchen tools is very cute!! The plate was garnished beautifully. We made Empadinha de palmito from dough.I tried palm heart at first. It's fantastic!I really enjoyed cooking and foods and Halloween!!