text:
\section{Introduction} \label{intro}

\subsection{Magnetic Cataclysmic Variables}

Cataclysmic variable stars (CVs) are interacting binaries in which a white dwarf (WD) accretes from a companion star that overfills its Roche lobe. Polars are a type of CV featuring a WD whose magnetic field is sufficiently high  \citep[$\gtrsim 10$ MG;][] {cropper} to synchronize its own rotational period with the binary orbital period. The accretion flow from the donor star will follow a ballistic trajectory until its ram pressure is matched by magnetic pressure from the WD. Moving out of the system's orbital plane, the flow then travels along the WD's magnetic field lines until it slams into a cyclotron-emitting accretion region near one of the WD's magnetic poles. Thus, no accretion disk can form, unlike non- or weakly magnetic CVs. The magnetically channeled part of the accretion flow is commonly referred to as an accretion funnel or an accretion curtain, and the region in which the accretion flow is diverted from its ballistic trajectory is known as the threading region. \citet{cropper} and \citet{hellier} both provide detailed descriptions of polars.

Polars have several important observational characteristics resulting from the high magnetic moment of the WD. For example, the spectrum of a typical polar is dominated by single-peaked emission lines, including high-ionization lines. Intense, single-peaked He II $\lambda\ 4686$ \AA\ is a common indicator of magnetic accretion. Moreover, cyclotron emission from the accretion region can contribute a significant fraction of the system's overall optical light. Because cyclotron radiation is highly beamed, its contribution to the light curve can be highly variable as our viewing angle of the accretion region changes across the orbital period. Thus, the orbital light curves of polars can exhibit rapid, high-amplitude variations seldom seen in non-magnetic CVs.

\subsection{MASTER OT J132104.04+560957.8}

\begin{figure*}[ht!]
\epsscale{1.17}
\plotone{J1321LC.pdf}
\caption{A long light curve of J1321 obtained with Van Vleck Observatory's 60-cm Perkin Telescope, illustrating the overall stability of the double-humped structure. Nevertheless, there are noticeable cycle-to-cycle variations, including the changes in the depth of the minima. The data are unfiltered with an exposure time of 30 sec, and the overall cadence is $\sim32$ sec per image. \label{LC}}
\end{figure*}

MASTER OT J132104.04+560957.8 (hereinafter, J1321) was first detected as an optical transient by \citet{Y12} and was subsequently found to exhibit 2-magnitude optical variations with an approximate period of 1.5 hours \citep{kato}. \citet{L15} published the first spectral and photometric observations of J1321 and classified the system as a likely polar based on the detection of strong, single-peaked H, He I, and He II $\lambda\ 4686$ \AA\ emission lines. Their average spectrum revealed a curiously red continuum that peaked near 540~nm without showing any spectral features from the donor star.

The phase plot of their photometry consisted of two prominent, partially overlapping humps, each of which persists for $\sim~35$\% of the orbit. However, in several instances, the fainter of the two humps displayed extraordinary morphological variations across consecutive orbital cycles (see Fig.~ 2 in \citealt{L15}). The exact cause of the variation was never pinpointed, but it was suggestive of significant changes in the accretion geometry on timescales of just 90 minutes.

\section{New Observations}

\subsection{Simultaneous LBT Spectroscopy \& Photometry}

We obtained simultaneous spectroscopy and photometry of J1321 using the Large Binocular Telescope (LBT) in binocular mode with the Multi-Object Dual Spectrograph \citep[MODS;][]{pogge10} and the Large Binocular Camera \citep[LBC;][]{giallongo08}. The LBT observations started 2015 May 19.367 (UT) and lasted 2.1 hours, or about 1.4 orbits of J1321.

Thirty-five spectra were obtained with MODS1 (using the SX mirror) in the grating mode using a 1.0-arcsec slit. Each exposure was 120~s, and read-plus-overhead time was 100~s. The blue channel covers the wavelength range from 320~nm to 562~nm, and the red channel records 567~nm to 1000~nm. The gap in wavelength coverage is caused by a dichroic filter that divides the light into the two spectrographs.

The spectra were bias-subtracted and flat-fielded using standard reduction procedures. The two-dimensional spectra were extracted using the {\sc 2dspec} package in IRAF. Wavelength calibration was performed using an argon lamp on the blue side and a neon lamp for the red. The spectra were transformed to flux using spectra of the spectrophotometric standard star HZ~44 obtained on the same night.

As MODS1 was taking spectra using the SX mirror, the LBC-red camera was recording images with the DX mirror. LBC is a mosaic of four CCDs, but only 1000 rows of chip~2 were read to reduce overheads. An exposure time of 15.2~s combined with a readout of 20~s resulted in 204 images taken simultaneously with the MODS1 spectra. The seeing over the time series varied between 1.1~arcsec and 1.3~arcsec (FWHM). All of the images were taken through a Bessel $V$ filter, and relative photometric uncertainties for J1321 are 5~millimag.

\subsection{Additional Photometry}
\label{photometry_sec}

Between 2013 and 2017, we obtained additional time-resolved photometry with the 60-cm Perkin Telescope at Wesleyan University's Van Vleck Observatory, the 80-cm Sarah L. Krizmanich Telescope (SLKT) at the University of Notre Dame, and the 1.8-m Vatican Advanced Technology Telescope (VATT).\footnote{Some of the VATT data were previously reported in \citet{L15}.} The exposure time for the first two instruments was 30~s, with between 2 and 4~s of overhead between consecutive images. For the VATT, exposure times were generally 20~s with 12~s of readout, but for one run, we used the Galway Ultra Fast Imager to achieve 10~s exposures with negligible overhead. The Perkin and SLKT time series were unfiltered in an effort to achieve a reasonable signal-to-noise ratio; we inferred approximate $V$ magnitudes by using the $V$ magnitude of the comparison star when calculating J1321's $V$ magnitude, a bandpass which we denote in our figures as ``CV.'' The VATT data used a $V$ filter. Figure~\ref{LC} shows a representative light curve from the Perkin Telescope, covering five consecutive orbital cycles.

\begin{figure}
\epsscale{1.17}
\plotone{crts.pdf}
\caption{A seven-year phase plot of the CRTS photometry using the ephemeris in Sec.~\ref{photometry}, illustrating the long-term stability of the light curve between 2007 and 2013. To enable a direct comparison with our time-series photometry (Sec.~\ref{photometry_sec}), we plot contours of the phase plot of our data. The dark and light contours indicate the innermost 50\% and 98\% of our data at a given phase, respectively. The amplitude of the primary maximum appears to have been lower in 2007 compared to our recent time series. The three faintest observations occur at phases consistent with missing secondary maxima (see text). \label{crts}}
\end{figure}

\subsection{Availability of Data}

Our full photometric and spectroscopic dataset is freely available as supplemental online material, but we request that this work be cited should these data be used in a subsequent work.

\section{Analysis}

\subsection{Long-Term Photometric Behavior}

Our observations and those in \citet{L15} show J1321 to be in a stable high state, consistent with a stable mass-transfer rate. However, archival photometry shows that J1321 underwent a period of prolonged dormancy before transitioning into a high state at some point between 2003 and 2007. Images taken in 1953 (POSS-I O and POSS-E Red), 1983 (Quick-V Northern), 1991 (POSS-II N), 1993 (POSS-II Red), and 1994 (POSS-II Blue) show the system in a very faint state, as do SDSS images from 2003 March, when $g = 21.65$. However, between 2007 and 2013, the Catalina Real-Time Transient Survey \citep[CRTS;][]{drake} observed J1321 a total of 65 times, and during that span, it was detected in a high state exclusively. To illustrate the stability of this high state, Figure~\ref{crts} plots the CRTS data, phased according to our ephemeris. Although the CRTS data in 2007 reveal the primary photometric maximum to have been several tenths of a magnitude fainter in 2007, the observed scatter at any given orbital phase in the remainder of the data is consistent with observed cycle-to-cycle variations. Thus, the CRTS data imply that there were no major variations in the overall brightness between 2007 and 2013, and our own monitoring of J1321 show that its overall brightness has remained unchanged since 2013. Because variations in the overall brightness are directly indicative of variations in the mass-transfer rate, it follows that J1321's mass-transfer rate has been very stable since at least 2007.

\citet{ms17} studied 44 well-sampled light curves of polars observed by CRTS over a span of $\sim$10 years, and their findings provide a useful context for assessing J1321's long-term light curve. The polars in their sample show an eclectic range of behaviors, with some remaining in persistent low states, others remaining locked in bright states, and still others alternating between the two. Were J1321 included in their sample, it would clearly be classified as a high-state polar, but none of the polars examined in their paper shows a transition similar to J1321's dramatic emergence from an extended faint state into a prolonged, apparently uninterrupted high state. However, this behavior in J1321 becomes apparent only when CRTS photometry is examined alongside older data, so it is possible that some polars in their study might have undergone similar changes before CRTS coverage commenced.

\subsection{Time-Series Photometry}\label{photometry}

\begin{figure*}
\epsscale{1.17}
\plotone{missing_maxima.pdf}
\caption{Four nightly light curves showing ``missing'' secondary maxima, presented as phase plots to underscore how the missing maxima do not affect the rest of the light curve. The measurements showing the missing maxima are plotted in red. In the top-left panel, the missing maximum began at the end of the observations, and in the top-right panel, it was already underway at the start of the time series. In the bottom-left panel, the three faintest measurements are 4.5-minute bins, as J1321 was undetectably faint in individual images. That particular missing maximum shows that the system began to rise toward secondary maximum as usual between $\phi \sim 0.3-0.4$, but it then faded precipitously in comparison to the two previous cycles.
\label{secmax}}
\end{figure*}

J1321's photometric behavior during our observations was nearly identical to the general behavior described in \citet{L15}. Each photometric cycle remained dominated by two partially overlapping humps of unequal amplitude, along with two minima of different depths. The brighter of the two humps is typically one-half of a magnitude brighter than the secondary maximum.

