text:
\section{Introduction}

Magnetic reconnection is thought to lie at the heart of energy release in solar flares. The earliest models based upon the dynamics of a planar current-sheet
\citep{Sweet1958,Parker1957} gave rise to slow reconnection rates that depend on the magnetic Lundquist Number $S$ by $1/\sqrt{S}$, where $S = v_A L/\eta$. Here, $v_A$ is the Alfv\'en speed, $L$
the current-sheet half-length and $\eta$ the magnetic diffusivity. In the corona, $S \approx 10^{12}$.
An alternative MHD model was proposed by \cite{Petschek1964}, in which fast steady-state
reconnection takes place along a small
fraction of the current-sheet length, made possible by the inclusion of slow shocks. Petschek's model remains of interest as it was the first to yield reconnection rates fast enough to account for
the rapid energy release observed in flares, varying instead as $1/\log S$.

These current-sheet configurations were incorporated into the
the standard ``CSHKP'' solar flare model (\citealp{Carmichael}; \citealp{Sturrock}; \citealp{Hirayama}; \citealp{Kopp}), where a rising flux rope causes the inflow of oppositely orientated magnetic field lines, creating between them a Sweet-Parker current-sheet in which reconnection occurs.
The standard model faces well-known fundamental challenges, related to the plasma micro-physics.
Petschek's mechanism assumes a certain large-scale steady configuration,
but questions surround how such a configuration might occur \citep[e.g.][]{Kulsrud2011}. Furthermore, additional physics must be introduced to explain how the plasma is heated, and how electric fields capable of accelerating particles to above MeV energies are generated. \citep[e.g.][]{Benz2016}.

In recent years, attention has been drawn to
the possible role of a tearing mode instability
across current-sheets (or
\textit{plasmoid instability}), in explaining the onset of ``fast'' reconnection, i.e. at a rate independent of $S$, in various regimes. In magneto-hydrodynamics (MHD), analytical growth rates of the plasmoid instability were derived under conditions
where current-sheet lengths greatly exceed their (MHD) thickness (\citealp{1990PhFlA...2.1487C,2007PhPl...14j0703L}). Such current-sheets were found to be intrinsically unstable to high-wavenumber perturbations, with growth rates greatly in excess of Alfv\'en crossing times.
A chain of number $S^{3/8}$ ($\approx 10^4$ in the solar corona) plasmoids are formed along sheet length $2L$, each with a length $S^{1/8}$ larger than the current-sheet width $\delta= L/\sqrt{S}$. Numerical 2D simulations with $S=10^6$ have supported the general picture of disruption of reconnecting current-sheets through the plasmoid instability, creating a turbulent cascade with a power spectrum consistent with in-situ observations of plasma turbulence \citep{2018PhRvL.121p5101D}. However, theoretical work must still be guided by observations.

In this study, we present observational evidence for the presence of unobservably
small magnetic structure, consistent with the plasmoid-fragmentation picture within a dynamically evolving current-sheet in the wake of a coronal mass ejection. We show that the magnitude of linear polarization is sensitive to unresolvable small-scale magnetic structures.

\section{The plasma-sheet associated with the September 10th 2017 flare}

In the corona, current-sheets are predicted to occur with a width of order 10 m \citep{Litvinenko}, far below the observable limit of even the best coronal instruments
($\approx 200$ km). However, rare sheets of hot plasma have been observed, associated with eruptive flares and appearing to be related to reconnection within a current-sheet \citep[e.g.][]{Liu}.
These ``\textit{plasma}-sheets'' are elusive and notoriously difficult to identify, most readily seen above the solar limb.

Perhaps the brightest and longest-lived plasma-sheet observation to date is associated with an X8.2-class flare on September 10th 2017 (e.g. \citealp{Long}; \citealp{Warren}; \citealp{Kuridze}; \citealp{Li}, \citealp{Cheng}; \citealp{Longcope}; \citealp{Gary}; \citealp{Morosan}).
The flare and coronal mass ejection
erupted from AR 12673 on the western solar limb, observed across the spectrum by multiple space-based and ground-based instruments.
Fortuitously, the CoMP instrument
obtained polarization data of the
plasma-sheet, and although the plasma-sheet has been well studied, no analysis of its
polarized light has been published.