To generate an updated ephemeris, we fit second-order polynomials to each of the observed photometric maxima and performed an O$-$C analysis on the measured times of maxima. We find that the photometric maximum follows an ephemeris of $$ T_{max}(BJD) = 2456284.8043(11) + 0.063235199(40) \times\ E.$$ The numbers in parentheses are the $1\sigma$ uncertainties on the final two digits, as determined from Monte Carlo simulations. Given J1321's classification as a polar, we presume that this period corresponds with both the binary orbital period and the WD's rotational period.

\subsubsection{``Missing'' Secondary Maxima}

Although J1321's overall behavior was consistent from night-to-night, we did observe two ``missing'' secondary photometric maxima, not including those previously reported in \citet{L15}. As noted in \citet{L15}, the secondary maximum is sporadically absent from a photometric cycle, essentially disappearing and reappearing on timescales of one orbit. While the secondary maximum usually peaks around V$\sim17$, the system drops below V$\sim$19 during a ``missing'' secondary maximum, and the customary hump-like appearance of the secondary maximum is replaced by irregular variation. Of the 45 observed secondary maxima in our data, only four are missing.\footnote{Another light curve, obtained on 30 June 2014 and shown in Fig. 2 of \citet{L15}, appears to show the very end of a fifth missing secondary maximum, but the data do not cover enough of the event to establish it conclusively as a missing maximum.} Figure ~\ref{secmax} plots these four light curves.

The missing secondary maxima do not appear to be correlated with any concomitant changes in the orbital light curve. In particular, there are no anomalies in the appearance of the primary maximum before or after a missing secondary maximum. This could indicate that the two photometric maxima are associated with different magnetic poles and that the accretion flow to one pole is less stable than the other.

\begin{figure*}
\epsscale{1.17}
\plotone{spectrum_full.pdf}
\caption{The spectra, alongside a light curve showing the simultaneous LBC photometry and the estimated $V$ magnitudes from the flux-calibrated MODS spectra. The second half of the first absorption dip is visible at the bottom of the figure near phase 0.9, and the second dip occurs one cycle later. Note the rapidly changing continuum as J1321 rises to its both of its maxima. Telluric lines are uncorrected. \label{trailedspectrum}}
\end{figure*}

\subsection{Spectra}\label{spec}

The LBT spectra show a rich assortment of single-peaked emission lines typically seen in polars, including the Balmer series, He I, and He II $\lambda$ 4686 \AA. Both the continuum and the spectral lines undergo dramatic, orbital-phase-dependent variations, the most remarkable of which is a brief reversal of the spectral lines from emission to absorption. This phenomenon is discussed in detail in section~\ref{absorption}.

The spectra provide insight into the variations in the optical light curve. During the photometric minimum, the continuum is weak and flat, with the Balmer jump in emission. As J1321 begins to rise from its minimum, the continuum begins to develop a smooth, prominent bulge, with the peak of the bulge moving blueward of 500~nm as the system brightens. After reaching its peak brightness, the system then fades to its secondary photometric minimum, when the bulge becomes less apparent and the continuum more closely resembles a sloped line that increases at shorter wavelengths. At the end of the secondary minimum, J1321 recovers to its secondary photometric maximum, and the continuum bulge becomes prominent again in the blue end of the spectrum. J1321 then fades back to its primary minimum, with the bulge disappearing completely. To illustrate these changes, we show our spectra and the simultaneous light curve in Fig.~\ref{trailedspectrum}.

We use cyclotron modeling in the following section to establish that the changes in the continuum are consistent with cyclotron beaming effects.

\subsection{Cyclotron Modeling}

The magnetic field of a polar can be estimated by identifying a set of cyclotron harmonic peaks or Zeeman lines in the spectra. Their absence in our data means that J1321's magnetic-field strength is difficult to directly measure. In polars with relatively low field strengths, a smooth, hump-shaped optical continuum results from the high-order cyclotron harmonics blending together. For example, in the low-field polars BL~Hyi \citep{schwope95} and LSQ1725-64 \citep{fuchs}, the field strength is $\sim$12~MG based on the detection of Zeeman lines, and each system shows a featureless cyclotron continuum in optical spectra.

In order to constrain the magnetic field strength of the WD in J1321, we use the homogeneous cyclotron emission model of \citet{chanmugam79} and \citet{wick85} to calculate optical spectra of accretion columns on a magnetic white dwarf. The shape of the spectrum depends on the plasma temperature, $kT$, and the magnetic field strength, $B$, which are assumed to be constant. The models also depend on the viewing angle, and a dimensionless depth parameter, $\Lambda$. The depth parameter is a combination of the optical path length, the magnetic field strength, and the electron density, and it determines the wavelength at which the accretion column becomes optically thin.

When bright, the spectra of J1321 show a smooth continuum with a broad peak between 400~nm and 500~nm, suggesting that we are seeing high harmonics blended together by a significant electron temperature. At plasma temperatures less than 10~keV, the homogeneous models predict that cyclotron harmonics should be noticeable in the spectra, even at fairly high harmonics. The smooth continuum of the LBT spectra implies a plasma temperature larger than 10~keV, and we adopt a temperature of 20~keV as did \citet{schwope95} for BL~Hyi.

\begin{figure}
\epsscale{1.25}
\plotone{cyclotron.pdf}
\caption{ Homogeneous cyclotron-emission models compared with J1321's continuum (dots) from one spectrum obtained at $\phi =0.06$, close to its photometric maximum. From that spectrum, we subtracted an average spectrum of the faintest part of J1321's orbit in order to isolate the cyclotron component. Residual emission lines were removed, and the spectrum was binned into 10~\AA\ steps. \label{cyclotron}}
\end{figure}

\begin{figure}
\epsscale{1.3}
\plotone{cyclotron2.pdf}
\caption{If the plasma temperature ($kT$) is fixed at 20~keV, it is possible hold the peak wavelength of the cyclotron spectrum constant by increasing the field strength and decreasing $\Lambda$. However, at sufficiently high field strengths (here, $B$ = 38~MG), individual cyclotron harmonics begin to appear. \label{cyclotron2}}
\end{figure}

Most of the model parameters are unconstrained in J1321, so we will simply look at how the models that fit a similar system, BL~Hyi, can be adjusted to look like J1321's cyclotron spectrum at maximum light. To isolate the cyclotron spectrum for our modeling, we selected a spectrum from $\phi = 0.06$, subtracted the average spectrum of J1321 during the faintest part of its orbit, and removed the residual emission lines. The resulting cyclotron continuum peaks at 433~nm, compared to 640~nm in BL~Hyi. Adjusting the \citet{schwope95} BL~Hyi model to achieve a significant blueward shift of the peak to match J1321 requires tweaking one or more of the four free parameters of the homogeneous models. For example, as Figure~\ref{cyclotron} shows, increasing the depth parameter $\Lambda$ by two orders of magnitude to $10^9$ while keeping $kT=20$~keV and $B=12$~MG fixed will push the model peak to 433~nm. As \citet{schwope95} also noted for BL~Hyi, the model significantly underpredicts the width of the observed cyclotron spectrum.

Due to the lack of constraints on the cyclotron modeling, many different sets of parameters can produce a smooth cyclotron spectrum that peaks near 433~nm. In particular, an increase in $B$ can be substantially offset by a decrease in $\Lambda$. For example, Figure~\ref{cyclotron2} shows that if $kT = 20$~keV, the cyclotron spectrum for $B = 18$~MG and $\Lambda = 10^7$ is almost indistinguishable from the spectrum for $B = 29$~MG and $\Lambda = 10^5$, except that the latter has a slightly wider peak. Likewise, boosting the plasma temperature to $kT=35$~keV while setting $B=12$~MG and $\Lambda = 10^7$ also results in a cyclotron spectrum that peaks at the observed wavelength.

Our models fix the viewing angle at 80$^\circ$, as was done for BL~Hyi in \citet{schwope95}. Thus, there is little room to increase the viewing angle to push the peak blueward. Without knowledge of the exact orbital inclination and the magnetic colatitude of the accretion region(s), there are too many free parameters to achieve a reasonably unique fit, and the situation would be even more underconstrained if the viewing angle were allowed to vary.

Typical values for $\Lambda$ are $\sim10^5-10^7$, and it is uncommon to find $kT > 20$ keV (e.g., UZ For, \citealt{sbt90}; BL Hyi, \citealt{schwope95}; EP Dra, \citealt{sm97}). Assuming that $\Lambda$ is in this range and that $kT = 20$~keV, we estimate the field strength to be less than $\sim$30~MG. At field strengths higher than $\sim$30~MG, individual cyclotron harmonics begin to appear (Fig.~\ref{cyclotron2}) if the other model parameters are adjusted to keep the peak of the cyclotron spectrum near 433~nm.

We conclude that we can reproduce J1321's optical continuum well enough to establish that it is a cyclotron spectrum. The large residuals from the homogeneous model suggest that a more sophisticated, heterogeneous model is needed to more accurately model cyclotron spectra in polars.

\begin{figure*}
\epsscale{1.17}
\plotone{absorption_dip.pdf}
\caption{Spectral changes in J1321 during the second absorption dip in our data, as the system rises from its minimum to its primary photometric maximum. To prevent overlap, each spectrum is offset from the previous spectrum by a constant of $0.2 \times 10^{-15}$ erg s$^{-1}$ cm$^{-2}$ \AA$^{-1}$. The absorption dip is clearly seen in H, He I, and He II. The inset plot offers a zoomed view of selected lines at the phase of maximum absorption. Additionally, the continuum develops a blueward-moving bulge as the system brightens. During the first absorption dip (not shown), more of the lines fully transitioned to absorption.\label{spectra}}
\end{figure*}

The presence of a cyclotron continuum for $\sim$85\% of the orbit implies that at least one accretion region is visible during that segment of the orbit. The absence of a cyclotron spectrum for the remainder of the orbit, without any concurrent weakening of the emission lines, points to an occultation of the accretion region(s) behind the limb of the WD. By contrast, if this were an eclipse of the cyclotron-emitting region by the secondary, there would have been at least a partial occultation of the line-forming regions. This finding accords with the fact that J1321 does not show the abrupt ingress and egress features that are almost universally observed in eclipsing polars \citep{L15}. Thus, J1321's status as a non-eclipsing system is secure, but for reasons discussed later, its orbital inclination is probably high.

\subsection{Phase-Dependent Absorption} \label{absorption}

The defining feature of J1321's spectral behavior is the appearance of deep H and He absorption lines for about one-tenth of the orbit. The LBT spectra detected two such line inversions in consecutive orbits, including the second half of the first event and the full duration of the second. As is shown in the spectra in Fig.~\ref{spectra}, for each of the optical H and He I lines, the absorption begins in the red wing of the line and quickly increases in equivalent width as it moves blueward. The emission components are quickly replaced by broad, deep absorption lines which continue to move towards shorter wavelengths. Near the end of the line inversion, the lines show P Cyg profiles with rapidly weakening absorption components. Although the wings of He II $\lambda$ 4686 \AA\ never fully transition into absorption, the line profile is bifurcated by a narrow absorption core which dips below the continuum. Like the H and He I absorption, the He II $\lambda$ 4686 \AA\ absorption component shifts blueward, but it is narrower and moves across a much smaller range of velocities. Figure~\ref{trailedspec} further illustrates this behavior with a set of trailed spectra of selected H, He I, and He II lines. As we will discuss in Section~\ref{other_polars}, emission-absorption reversals like this have been reported in only a handful of polars and are attributed to an eclipse of the accretion region by the curtain \citep{schmidt}.

\begin{figure*}
\epsscale{1.17}
\plotone{trailed_spec.pdf}
\caption{Trailed spectra of four lines. The phases are defined such that the dip occurs at $\phi = 0.9$, as it does in other polars showing the phenomenon. As noted in the text, the systemic velocity is unknown and is assumed to be 0 km s$^{-1}$ in this figure. Near $\phi = 0.0$, high-velocity, redshifted emission is more readily seen in the higher-order Balmer lines.\label{trailedspec}}
\end{figure*}

We modeled the strongest absorption lines as the sum of two independent absorption Gaussians and measured the width of the absorption by numerically determining the FWHM of the combined function. The second absorption component permits the line profiles to be skewed. H$\alpha$ always had the highest FWHM, peaking at 900 km s$^{-1}$, approximately 150-200 km s$^{-1}$ higher than He I $\lambda\lambda$ 5876 \AA, 6678 \AA\ and 7066 \AA. In the blue end of the spectrum, the FWHMs for H$\beta$ and H$\gamma$ were as high as 700-800 km s$^{-1}$, compared to a peak FWHM of 600 km s$^{-1}$ for He I $\lambda$ 4471 \AA. He II $\lambda$ 4686 \AA\ was the narrowest of the absorption lines, with a FWHM of 370 km s$^{-1}$.

One challenge with interpreting these FWHM values is that line emission from the accretion flow probably suppresses the FWHM of the absorption, such that the observed absorption features are the sum of absorption and emission components. As an illustration, Fig.~\ref{linemodel} models He II $\lambda$ 4686~\AA\ as the sum of an emission Gaussian and an absorption Gaussian. Although the superposition of these two Gaussians yields a reasonable fit to the data, the narrow absorption feature in the observed spectrum bears little resemblance to the broad, deep absorption component in the model. The actual amplitude and FWHM of the emission component are unknown during the dip, so it is impossible to reliably recover the shape of the absorption component. If the observed absorption lines are contaminated by the presence of emission, as we suspect, then measurements of the FWHM of the observed absorption features will systematically underestimate the true FWHM of the absorption component. Thus, the FWHMs that we have reported are probably lower limits for the true absorption components.

\begin{figure}
\epsscale{1.15}
\plotone{linemodel.pdf}
\caption{A profile of He II $\lambda$ 468.6 nm, shown as the superposition of two Gaussians representing emission and absorption components. Contamination from the emission component causes the observed line profile to be significantly shallower and narrower than the true absorption component. The amplitude and FWHM of the emission Gaussian were fixed to their values from a spectrum taken outside of the line inversion, while all remaining parameters were allowed to vary freely. Because changes to the parameters of one of the Gaussians can be offset by changing those of the other, this fit to the data is not unique and is meant to be illustrative. \label{linemodel}}
\end{figure}

Section~\ref{dip-discussion} explores the physical implications of the absorption event and uses it to probe the structure of the accretion curtain.

\subsection{Doppler Tomography}

We computed Doppler tomograms of the system using the inside-out projection implemented by \citet{kotze}. By plotting the highest-velocity emission at the origin of a polar plot as opposed to its circumference, this projection excels at deblending low-velocity emission while revealing high-velocity structure. The inside-out tomograms of He~II $\lambda~4686$ \AA\ and He~I $\lambda~5876$ \AA, both of which are shown in Fig.~\ref{tomo}, clearly distinguish the ballistic portion of the stream from the accretion curtain. The absence of the donor in the tomograms and trailed spectra suggests some combination of shielding by the accretion flow and insufficient spectral resolution.

\begin{figure*}
\epsscale{1.15}
\plottwo{4686_inside_out.pdf}{5876_inside_out.pdf}
\caption{Inside-out Doppler tomograms of He II $\lambda$~4686 \AA\ (left) and He I $\lambda$~5876 \AA\ (right). We adopt an inclination of 65$^{\circ}$ and a systemic velocity of 0 km s$^{-1}$. Because the time of inferior conjunction is unknown, the tomograms are phased such that the absorption dip is centered on $\phi\sim0.9.$ The inside-out projection clearly resolves the ballistic and magnetically-channeled regions of the accretion flow. In the He I tomogram, there is high-velocity emission near angle 45$^{\circ}$, as might be expected from radial inflow towards a second accreting pole on the opposite side of the WD. Although this emission is present in tomograms of other He I lines, it is weak in Balmer-line tomograms. \label{tomo}}
\end{figure*}

Properly phasing a tomogram requires knowledge of the time of the donor star's inferior conjunction. Since we did not detect spectral features from the donor, we estimate this parameter using two complementary methods. First, we presume that nearly all of the ballistic portion of the accretion stream produces detectable spectral lines, such that the start of the ballistic stream is a proxy for the position of the donor star. Accordingly, we adjusted the time of inferior conjunction until the stream originated near the donor's expected position above the origin. Second, absorption dips caused by the accretion stream in polars are generally observed near $\phi_{orb} \sim 0.9$, a tendency that can be used to crudely guess the time of inferior conjunction. The phasing from the two methods was similar, so it is likely that our tomograms are phased with reasonable accuracy, ensuring that they can be compared directly with those of other systems.

Another important consideration is the unknown systemic velocity, $\gamma$. As shown by \citep{schwope99}, adopting an incorrect value of $\gamma$ can introduce false structure into a Doppler map, so we tested a range of values for $\gamma$ between -200 km s$^{-1}$ and 200 km s$^{-1}$ to search for a dependence on $\gamma$. We found that the large-scale structure in our tomograms was substantially independent of $\gamma$ between $-200$ km s$^{-1}$ and 100 km s$^{-1}$, and we assumed a value of $ \gamma = 0$ km s$^{-1}$.

\section{Discussion}

\subsection{Missing Secondary Maxima}

The cause of the missing secondary maxima remains unclear, and there is no discernible pattern as to when they occur. It could be that a short-term fluctuation in the mass-transfer rate causes either a change in the extent of the cyclotron-emitting region (in the case of one-pole accretion) or a brief cessation of accretion onto a second accreting polecap (in the case of multipole accretion). While certain single-pole accretion geometries can produce a double-humped light curve because of the beamed nature of cyclotron emission, the fact that the primary maxima are unaffected by the missing secondary maxima suggests that the two maxima are produced in different regions, offering circumstantial support for two-pole accretion. DP~Leo, in which accretion onto a second pole results in a highly variable secondary photometric maximum, provides a precedent for this explanation \citep[Fig. 1 in][]{b14}.

However, any rigorous explanation of the missing secondary maxima would likely require at least some knowledge of the accretion geometry, in particular the number of accretion regions and their locations on the white dwarf. This information could be gleaned from X-ray and/or polarimetric observations. The current absence of such data prevents us from offering a more refined hypothesis for the missing maxima.

\subsection{Emission-Absorption Line Inversions}
\label{dip-discussion}

Emission-absorption line inversions occur when the accretion region is viewed through an accretion curtain that is optically thin in the continuum but optically thick in the spectral lines. Thus, our line of sight (in the emission lines) stops at the relatively cool gas in the outer curtain, thereby obscuring the underlying cyclotron continuum at the wavelengths of those transitions. In the continuum, however, the curtain has a very low optical depth, so the cyclotron emission readily passes through it \citep{verbunt}.

Emission-absorption reversals can be used to assess models of the line-producing regions of the accretion curtain. \citet{fw} modeled the H, He~I, and He~II emission of accretion funnels and found that a combination of irradiation and magnetic heating was necessary to reproduce the observed line strengths in polars. They concluded that although irradiation was sufficient to account for the H and He I fluxes, the strength of the He~II emission necessitated an additional heating mechanism. Their preferred candidate for the extra source was magnetic heating in the threading region, where the stream couples onto the magnetic field lines. Based on their modeling, the H lines are produced throughout the curtain, while the He~I and He~II emission should be mostly confined to the threading region and, to a lesser extent, the terminus of the funnel as it approaches the accretion shock.