Important earlier studies of intensity images and spectra include that of
\cite{Warren}. They used Extreme ultraviolet (EUV) Imaging Spectrometer (EIS) \citep{Culhane} and Atmospheric Imaging Assembly (AIA) \citep{Lemen} data to study the spectroscopic evolution and structure of the plasma-sheet. Using temperature sensitive EIS lines, they calculated a mean plasma-sheet temperature of 15-20 MK. It was deduced that the plasma-sheet must be heated by processes originating from magnetic reconnection, as is consistent with the CSHKP model.

\cite{Li} and \cite{Warren} investigated non-thermal broadening
 of spectral lines
within the plasma-sheet, finding non-thermal velocities as high as 200 km s$^{-1}$. The highest line widths (measuring
velocities of plasma superposed along the line-of-sight, or ``LOS'')
were seen first at the base of the plasma-sheet, later they shifted to higher altitudes. The broad lines were hypothesized to indicate small-scale turbulent velocity fluctuations from plasmoid fragmentation during reconnection. In support of this idea, \cite{Cheng} analyzed the plasma-sheet plane-of-sky (POS) outflows and find a power-law spectrum of fluctuations in wavenumber space consistent with a turbulent cascade of energy toward smaller scales.

Thus, while there is indirect evidence for the presence of instabilities in the plasma-sheet of the September 10th 2017 flare, none of the evidence has provided clear insight into the nature of the plasma-sheet's magnetic field and its role in onset of turbulence. More direct observations of the magnetic field may be a crucial clue to our understanding magnetic reconnection in this and similar events.

\begin{figure*
  \centering
  \includegraphics[width=16cm]{event.eps}
  \caption{Left: GOES-15 X-ray flux for the flare, displaying CoMP observing times.
  Right: Location of the plasma-sheet FOV used in this study.}
  \label{fig:event}
\end{figure*}

\section{Observations}

The September 10th 2017 flare originated from AR 12673 on the western limb, peaking at 16:06 UT. In this study we use observations from the High Altitude Observatory (HAO) Coronal Multi-channel Polarimeter (CoMP), between 17:07:50 and 20:10:36 UT. The CoMP instrument has an aperture of 20 cm and uses a coronagraph to observe the low corona from $\sim$1.03 to 1.5 \(R_\odot\). CoMP measures the intensity and linear polarization (Stokes I,Q,U) of infrared Fe XIII 1074.7 nm and 1079.8 nm lines, with a formation temperature of $\sim$1.5 MK. 48 of the 62 available observations occurring between 19:44:36 and 20:10:36 UT
measured the Fe XIII lines centered at three wavelengths, each
through a filter of
roughly Gaussian shape (FWHM of 1.3 \AA),
with a 4.35\arcsec\ spatial sampling and 30 second cadence.
CoMP observing times are shown in the left panel of Figure \ref{fig:event}.

The K-Cor instrument at the Mauna Loa Solar Observatory also observed the event, measuring white light polarization ($pB$) from 1.05 to 3 \(R_\odot\) over the same observing duration as CoMP. K-Cor has a lower resolution than CoMP (spatial sampling of 5.64\arcsec) but a higher cadence of 15 s.

EUV observations by AIA onboard the Solar Dynamics Observatory (SDO) provide context, with a higher cadence ($\sim12$ seconds) and considerably higher spatial resolution (0.6\arcsec). The plasma-sheet is most visible in the 193 {\AA} passband, measuring both Fe XXIV and Fe XII emission. Given the plasma-sheet's high temperature, most of the observed emission is likely from the 20 MK Fe XXIV line.
Despite its high temperature, the plasma-sheet is also seen in cooler AIA passbands, such as 211 {\AA} (\cite{Warren}), dominated by plasma closer to 2 MK.
In AIA 193 {\AA}, the plasma-sheet is clearly visible from 16:06 to beyond 20:30 UT. Therefore, although the higher cadence CoMP observations start 2 h 38 m after the flare peak, the plasma-sheet is still visible in EUV observations during this time. This is much longer than the Alfv\'en crossing time, which is just a few minutes
for a magnetic field strength of 10G.