Our observations support some aspects of this model while challenging others. In particular, our data are inconsistent with their prediction that He I emission is produced primarily in the threading region. It follows from the non-eclipsing nature of J1321 that the threading region---which, by definition, is confined to the orbital plane---cannot cross our line of sight to the accretion region, as is illustrated by the schematic in Fig.~\ref{model}. As a result, it cannot be the source of the He~I absorption. Furthermore, for both H and He~I, the absorption occurs across the same phases, starts in the red wing of the line, moves blueward, and fully engulfs the line during the strongest part of the dip. Thus, it is likely that the H and He~I line-forming regions are largely coextensive. The large FWHMs for both H and He~I (Sec.~\ref{absorption}) during the dip are consistent with our line of sight passing though a wide range of gas velocities within the curtain, implying that the Balmer and He~I lines are formed throughout much of the curtain. Although the $\sim$25\% higher FWHM for the Balmer lines relative to nearby He I lines shows that the corresponding line-forming regions are not entirely co-spatial, He~I must originate throughout a larger portion of the curtain than predicted by \citet{fw}.

The best interpretation of the He~II absorption is somewhat ambiguous. On one hand, the fact that H, He~I, and He~II all undergo the same blueward motion during the line inversion suggests that they share a common line-formation region within the curtain. Although the model of \citet{fw} predicts that the threading region should be the primary line-formation region for He~II, the same argument regarding the He~I absorption applies to He~II; the threading region does not cross our line of sight to J1321's accretion region and therefore cannot be the source of the He~II absorption. Consequently, the He II-absorbing material must reside within the curtain. On the other hand, the comparatively limited velocity range of the He~II absorption is compelling evidence that the He~II-emitting regions are not entirely co-spatial with the H and He~I line-forming regions.

There are at least two plausible explanations for the reduced depth and width of the He~II absorption relative to the other lines. One is that only a small region within the curtain is hot enough to produce significant He~II absorption during the line inversion, resulting in a reduced range of velocities within the absorbing gas. Alternatively, the He~II absorption might actually be deeper and wider than indicated by the narrow absorption core in our spectra, but blended emission from another He~II line-formation region could significantly dilute its appearance (see Sec.~\ref{absorption} and Fig.~\ref{linemodel}).

In spite of this ambiguity, it is evident that H and He~I are produced in similar regions throughout the curtain, while He~II is produced in at least part of the curtain. One possible explanation for these observations is that the entire curtain is significantly hotter than predicted by \citet{fw}. Unless irradiation-induced heating is stronger than predicted, this conclusion implies the existence of an additional mechanism that heats the entire curtain.

The cause of the steady blueward motion of the lines during the dip is unclear. One simple interpretation is that the threading region has a sufficiently wide azimuthal extent to intercept multiple field lines. Gas captured near one end of the threading region would therefore follow a different trajectory than gas seized at the opposite end. Thus, at the start of the dip, the absorbing gas is following field lines which move directly away from us in the radial direction; during the later phases of the dip, the gas travels along different field lines which cause it to have lower projected velocities. The significant azimuthal extent of the curtain in the tomograms ($\sim 45^{\circ}$) lends some credence to this possibility. Alternatively, as \citet{schmidt} pointed out, density variations of the curtain can cause azimuthal variations in the curtain's optical depth, impacting the radial velocity of the absorption.

There is some evidence of a secondary line eclipse exactly halfway between the two line inversions. This is most clearly seen just after phase 0.4 in the trailed spectrum for He~II from Fig.~\ref{trailedspec}, and it could be an occultation of the threading region by the curtain. If so, the non-detection of this event in the other lines would be consistent with the threading region being an enhanced source of He~II emission in comparison to the other spectral lines. However, the diminution of the He~II line is present in just one spectrum, so this possible feature should be treated skeptically unless it is confirmed by subsequent observations.

\subsubsection{Other Polars with Line Inversions}
\label{other_polars}

While emission-absorption reversals have been observed in at least four other polars, the phenomenon has unique characteristics in each of the systems. Just one other system, FL Cet \citep{schmidt}, shows the effect in all of its major lines in the optical. FL Cet is an eclipsing polar, with the dip occurring just before the eclipse. During the dip, its H and He I lines switch from emission to absorption, while He II develops a weak P Cyg absorption component. The H and He I lines behave identically throughout the absorption event and fully engulf the emission lines, exactly as is observed in J1321. \citet{schmidt} concluded, as we have for J1321, that H and He I are emitted from the same regions within the curtain. Likewise, in both systems, the He II $\lambda$ 4686~\AA\ absorption component is comparatively weak and does not fully engulf the emission.

However, the motion of the absorption in J1321 and FL~Cet is notably different. In contrast to the steady blueward motion of J1321's absorption lines, the absorption dip in FL~Cet begins in the {\it blue} wing of each line, moves redward to the line center, engulfs the entire line, and finally reverses direction, weakening as it moves blueward. Moreover, during the absorption phase, He II develops a weak P Cyg absorption component which does not move significantly, unlike the He II absorption in J1321, which appears near the line center and moves somewhat blueward.

In the other three polars with emission-absorption reversals, the effect is detectable only in a handful of lines. In EF~Eri, \citet{verbunt} observed absorption components only in the H and He I lines between 5500~\AA\ -- 7000~\AA\ (the red limit of their spectra). During the absorption phases, the profiles of the lines blueward of 5500~\AA\ are distorted but remain fully in emission.

A similar wavelength dependence is apparent in MN~Hya \citep{rw98}. H$\alpha$ and H$\beta$ develop redshifted absorption components, and He I $\lambda$~5876~\AA\ is fully enveloped by absorption. The other H and He I lines become nearly indistinguishable from the continuum during the strongest part of the dip, but the He II $\lambda$ 4686~\AA\ line remains very prominent and is almost unaffected.

The absorption dip in the final polar, V808 Aur, is more complicated. \citet{borisov} showed that He I fully transitions into absorption, but H$\beta$ retains an emission component throughout the inversion. Its He~II $\lambda$ 4686 \AA\ line, meanwhile, shows only a partial diminution of its blue wing without ever dipping below the continuum. They reported that the absorption features moved from red to blue during the inversion.

Three of these four polars (FL~Cet, V808~Aur, MN~Hya) are eclipsing, so it appears that absorption dips are preferentially observed in high-inclination systems. If so, this favors a moderately high orbital inclination for J1321.

\begin{figure}
\epsscale{1.17}
\plotone{binary.pdf}
\caption{A possible accretion geometry for J1321 shortly after the start of the line inversion, generated using the code by \citet{kotze}. The white dwarf is obscured behind the gas in the accretion curtain. Because J1321 is a non-eclipsing system, the threading region cannot pass in front of the accretion region and therefore cannot be the source of the observed He II absorption in J1321, in contrast to theory.\label{model}}
\end{figure}

\subsection{Longitude of the Accretion Region}

Observations of eclipsing polars, including the three discussed in Section~\ref{other_polars}, have established that the accretion region tends to lead the donor star, such that it is viewed most directly before the orbital eclipse. However, if the orbital phases inferred from our tomograms are reasonably accurate, the accretion region is probably close to the line of centers of the donor and WD, and it might even trail the donor. As shown in Fig.~\ref{trailedspectrum}, there is no cyclotron spectrum between inferred orbital phases 0.65-0.8, implying that the accretion region is behind the limb of the WD during the phases at which it would be viewed face-on in other polars. Indeed, the appearance of the cyclotron spectrum at phase 0.8 suggests that the accretion region is located in the trailing hemisphere of the WD, but better knowledge of the orbital phases is necessary before this can be explored more rigorously.

\section{Conclusion}

Our time-resolved spectra of J1321 show that its emission lines briefly transition into absorption lines each orbit. We attribute this behavior to the occultation of the accretion region by the accretion flow. The similar behavior of the H and He I lines during the dip is consistent with these lines originating throughout the curtain, in contrast to theoretical predictions. Additionally, He II $\lambda$ 4686 also develops an absorption component, but it never fully transitions into absorption. Because J1321 is not an eclipsing system, the source of the He~II absorption cannot be the threading region and must instead be gas within the accretion curtain, implying that the curtain has a significantly higher temperature than predicted by theory.

An examination of our photometry, along with archival data, reveals that J1321 transitioned from a prolonged faint state into an ongoing and stable high state at some time between 2003 and 2007. Because the strength of the absorption undoubtedly depends in part on the mass-transfer rate, the stability of J1321's mass-transfer rate will facilitate follow-up observations of this phenomenon.

\section*{Acknowledgments}

We thank the anonymous referee for an insightful report that led to the improvement of this paper.

MRK and PG acknowledge support from the Naughton Foundation and the UCC Strategic Research Fund.

This work has been supported in part by the National Science Foundation (Grant No. PHY-1062819).

We thank Paul Mason and Joshua Santana for sharing with us their unpublished manuscript about the behavior of polars observed by CRTS.

We are grateful to R. Boyle, the Vatican Advanced Technology Telescope, and the Vatican Observatory for generous allocations of observing time.

The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.

The National Geographic Society - Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society.

The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation.

The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory.

The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are: The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia; The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; and The Ohio State University.

This paper used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research.

redpajama_set_name: RedPajamaArXiv


May we present to you our new regional managers Sylvie and Yves. Sylvie is a sweet, blond but seasoned sales-manager who has the ambition and heart to go far with this company. Yves just finished school and is jam packed with enthousiasm to make it as the best sales-manager there is. You'll see them soon in your city!


text:
The Seattle Seahawks' newest linebacker is changing what professional football looks like.
Today's professional football world has never seen a player like Shaquem Griffin.
In 2016, he won the American Athletic Conference defensive player of the year award, with 92 total tackles, 11.5 sacks, two forced fumbles, two fumble recoveries, and an interception. (For you non-football folks, that's really good.)
In March 2018, he clocked the fastest 40-yard dash time for a linebacker in the NFL Scouting Combine since 2003.
And in April 2018, he lived out every aspiring football player's dream of playing in the NFL when he was drafted as a defensive lineman for the Seattle Seahawks.
The big kicker? He's accomplished all of that one-handed. Literally.
Shaquem Griffin starred on the undefeated University of Central Florida football team last year. Photo via Kevin C. Cox/Getty Images
Griffin's left hand was amputated when he was 4 years old.
He was born with a condition called amniotic band syndrome, a rare disorder that occurs in the womb, causing the amniotic sac to entangle with limbs. Before the amputation, the tissue in Griffin's left finger was soft, "like a glove filled with jelly," according to ESPN.
It was also painful. "Everything I touched burned," Griffin told the network.
His mother, Tangie, recalled her son attempting to cut off his fingers one night to relieve the pain. She called the next day to schedule the surgery.
Shaquem will join his twin brother, Shaquill, on the Seahawks roster. Shaquill, who is one minute older than Shaquem, was drafted last year by the Seattle team.
Shaquill (left) and Shaquem Griffin (right) have done everything together. They played high school football togethe… https://t.co/GT5VIkb2iQ
— Darren Rovell (@Darren Rovell) 1524939325
Missing a hand has definitely raised challenges in his life, but Griffin has never let it hold him back.
Shaquem Griffin had to work hard to get to where he is today — professional football requires intense dedication, and is definitely not for the faint of heart. His indomitable will is nothing short of infectious.
"Never let anyone tell you what you can't do," he told College Gameday in 2016. "If somebody says you can't walk, prove them wrong. Somebody tells you can't play football, prove them wrong."
Shaquem Griffin, for everyone who's ever been told they can't. https://t.co/XqJO8r4azw
— SportsCenter (@SportsCenter) 1524951969
The odds have always been against Shaquem Griffin... He wasn't supposed to play in college, but he proved himself.… https://t.co/JKf38N7JOH
— CBS Sports (@CBS Sports) 1524938694
Griffin's success in football offers representation to kids with disabilities.
Heroes that we feel a connection with are important. They inspire us, they give us something to shoot for, and they remind us that we are capable of great things.
Kids with disabilities don't often see themselves reflected in the highest ranks — especially in mainstream professional sports. To see a man with one hand playing on an NFL team opens up a world of possibilities for those who have been told, directly and indirectly, that they are not physically made for certain things.
Take, for example, this young cheerleader, who was born with the same condition as Shaquem Griffin and who is one of his biggest fans:
Julianna, one of @Shaquemgriffin's biggest fans, sent him the sweetest support message before the NFL draft. 💛 (v… https://t.co/V8evBnaN2C
— NBC Sports (@NBC Sports) 1524955548
Griffin credits his family for helping him develop his strength and attitude. In an open letter to the general managers in the NFL, Griffin wrote about a coach from his childhood who told him he shouldn't play football. Griffin said it was his family who pushed him to never give up.
"I'm blessed to have thick skin. But I'm even more blessed to have a family that never let me make excuses and who raised me to never listen to anybody who told me I couldn't do something — especially because of my hand."
Here's to Shaquem Griffen single-handedly changing the face of the NFL.
Oz Pearlman wowed the Seattle Seahawks with his mentalism - Upworthy ›
Brendan Fraser showed up at a screening of 'The Mummy' completely decked out in costume
The audience went wild.
Heather Wake
The Prince Charles Cinema/Youtube
Brendan Fraser dressed as Rick O'Connell.
Brendan Fraser might be making the greatest career comeback ever, racking up accolades and award nominations for his dramatic, transformative role in "The Whale." But the OG Fraser fans (the ones who watch "Doom Patrol" solely to hear his voice and proudly pronounce his last name as Fray-zure, for this is the proper pronunciation) have known of his remarkable talent since the 90s, when he embodied the ultimate charming, dashing—and slightly goofball—Hollywood action lead.
Let us not forget his arguably most well known and beloved 90s character—Rick O'Connell from the "Mummy" franchise. Between his quippy one-liners, Indiana Jones-like adventuring skills and fabulous hair, what's not to like?
During a double feature of "The Mummy" and "The Mummy Returns" in London, moviegoers got the ultimate surprise when who should walk in but Brendan Fraser himself, completely decked out in Rick O'Connell attire. The brown leather jacket. The scarf. Everything.
"I am proud to stand before you tonight," he told the audience. "This is a film that was made in Britain. You should know that! Even the second one, too. Be proud. Thank you for being here."
He continued, "We didn't know if it was a drama or a comedy or a straight-ahead action or romance, a horror picture, more action, all of the above. No idea until it tested in front of British audiences. Thank you for that."
Fraser then asked the crowd if anyone hadn't actually seen the movie yet, before shouting, "Outstanding!" when somebody raised their hand. He then quickly made a polite plug encouraging people to go see "The Whale" before whisking himself away, saying, "I won't take up any more of your time."
Uh, yeah…I don't think any time spent with Brendan Fraser is a waste. Do you?
Watch the adorable clip below:
As to whether or not "Mummy" fans will ever see a new Rick O'Connell story up on the big screen—only time will tell. In the meantime, we'll keep watching this video on repeat.
Hollywood icons Brendan Fraser and Adam Sandler sat down for an epic chat with each other ›
Brendan Fraser's emotional awards speech about hope left audience in tears ›
Brendan Fraser's teary reaction to a six-minute standing ovation is simply a must-watch ›

redpajama_set_name: RedPajamaCommonCrawl


Cozy Chicks: Happy 2000th blog post to us!
Happy 2000th blog post to us!
This week the Cozy Chicks (yup, all 8 of us) are celebrating our 2000th blog post.
Over the years the line-up has changed, but during that time we've been sharing our personal and writing lives. The ups, the downs, recipes, and everything in between.
If you've got the time, we'd love to know how long you've been reading the blog, and what you like best about it.
Hurry! We'll be picking the winners on Friday.
Happy Anniversary!! New to your blog and loving it. My list of Cozy authors is growing. Congrats to you all and thanks.
I love to hear of the new cozies coming out. I think I've been here from pretty close to the beginning!!!
Happy anniversary. I'm a newbie here and loveee your blog. Keep up the great work.
It's hard to remember wheat this was not my first stop.
Been reading y'all for over a year now. Discovered you through Facebook and was thrilled to know most of my favorite authors are on here. Congratulations and continued success!
Good Morning and Happy 200th Blog Anniversary. I heard about your blog after reading several Maggie Sefton Books. She is from the DC area so I can relate to her books geographically. I love reading and feeling your blogs because of all the underlying humor and writing passion, I can hear and feel from reading the blogs.
I have to order the cookbook as I am a personal chef and love cooking.
Happy 2000th and congratulations! This is the first thing I read every morning.
For a 'good while'. Love your blog and all the books!
I'm not sure how long I've been reading the blog, but I know that it is now part of my day.
I've been reading Cozy Chicks for a few years. I love hearing about your new books,and what is happening in your lives. Congratulations on your 2000th blog!!
Looking forward to the 4000th blog post!
Thanks for adding cozy into my life.
Congratulations!!!!!! I love this blog!!!
I love this blog! Thanks for all of them! I sent an email too!
Happy Anniversary! I've been reading the blog for many years now. I met Michele Scott at a writer's conference in San Diego and she introduced me to the blog, which had not been up for very long at that time. I've enjoyed the blog all this time, learning about your books and your lives. Thank you!
HAPPY ANNIVERSARY TO YOU ALL!!
I have been a fan of many of you, reading for more than 10 years but I did not discover the blog until I joined facebook in 2008 or 2009. heres to many many more years!
I just love all of your posts, books and I read them every time since I signed up a few months ago!
All of you 'Cozy Crimers' are becomming more and more popular in Europe too.
Happy Anniversary! Keep up the great blogs - I love finding new titles/authors to read!
Has it been that long? I think I was there pretty soon at the beginning.
If this is 2000 lets go for 20,000!
Gosh, it seems like it's been a couple of years, ever since I discovered cozy mysteries.
My favorite things about the Cozy Chicks blog is the list of new books coming coming out. I always look forward to seeing all the fabulous covers.
I love this blog, because of it I have now read 40 titles and found and fell in love with so many wonderful series....THANK YOU!
Happy Anniversary to each of you and all of you.
And Thank you, not only for the offer of the gift bag contest, but for sharing who you are with all of us.
Happy Anniversary! Wow, 2000th is a big milestone. I've been reading for just a little over 6 months now. It's one of the first things I read when I get home from work.
Happy Anniversary! Love your blog. I have been reading it for 2 years. You guys are wonderful!
Wow, 2000 blog posts is a milestone, indeed! Happy Anniversary!! I love reading about new cozy mysteries, and the day-to-day activities of the cczy chicks!
Wow, 2000 blogposts already! I have been following a few years already, and am still not bored, so keep doing what you are doing so well!
Hi there! I have been following your blog for a long time... couple of years I believe.. I love all your posts and all the cozy mystery chatter I can find on here. keep up the good work!!! I love it!!


Atlas Titan isn't your typical billionaire heir.
He defied the expectations of his tycoon father and well-heeled, affluent family by becoming a Navy SEAL and later a clandestine operative for the darkest government agencies.
He thought he'd left that world behind for a Bay Area start-up with his brothers, but a man's past has a way of catching up with him.
I'm Piper Kipton. I'm on the run from my own mistakes, and there's only one man who can protect me from them. And he just so happens to be 6'5 with rugged good looks and a penchant for making me weak at his touch.
Brought together by unfortunate circumstances, Atlas will do everything in his power to protect me from the dangers that lurk beyond the guarded walls of our luxury digs. But who will protect us from our forbidden desire for one another?
Atlas says it's a waste of time to wish for a better past. Little do we both know- the secrets of our pasts might be the only way we can possibly have a future.
Alison Ryan is a romance author who lives with her husband and sons in a southern kind of heaven. She loves books about love, watching too much Bravo, and good bourbon. Not always in that order.