Figure \ref{fig:polarization}A shows AIA 193 {\AA} observations of the plasma-sheet, averaged over the CoMP observing period and processed using the Multi-Gaussian Normalisation (MGN) technique (\cite{Morgan}). In this image, the plasma-sheet is seen as the bright horizontal structure, located above the saturated flare loop. A diffraction pattern from saturated intensities is also visible, as a faint cross emanating from the flaring region. The location of this field of view (FOV) is shown in Figure \ref{fig:event}B.

\begin{figure*
  \centering
  \includegraphics[width=14.5cm]{cross_section.eps}
  \caption{
  A) Normalized AIA 193 {\AA} intensity. Curved white line marks position of the CoMP occulting disk.
  B) AIA 193{\AA} cross-section of intensity along the dashed green line in adjacent panel.
  C) CoMP 1074.7 nm $I$
  D) CoMP 1074.7 nm cross-section of $I$, along the dashed green line in adjacent panel.
  E) CoMP 1074.7 nm $P$. Red lines are polarization vectors, with length proportional to $-1/\log(P)$.
  F) CoMP 1074.7 nm cross-section of $P$, along the dashed green line in adjacent panel.
  G) CoMP 1074.7 nm azimuth angle $\theta$, relative to the radial direction. White lines show the corresponding polarization vectors.
  H) CoMP 1074.7 nm cross section of $\theta$, along the dashed green lines in adjacent panel. CoMP images have an overlaid artificial-occulter to increase sharpness at image edge.
  }
  \label{fig:polarization}
\end{figure*}

\section{Spectropolarimetry}

Linearly polarized radiation is created by the scattering of anisotropic radiation from the solar surface by coronal plasma. The anisotropic radiation generates unequal populations of magnetic sub-states, (\textit{atomic} polarization), dependent on the local thermal and magnetic conditions of the plasma \citep{Charvin1965}. The atomic polarization of \ion{Fe}{13} is, to within a few percent, proportional to the factor $3 \cos^2\theta_B-1$, where $\theta_B$ is the angle between the magnetic field vector and direction of the center of the incident radiation (equation 45 of \cite{CasiniJudge}, \cite{Judge2007}). Emission from a complex atom excited by anisotropic radiation must be computed from a solution to the statistical equilibrium equations. The term $3 \cos^2\theta_B-1$ is the leading order angular
factor in the radiative excitation of atomic sub-levels for each
transition. \cite{Judge2007} demonstrated that for multiple levels in an atomic model, the linear polarization arising from sub-level populations follow this term within a few percent for typical M1 transitions. This is because incident solar radiation
is strongest in the optical and infrared wavelengths where the M1 transitions
are found. The polarization can be destroyed by isotropic processes, including collisions by a sufficiently high density of thermal electrons and protons.

The emitted radiation is linearly polarized by a factor
proportional to
the amount of atomic polarization, therefore varying as
\begin{equation} \nonumber
  P \propto 3 \cos^2\theta_B-1.
  \label{eqn:linear}
\end{equation}

 For a radial magnetic field, the magnetic field vector is parallel to incident radiation ($\theta_B = 0$) and linear polarization is at a maximum. For a tangential magnetic field, atomic polarization becomes negative. The atomic polarization passes through
 zero as $3\cos^2\theta_B=1$, at the `Van Vleck' angle $\theta_B=\theta_{VV} = 54.74^{\circ}$. Because we have no prior knowledge of $\theta_B$ relative to $\theta_{VV}$, the change in sign of atomic polarization leads to
 a well-known 90$^{\circ}$ ambiguity in determining the POS projection of magnetic field direction.

CoMP measures the two components of linear polarization relative to
a fixed reference direction, as well as total unpolarized intensity (Stokes $U$, $Q$ and $I$ respectively). Combining these, we calculate fractional linear polarization through,
\begin{equation}
  P = \sqrt{U^2 + Q^2}/I.
  \label{eqn:stokes}
\end{equation}
We can also use Stokes U and Q to calculate the azimuth angle of the polarization vector in the POS,
\begin{equation}
  \theta = \frac{1}{2}\arctan{(\frac{U}{Q})}.
  \label{eqn:azi}
\end{equation}
While $\theta$ is determined by $U$ and $Q$ measurements, the corresponding polarization vector has
the $90^{\circ}$ ambiguity to magnetic field lines, either parallel, perpendicular, or undetermined depending on whether
the actual (unknown)
angle $\theta_B$ is
greater than, smaller than or equal to $\theta_{VV}$.
The polarization vector is not a physical ``vector'' but a line with a magnitude and azimuth.

The corona is optically thin to infrared radiation. Therefore, every observation involves
integration over the LOS. Variations in $\theta_B$ along the LOS lead
to a superposition of different polarization vectors (weighted by the local plasma density), causing a reduction of $P$.