Rising interest rates coupled with increasing home prices discouraged home buying activity during the third quarter, according to Freddie Mac's latest forecast.
Freddie Mac said mortgage rates remained steady at 4.6 percent for the third quarter until the weekly average rate reached a seven-year high at 4.9 percent at the beginning of October. Freddie Mac forecasts the 30-year fixed-rate is expected to average 4.5 percent in 2018, rise to 5.1 percent in 2019 and to 5.6 percent in 2020.
Additionally, Freddie Mac believes home price appreciation will be 4.6 percent in 2019 and slow to 2.9 percent in 2020.
The forecast predicts total home sales (new and existing) will decline modestly this year to 6.07 million, increase1.8 percent to 6.18 million in 2019, and rise1.1 percent to 6.25 million in 2020.
This article has been viewed 722 times.


text:
<?php

declare(strict_types=1);

namespace Sphp\Html\Attributes;

use IteratorAggregate;
use Sphp\Stdlib\Strings;
use Sphp\Html\Attributes\Exceptions\ImmutableAttributeException;
use Traversable;

/**
 * An implementation of CSS class attribute
 *
 * The class attribute specifies one or more class names for an HTML element
 *
 * @author  Sami Holck <sami.holck@gmail.com>
 * @license https://opensource.org/licenses/MIT The MIT License
 * @link    https://github.com/samhol/SPHP-framework GitHub repository
 * @filesource
 */
class ClassAttribute extends AbstractAttribute implements IteratorAggregate, CollectionAttribute {

  protected const DELIMETER_REGEX = '/[\s]+/';
  protected const VALID_ATOMIC_VALUE = '/^(-?[_a-zA-Z]+[_a-zA-Z0-9-]*)$/';

  /**
   * stored atomic class names
   *
   * @var array<string, bool>
   */
  private array $values = [];
  private bool $required = false;

  /**
   * Constructor
   *
   * @param string $name the name of the attribute
   * @param string|string[] $value
   */
  public function __construct(string $name = 'class', $value = null) {
    parent::__construct($name);

    //this->parser = $parser;
    if ($value !== null) {
      $this->setValue($value);
    }
  }

  /**
   * Destructor
   */
  public function __destruct() {
    unset($this->values);
  }

  /**
   * Explodes a string containing CSS class names separated by whitespace characters
   *
   * @param  string $string a string to explode
   * @return string[] an array containing atomic CSS class names
   */
  protected function explodeClassNameString(string $string): array {
    $result = preg_split(static::DELIMETER_REGEX, $string, -1, \PREG_SPLIT_NO_EMPTY);
    if (!$result) {
      $result = [];
    }
    return $result;
  }

  /**
   * Parses a collection of raw class names to an array of atomic class names
   *
   * @param  string ... $raw a collection of raw CSS class names
   * @return string[] an array of atomic class names
   * @throws AttributeException if the raw input is not valid
   */
  protected function parseClassNames(string ... $raw): array {
    $parsed = [];
    foreach ($raw as $value) {
      $parsed = array_merge($parsed, $this->explodeClassNameString($value));
    }
    return array_unique($parsed);
  }

  /**
   * Parses a collection of raw CSS class names to an array of atomic class names
   *
   * @param  string ... $raw a collection of raw CSS class names
   * @return string[] an array of individual class names
   * @throws AttributeException if the raw input contains invalid class names
   */
  protected function parseAndValidateClassNames(string ... $raw): array {
    $parsed = $this->parseClassNames(... $raw);
    $invalid = preg_grep(static::VALID_ATOMIC_VALUE, $parsed, PREG_GREP_INVERT);
    if (!empty($invalid)) {
      throw new AttributeException('Invalid class names found (' . implode(', ', $invalid) . ')');
    }
    return $parsed;
  }

  public function forceVisibility() {
    $this->required = true;
    return $this;
  }

  public function isAlwaysVisible(): bool {
    return $this->required || $this->isProtected();
  }

  public function __toString(): string {
    $output = '';
    if ($this->isVisible()) {
      $output = $this->getName();
      if (!$this->isEmpty()) {
        $output .= '="' . implode(' ', array_keys($this->values)) . '"';
      } else {
        $output .= '=""';
      }
    }
    return $output;
  }

  public function isVisible(): bool {
    return $this->isAlwaysVisible() || !empty($this->values);
  }

  public function isEmpty(): bool {
    return empty($this->values);
  }

  /**
   * Sets new atomic values to the attribute removing old non locked ones
   *
   * **Important:** Parameter `$values` restrictions and rules
   *
   * 1. A string parameter can contain multiple class names separated by spaces
   * 2. An array can be be multidimensional
   * 3. Duplicate values are ignored
   *
   * @param  string|string[] ...$values the values to set
   * @return $this for a fluent interface
   */
  public function setValue($values) {
    $this->clear();
    $this->add((string) $values);
    return $this;
  }

  /**
   * Adds new atomic values to the attribute
   *
   * **Important:** Parameter ´$values´ restrictions and rules
   *
   * 1. A string parameter can contain multiple class names separated by spaces
   * 2. Duplicate values are ignored
   *
   * @param  string ...$values the values to add
   * @return $this for a fluent interface
   */
  public function add(string ...$values) {
    $parsed = $this->parseAndValidateClassNames(...$values);
    foreach ($parsed as $class) {
      if (!isset($this->values[$class])) {
        $this->values[$class] = false;
      }
    }
    return $this;
  }

  /**
   * Checks whether the given atomic values are locked
   *
   * **Important:** Parameter <var>$values</var> restrictions and rules
   *
   * 1. A string parameter can contain multiple class names separated by spaces
   * 3. Duplicate values are ignored
   *
   * @param  null|string|string[] ...$values optional atomic values to check
   * @return bool true if the given values are locked and false otherwise
   */
  public function isProtected(string ...$values): bool {
    if (count($values) === 0) {
      return in_array(true, $this->values);
    } else {
      $locked = false;
      //$values = $this->parser->parse($values);
      foreach ($this->parseClassNames(...$values) as $class) {
        $locked = isset($this->values[$class]) && $this->values[$class] === true;
        if (!$locked) {
          break;
        }
      }
      return $locked;
    }
  }

  /**
   * Locks the specified atomic values
   *
   * **Important:** Parameter <var>$values</var> restrictions and rules
   *
   * 1. A string parameter can contain multiple class names separated by spaces
   * 2. Duplicate values are ignored
   *
   * @param  string ...$content the atomic values to lock
   * @return $this for a fluent interface
   */
  public function protectValue(string ...$values) {
    foreach ($this->parseAndValidateClassNames(...$values) as $class) {
      $this->values[$class] = true;
    }
    return $this;
  }

  /**
   * Removes given atomic values
   *
   * NOTE: A string parameter can contain multiple space separated class names
   *
   * @param  string ...$values the atomic values to remove
   * @return $this for a fluent interface
   * @throws ImmutableAttributeException if any of the given values is immutable
   */
  public function remove(string ...$values) {
    foreach ($this->parseClassNames(...$values) as $class) {
      if (isset($this->values[$class])) {
        if ($this->values[$class] === false) {
          unset($this->values[$class]);
        } else {
          throw new ImmutableAttributeException("Value '$class' in '{$this->getName()}' attribute is immutable");
        }
      }
    }
    return $this;
  }

  public function clear() {
    if (!empty($this->values)) {
      $this->values = array_filter($this->values, function ($locked): bool {
        return $locked;
      });
    }
    return $this;
  }

  /**
   * Determines whether the given atomic values exists
   *
   * NOTE: A string parameter can contain multiple comma separated class names
   *
   * @param  string ...$value the class names ans atomic values or comma separated
   * @return bool true if the given atomic values exists
   */
  public function contains(string ...$value): bool {
    $exists = false;
    foreach ($this->parseClassNames(...$value) as $class) {
      $exists = isset($this->values[$class]);
      if (!$exists) {
        break;
      }
    }
    return $exists;
  }

  public function getValue() {
    if (!empty($this->values)) {
      $value = implode(' ', array_keys($this->values));
    } else {
      $value = null;
    }
    return $value;
  }

  /**
   * Counts the number of the atomic values stored in the attribute
   *
   * @return int the number of the atomic values stored in the attribute
   */
  public function count(): int {
    return count($this->values);
  }

  public function toArray(): array {
    return array_keys($this->values);
  }

  /**
   *
   * @param  callable $filter
   * @return $this for a fluent interface
   */
  public function filter(callable $filter) {
    $result = [];
    foreach ($this->values as $class => $locked) {
      if ($locked || $filter($class)) {
        $result[$class] = $locked;
      }
    }
    $this->values = $result;
    return $this;
  }

  /**
   *
   * @param  string $pattern
   * @return $this for a fluent interface
   */
  public function contaisPattern(string $pattern): bool {
    $contains = false;
    foreach ($this->toArray() as $class) {
      if (Strings::match($class, $pattern)) {
        $contains = true;
        break;
      }
    }
    return $contains;
  }

  /**
   *
   * @param  string $pattern
   * @return $this for a fluent interface
   */
  public function removePattern(string $pattern) {
    $filter = function ($value) use ($pattern) {
      return !Strings::match($value, $pattern);
    };
    $this->filter($filter);
    return $this;
  }

  /**
   * Returns an external iterator
   *
   * @return Traversable<string> external iterator
   */
  public function getIterator(): Traversable {
    return yield from array_keys($this->values);
  }

}

redpajama_set_name: RedPajamaGithub


Here is a generation of men quickly fading from Hollywood's midst, men who remember the days before Madonna, The Matrix, and MTV were dreamed into existence, men who first knew the likes of Walt Disney and Groucho Marx as actual flesh and bone, not cultural institutions. Richard Farnsworth was such a man: a true show business pioneer and two-time Oscar nominee, most recently for 1999's The Straight Story. But he too is now gone, dead from a self-inflicted gunshot wound. He was 80 years old.
It was Margaret who talked her bashful husband into giving speaking parts a bona fide try. For his first major role, in 1978's Jane Fonda-starring Western Comes a Horseman, Farnsworth nabbed a best supporting actor nod and a new career. His soulful eyes and plainspoken delivery imbued each part with graceful gravitas, be it the gentlemanly stagecoach robber of 1982's The Grey Fox or the genial grandfather of 1986's TV series Anne of Green Gables. "His face was a marvelous map of emotions," says Gables director Kevin Sullivan.
Farnsworth's cancer worsened after Story finished, but he still showed at the Oscars. "He was walking with a cane, but his spark was there," remembers Chad Lowe, his costar in 1992's Highway to Hell. And Farnsworth kept that spark till the very last days. Though confined to a wheelchair, he visited the local racetrack. The week before he died, he went to Santa Fe to accept an award from the New Mexico governor. And in early October he was even talking to his agent about taking a role in a Charlton Heston movie about World War II vets.


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text:
Home/Business/Sports Stars and Brand Endorsement
BusinessSports
Sports Stars and Brand Endorsement
INFOtainment News Follow on Twitter September 21, 2017
Source: Pixabay
Celebrity sells, but popular culture is a fickle creature and celebrities can fall from grace in an instant. Sports stars are something different, whilst we might say of a celebrity that they are famous for being famous, we can never say that of a sports star. We know that sporting achievement is the result of exceptional gifts and complete dedication; we know that sports stars are remarkable human beings. So, when a sports star becomes an ambassador for a product the effect is global and immensely powerful.
Cristiano Ronaldo – Three-time winner of the FIFA Ballon d'Or, 372 goals in 360 appearances for Real Madrid, Ronaldo is the highest paid, most famous athlete in the world. Not surprisingly he's in huge demand as a product ambassador: his name is linked to Armani, Castrol, Coca Cola, KFC and Emirates Airlines. He is part of the TAG Heuer ad campaign, 'Don't Crack Under Pressure' and the Formula 142mm Chronograph Ronaldo Special Edition watch is produced in his team colours of red and green. Following in the footsteps of Michael Jordan and James LeBron he became the third athlete to sign a lifetime deal with Nike which will make him the world's first sports billionaire.
Serena Williams – In terms of the strength of her reputation, Williams is the female sports star who comes closest to Ronaldo. Arguably the greatest female tennis player of all time, with 21 Grand Slam singles titles and multiple doubles titles, Williams was ambassador for Puma for five years before switching to Nike in a $40 million endorsement deal signed in 2013. Like Ronaldo her name is also linked to a string of other products, including Gatorade, Wilson, AudeMars Piguet and Delta Airlines.
Boris Becker – Former tennis world number one and six times major singles winner, Becker is also an enthusiastic and successful poker player. In 2013, he won more than €90,000 at the poker table, so it is perhaps a natural progression that he should become ambassador for partypoker. 'I'm equally competitive at the poker table as I was on the tennis court…I'm hoping to use my experience on the tennis court to my advantage.'
Ronda Rousey – Watched by over a billion households in a hundred and fifty-eight countries, Mixed Martial Arts is one of the fastest growing spectator sports in the world and despite her shock defeat at the hands of Holly Holm, Rousey remains its biggest female star. She confounds stereotypes by being a glamorous woman who is successful in a violent, brutal sport. She's also not afraid of a challenge outside of the octagon as she proved when she became the first woman in twenty-two years to host Saturday Night Live. In December 2016, she became Pantene's newest brand ambassador for their campaign which runs with the slogan: 'Don't hate me because I'm strong. Strong is beautiful'.
Do You Have These 5 Must-Know Habits of Successful People?
3 Most Common Reasons Couples Fight
8 High-Yield Business Ideas
The Many Benefits of Leasing a New Car
Virtualization: What Are The Business Benefits?
F1 Driving innovations which can Make Road Cars Safer
The JOBS Act: Encouraging Startups, Supporting Small Businesses


text:
Q: Delphi: Memory leak when creating a TStringList inside a class I have this pieces of code
TSql = class
  private
    FConnString: TStringList;
  public
    property ConnString: TStringList read FConnString write FConnString;
    constructor Create;
    destructor Destroy;
  end;

var
  Sql: TSql;

...

implementation

{$R *.dfm}

constructor TSql.Create;
begin
  //inherited Create;
  FConnString:=TStringList.Create;
end;

destructor TSql.Destroy;
begin
  FConnString.Free;
  //inherited Destroy;
end;

procedure TForm1.Button1Click(Sender: TObject);
begin
  Sql.Create;
  Sql.ConnString.Add('something');
  showmessage(Sql.ConnString.Text);
  Sql.Destroy;
end;

Why when creating the FConnString is creating a memory leak, after a press the button?
..................................
..................................
..................................
..................................

A: EDIT The actual problem
The original code in the question was as follows:
procedure TForm1.Button1Click(Sender: TObject);
begin
  Sql.Create;
  Sql.ConnString.Add('something');
  showmessage(Sql.ConnString.Text);
  Sql.Destroy;
end;

The problem line was Sql.Create; which should have been Sql := TSql.Create;. The reason this causes a memory leak is as follows:

*

*Sql.Create; is called from a nil reference.

*This calls TStringList.Create; and attempts to assigned the result to FConnString.

*Because Sql is a nil reference, this triggers an Access Violation.

*The problem is there is no way to destroy the TStringList instance that was created.

Additional problems in original answer
Your destructor is virtual, you're not overriding.
You're not calling your inherited Destructor.
TSql = class
  private
    FConnString: TStringList;
  public
    property ConnString: TStringList read FConnString write FConnString;
    constructor Create;
    destructor Destroy; override; //Correction #1
  end;

destructor TSql.Destroy;
begin
  FConnString.Free;
  inherited Destroy; //Correction #2
end;

EDIT
A few general tips:

*

*I applaud you for using composition (making FConnString a member instead of inheriting from TStringList). However, by exposing it publicly, you would lose many of the benefits. Specifically you would be exposed to Law of Demeter violations. I'm not saying never do it. But be aware that you can create a maintenance problem down the line if a large amount of client code accesses ConnString directly.

*Declaring FConnString: TStringList; violates the principle of Program to an interface, not an implementation. TStringList is a specific implementation of TStrings and this declaration prevents use of other subclasses of TStrings. This is more of a problem combined with #1: if in a few years time you find and want to switch to a different/better subclass implementation of TStrings client code that is binding to TStringList now creates much more work and risk. Basically the preferred aproach can be summed up as:

*

*Declare the variable as the abtract base type.

*Create the instance as the specifically chosen implementation subclass.

*Let polymorphism ensure subclass behaviour is applied correctly in overridden methods.

Again this is a general guideline. If you specifically need access to properties/methods that were added at the TStringList level of the hierarchy, then you have to bind to that class. But if you don't need it, don't do it.

A: There are two things I see. The first of which was already covered by the other comments and answer regarding the lack of "override" on the destructor.
The second issue is the property declaration itself. In general, you should never declare a property that references an object field in the "write" clause. The reason is that assigning to that property will "leak" the existing instance in that field. Use a method for the "write" clause of the property declaration:
property ConnString: TStringList read FConnString write SetConnString;
...
procedure TSql.SetConnString(Value: TStringList);
begin
  FConnString.Assign(Value);
end;

Also notice that this method does not overwrite the FConnString field either. It merely copies the "value" or the "content" of the Value TStringList into the FConnString instance. In this manner the TSql instance is in complete and total control over the lifetime of that field. It is the responsibility of the code assigning that property to control the lifetime of the Value TStringlist.

A: You forgot to declare Destroy() with the override specifier, so TSql.Destroy is not actually being called when the object is destroyed.
destructor Destroy; override;

A: The object is not created correctly. It must be:
Sql:=TSql.Create;

From here is coming the memory leak.

redpajama_set_name: RedPajamaStackExchange


Loras College offers Teacher Education applications major to licensure in early childhood education, elementary education, secondary education and instructional strategist (specific education). If he will not do this, the Senate Rules committee – which by law have to confirm appointed Regents – should reject Crane and demand that the Governor nominate a better candidate making use of the legally essential method. The great news is that you can nonetheless get in touch with the Division of Education to see what you want to do in order to get your student loan out of default, and you will be eligible for federal assistance as soon as again when you have gotten the matter squared away. This is frequent sense now, but a secular trend of disinvestment seemed to come as news to the regents and to most of UCOP ten years ago.
It was an easy decision to explore the late 1790s after studying and generating the gown and millinery for the American Duchess Guide earlier this year. Rodney Malesi, United States International University-Africa (Kenya) talked on Constructing Details Literacy in Copyright, Licensing, and Associated Legal Matters: A USIU-Africa Library Knowledge. Strong public funding, I stated, explained why UC wasn't SUNY or the UNC or Texas technique with a couple of flagships and then a miscellany of varied campuses that carried out small or no investigation.
They might also be repelled by the increasing expense of tuition, and whilst it is correct that a higher education could be a single of the biggest expenditures you will ever face, the significance of a college education has become quite evident in terms of earning possible inside today's economy. In reality, it seems completely possible that HireVue's algorithm about body language and facial expression could also effortlessly track and quietly count skin color or gender characteristics. Social Sciences – Philippine Government New Constitution with Human Rights, Philippine History, Basic Economics, Taxation, Agrarian Reform, Society, Culture with Household Planning Rizal and other Heroes, Philosophy of Man, Arts, Basic Psychology and Info and Communication Technology.
If you are somebody who presently works for 30+ years and have been laid off, appear at your job responsibilities and focus on the projects you impact, the people you assisted in becoming leaders. This course will deepen student's capacity to determine person learning variations amongst kids (grades K-6) and to develop specific strategies for meeting their different learning demands. The overall picture of the economics of early childhood education is as a result very difficult, with different sources of funding complementing each other, complex systems of transfers in between levels of government, and intricate combinations of public and private funding.
The last two aim to have students acquire an understanding of the learners' characteristics, curriculum, strategies of teaching, theories of learning and teaching, partnership in between theory and practice, and school as a social institution. The U.S. has been transformed from a manufacturing-based economy to an economy based on information, and the importance of a college education nowadays can be compared to that of a high school education forty years ago. According to the perfect of investigation-university, the university teaching staff is actively involved in the study of the institution.