\section{Analysis}

Figure \ref{fig:polarization}A shows the time-averaged intensity of AIA 193 {\AA} emission, sampling hot
Fe XXIV emission, from 18:00 - 20:00 UT. During this period, the plasma-sheet dimmed, but with no significant variation to its shape. The plasma-sheet appears as a near-horizontal structure, stretching out from the top of the flare loop arcade (X $\approx 1020$\arcsec). A cross-section through the plasma-sheet places the plasma-sheet centroid at $Y\approx-145$\arcsec\ (Figure \ref{fig:polarization}B).

In comparison, Figures \ref{fig:polarization}C and E respectively show intensity $I$ and linear polarization $P$ of cooler Fe XIII 1074.7 nm emission. All CoMP data shown are ``level 2" data products from an improved pipeline from early October 2019 (de Toma and Galloy, private communication).

The images were calculated using the mean of 46 CoMP $I$, $Q$ and $U$ measurements from 19:44:36 to 20:03:06 UT (later images were excluded due to poorer seeing from passing cloud). Fe XIII 1074.7 nm emission comes from plasma around $\sim$1.5 MK, in contrast to AIA 193 {\AA} at $\sim$1.2 and 20 MK. With clear emission in the post-flare loop-top, the absence of strong Fe XIII intensity in the plasma-sheet is striking. The AIA 211 {\AA} and 193 {\AA} channels do show the plasma-sheet at the
later times CoMP observed, but emission is weaker and more diffuse than at earlier phases.

The fractional linear polarization $P$ reveals a prominent dark triangular structure with a yet smaller dark structure underneath, just above the limb. The latter feature aligns with the bright flare looptop in the AIA image. The triangular feature however, overlies the bright region over the looptops. These two regions both have $P < 0.01$. Above the dark triangular structure,
aligned roughly along the AIA plasma-sheet emission, there is a broad, dark region, positioned radially from the top of the overlying structure to the west-most edge of the CoMP FOV. A cross section through the region shows a significant drop in polarization (Figure \ref{fig:polarization}F), despite no clear $I$ signature at the same location (Figure \ref{fig:polarization}D).
Here, we see a broad gradual drop in polarization down to $P < 0.01$, from values of $P \approx 0.055$ and $0.075$ either side of the feature. Despite being $\sim 10$ times broader than the structure observed in AIA 193 {\AA}, minimum $P$ occurs at approximately the same location as peak AIA 193 {\AA} emission.

\cite{Cheng} examined the structure in white-light with the K-Cor instrument, measuring the plasma-sheet to be 2.5 times larger in polarized brightness ($pB$) than seen in AIA 193 {\AA}.
This difference may be related to the dependencies of EUV and $pB$ intensities on plasma density $n$ as $n^2$ and $n^1$ respectively. \ion{Fe}{13} emission theoretically depends on $n^{\alpha}$, where $\alpha$ is closer to 1 than 2
owing to radiative excitation
and some collisional depopulation.

Polarization Azimuth angles $\theta$ are shown in Figure \ref{fig:polarization}G. The color map shows angle $\theta$ relative to the local radial, and white lines plot the vectors associated with this angle. Plotted vector length is proportional to $-1/\log(P)$. Polarization vectors are also shown in Figure \ref{fig:polarization}E. The polarization vectors are close to radial above and below the plasma-sheet, and apparently trace the outline of the flare loops and overlaying magnetic field. Beneath this region, azimuth angles are near tangential to the solar
surface. Such behavior is unusual, as azimuth angles normally flip by 90$^\circ$ after crossing $\theta_{VV} \approx 54^\circ$. It can occur under conditions where there is a particular symmetry along the LOS.

Taking a cross-section of polarization azimuths across the sheet, we see the angles moving from $-20^{\circ}$ to $0^{\circ}$, interrupted by a large dip to $-30^{\circ}$. The peak of the azimuth drop is at the same location as maximum AIA 193 {\AA} emission and minimum \ion{Fe}{13} polarization. This may be a measurement artifact, as noise in $U$ and $Q$ increase as $P$ decreases.

\section{Interpretation}

Linear polarization is created throughout the solar corona. There are only two mechanisms by which linear polarization can be reduced. Firstly, collisions by thermal particles can locally destroy atomic polarization.
Secondly, integrations along the LOS and across the POS can both reduce the net polarization observed, dependent on $\theta_B$.
At least one of these processes must be responsible for the significant and broad drop in polarization observed across the plasma-sheet.