text:
Latvijas Banka
Latvijas Banka (Bank of Latvia, National Bank of Latvia) is the central bank of the Republic of Latvia. It was created out of the State Savings and Credit Bank, whose assets and liabilities were taken over by the Bank of Latvia on November 1, 1922. The objective of the operation of the Bank of Latvia as the central bank is price stability promoting Latvia's long-term economic growth. The Bank of Latvia is independent in making and implementing decisions. It is supervised by the Parliament (Saeima) of the Republic of Latvia. The Council of the Bank of Latvia comprises the Governor, Deputy Governor and six members whose term in office is six years. The Bank of Latvia is a full-fledged participant in the ESCB and cooperates with the Bank for International Settlements (BIS), the World Bank and other international financial institutions. In December 2001, Ilmars Rimsevics was appointed Governor of the Bank of Latvia. As of December 2011, Latvijas Banka had total assets of 3.539 billion lats (US$6.42 billion).
K. Valdemara street 2A
Riga, LV-1050
Fax: (+371) 6702 2420
Website: www.bank.lv


text:
Hysteropterum evanescens är en insektsart som beskrevs av De Bergevin 1919. Hysteropterum evanescens ingår i släktet Hysteropterum och familjen sköldstritar. Inga underarter finns listade i Catalogue of Life.

Källor

Sköldstritar
evanescens

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text:
[ weird things ]
science, tech, and other oddities [ wt ]
# latest # science # space # tech # oddities # astrobiology # sex # evolution # politics # health # education
podcast sci-fi saturday
about weird things contact us
counting exoplanets by their gravitational wells
Just like supermassive black holes, planets can bend light with their gravity. But do they bend it enough for us to detect them that way?
by: Greg Fish on 01.13.2012
Depending on who you talk to, planets around alien suns are either somewhat rare due to the chaotic nature of planetary formation around infant stars, or even more plentiful than the stars themselves. Since exoplanets are rather small and dim, lost in the glare of their host suns, spotting them takes a lot of time and effort. Direct observation means catching a momentary dip in starlight from an object of indeterminate size at a time that's random to the observer. If a currently unknown planet orbits its sun every 237 days, how will you know to point your telescope at the right star every 237 days? There just has to be a better way of taking the galactic census so we can figure out what the average solar system looks like, and ultimately, what are the chances one may have the right conditions to host life. And there may be according to a group of astronomers who used a very familiar manifestation of general relativity to escape the normal fuss and bother of exoplanet detection, trying to find planets that orbit a little bit farther from their suns to get a rough measure of solar system sizes.
When we last talked about the physics of wormholes, we looked at microlensing, essentially the distortions in the appearance of an astronomical object caused by the gravity of something relatively small in front of this object in our line of sight bending the fabric of space. Usually we deal with gravitational lensing on the scales of galaxy and galaxy clusters and it's partially how we know that dark matter exists. At either end of the light distorting spectrum it's the same mechanism at work. Traveling photons are skewed by the uneven fabric of space and time. So, the researchers posited, if galaxies can distort the appearance of other galaxies and we see stars doing the same thing, what about planets orbiting stars? We know they also bend light in the wake of their gravitational wells, so a planet orbiting at some distance around a star should distort its halo. And so, after watching 100 million stars, they found evidence of exoplanets in orbit around their parent suns exactly as general relativity predicted would happen if they were there. Of course this is all easier said than done.
Since a star pumps out so much light and the planets have to orbit at just the right inclination to be spotted in the act of disturbing the halo, the 100 million stars had to be narrowed down to just 500 promising ones, and those 500 had to be watched for five long years until ten cases of direct microlensing were finally seen. But all that effort didn't seem to bring consistent data since the results seem all over the place. According to the tally, between 6% and 23% of stars seem to host a Jupiter-like world, between 23% and 74% have a Neptune-like body, and between 25% and as many as 97% might have a terrestrial planet around them. As the planet size gets smaller, the uncertainty increases wildly, so much so as to be almost meaningless for terrestrial worlds which are the ultimate goal of all planet hunters. The exoworlds are just too dim, too far away, and too small to register prominently on our existing instruments, and although the study does imply that pretty much all stars have a solar system of some sort, it can't actually tell us anything definitive about what sort of planet we could usually expect. Going by this survey, it could be anything from a turbulent gas giant to Earth 2.0.
Don't get me wrong, trying to use microlensing to find the statistical distribution of planets is a terrific idea. It's just that the universe keeps on placing interesting things too far away for us to spot with out current tools. We could even try this trick again with better equipment and hyper-sensitive telescopes to see if we can get more predictive and accurate tallies. However, it seems that until then, the candidate worlds seen by Kepler, and in the future, the Terrestrial Planet Finder, will provide us with the most accurate and predictive sampling of our galactic neighborhood since they can point to actual planets with an accuracy I doubt we could get from even the most precise measurements of planet-created microlensing manifesting around distant alien suns. This sort of survey would give us a more accurate picture of planetary distribution across the galaxy and allow us to build an accurate picture of a typical alien solar system. With such a model, we could look at any random star and have a decent idea of what we should expect to see orbiting it and at approximately what distances from it so we can better time our telescopes' observations in the hunt for another planet that hosts intelligent life.
See: Cassan, A., et al. (2012). One or more bound planets per Milky Way star from microlensing observations Nature, 481 (7380), 167–169 DOI: 10.1038/nature10684
# space // astronomy / astrophysics / exoplanets / general relativity
by: Greg Fish
Los Angeles-based editor and founder of Weird Things, co-host of the WoWT Podcast, ex-Soviet computer lobotomist with a graduate degree in computer science. Specializes in, but not limited to, popular science, technology, the web, and conspiracy theories. His work also appeared in Rantt, BusinessWeek, i09, HowStuffWorks, SEED, RawStory, Science To The People, Le Monde, and Discovery News/Seeker, and he has a weekly radio segment on The Shift With Drex.
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As stars mourned the death of "Star Wars" icon Carrie Fisher, the cast of "Scream Queens" rallied around their co-star Billie Lourd, Carrie's daughter, in her time of grief. Billie hasn't spoken out about her loss yet, but the cast from her show is letting her know they're here for her. Show regulars like Abigail Breslin, Lea Michele, and Taylor Lautner all shared some love for Billie.
Even Ariana Grande, who had a brief run in the show's first season, reached out to Billie in an Instagram post. Ariana seemed to take a cue from Carrie's outspoken nature when she called out a fan for objectifying her to her face, so it's no surprise she wants to let Carrie's daughter feel some love.
See some of the sweet messages from Billie's co-stars below.


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text:
"Shell-ebrate" Five Years With Birch Aquarium's Sea Turtle At Their Turtleversary!
See + Do Celebration commemorates Loggerhead's inspirational story of survival
Monday, January 6, 20200
Birch Aquarium at Scripps Institution of Oceanography at UC San Diego is celebrating the fifth anniversary of their rescued Loggerhead Sea Turtle's arrival with the first-ever Turtleversary on January 11 and 12 from 11 a.m. to 3 p.m.
The family-friendly "shell-ebration" will be a fun-filled weekend of sea turtle-themed activities, crafts, and marine reptile science. Guests are encouraged to get hands-on with sea turtle biofacts, learn about local sea turtle research, and get an insider's look at how the aquarium's sea turtle is target trained and cared for.
The Loggerhead's story of perseverance, and the technological advances made to ensure her continued survival, have inspired people from around the world.
"Our collaborations with our colleagues have inspired students and researchers alike," said Jennifer Nero Moffatt, the aquarium's senior director of animal care, science and conservation. "Sea turtles hold a special place in our hearts and need our protection; all 7 species in danger from numerous environmental impacts. Our guests are able to get close to our Loggerhead Sea Turtle and feel a sense of wonder for our ocean planet."
Birch Aquarium's female Loggerhead Sea Turtle was found injured and sick in a power plant outflow canal in New Jersey. After rescue, she was nursed back to health at South Carolina Aquarium and was deemed non-releasable as the medical teams believed she would not survive on her own. Birch Aquarium took in the sea turtle November, 2014, and was revealed to the public in January, 2015. Since then she has grown significantly and now weighs 215 pounds.
Birch Aquarium's turtle made international news in 2018 for the 3D-printed prosthetic that fits like a puzzle piece into her shell. This groundbreaking brace was the first of its kind for a sea turtle shell, and has now successfully mitigated the abnormal shell growth.
Sat – Sun
Jan 11, 2020 – Jan 12, 2020
Birch Aquarium


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This metric gives you insight into your website visitors. For instance, desktop visitors might have different needs and require a different user experience than tablet or mobile visitors. Importantly, if you see mobile traffic increasing as a percentage of total traffic, it's critical to ensure your mobile site offers a positive experience for those users. In addition to the need for your site's look and feel to be strong on mobile, forms with long fields should be avoided among other things.