\subsection{Collisions}

\begin{figure
  \centering
  \includegraphics[width=8.5cm]{kcor.eps}
  \caption{
  Top) Theoretical density curve for Fe XIII 1074.7 to 1079.8 nm intensity ratio. The dashed lines mark the measured ratio at 1050\arcsec\ above the limb, with corresponding density at this location.
  Middle) Time averaged K-Cor polarized brightness ($pB$) observations from 18:00 - 19:30 UT, with units B/Bsun. Blue dashed line marks the location of the cross-section in the panel below.
  Bottom) Variation in $pB$ along the plasma-sheet.
  }
  \label{fig:kcor}
\end{figure}

\begin{figure*
  \centering
  \includegraphics[width=14.5cm]{simulation.eps}
  \caption{Maps of linear polarization $P$ for plasma-sheet models, with associated cross-sections. CoMP occulting disk position is marked by the red curved line, and polarization vectors as red dashes. Cross-section locations are marked by the blue and green dashed lines, corresponding to the plot color of the cross-section. Models show:
  AB) Laminar plasma-sheet, with magnetic field parallel to the sheet direction.
  CD) Potential field model generated from infinite LOS line currents placed at \textit{unresolvable} intervals along the plasma-sheet, combined with a sub-surface dipole. This represents plasmoid reconnection within the current-sheet.
  EF) The same potential field model as above, but with currents placed at resolvable distances.
  GH) Nonphysical plasma-sheet with a randomly orientated field, analogous to plasma turbulence.
  }
  \label{fig:sim}
\end{figure*}

To determine if collisions are responsible for removing polarization in the plasma-sheet, we must estimate the density of the region.
The CoMP \ion{Fe}{13} 1074.7 nm and 1079.8 nm lines are a density sensitive pair. We
used the Coronal Line Emission (CLE) program \citep{Judge+Casini2001} to determine the relationship between the line intensity ratio and electron density (at 1.5 MK).
The 1079.8 nm emission is weak, extending only to the base of the plasma-sheet at $\sim1050$\arcsec. At this height, we calculate an electron density at 1.5 MK of $2.8 \times 10^8$ cm$^{-3}$, based on an intensity ratio of 0.27 (Figure \ref{fig:kcor}).

At higher altitudes, this density is likely even lower. We can demonstrate this by measuring the change in total electron density with height, as it is proportional to the polarized brightness $pB$ measured by K-Cor (Figure \ref{fig:kcor}). $n_e$ varies as

\begin{equation}
  n_e \approx \frac{pB} {6.65\times10^{-25} 0.11 \ell},
  \label{eqn:pB}
\end{equation}

\noindent
where $\ell$ is the integration length along the LOS (\citealp{1990ApJ...349..656O}).

At an altitude of 1115\arcsec, $pB=0.5\times10^{-6}$. Therefore, if $\ell$ is greater than the observed plasma-sheet width $w\approx 5$ Mm, $n_e < 1.4\times 10^{10} $ cm$^{-3}$. Assuming $\ell \approx 30$ Mm \citep{Cheng},
$n_e \approx 2\times10^9$ cm$^{-3}$.
These densities are not high enough to destroy atomic polarization via collisions. We therefore conclude that this is unlikely the cause of low linear polarization in the plasma-sheet.

\subsection{Magnetic field structure within the plasma-sheet}
Levels of linear polarization are dependent on magnetic field structure and orientation. The approach of $P$ to zero for angles
near $\theta_{VV} \approx 54^\circ$ suggests that the small values of $P$ can be accounted for either by a large-scale field close to this angle, or by a more structured field in the POS and/or LOS that contains a mix of angles $\theta_B$.

The morphology of the dark triangular structure in $P$ (Figure \ref{fig:polarization}E) strongly suggests that the Van Vleck effect is operating at the edge of the arcade field, as magnetic field lines wrap around the large-scale current systems producing them.
Such magnetic null lines are commonly seen in
calculations and data \citep[e.g.][]{Judge+Low+Casini2006,Gibson}.
However, the geometry of a Sweet-Parker plasma-sheet, with a magnetic field direction close to radial, is incompatible with continuous Van Vleck nulls produced in this fashion. Such a configuration is shown in Figure \ref{fig:sim}A, modeled in CLE as an infinitely long laminar current-sheet. Here, we see almost no drop in polarization (Figure \ref{fig:sim}B). Therefore, the levels of $P$ measured by CoMP are inconsistent with a laminar Sweet-Parker current-sheet in the standard eruptive flare model.

Small-scale magnetic structures, such as plasmoids or a turbulent magnetic field (formed perhaps as a result of current-sheet instabilities), naturally lead to variations in $\theta_B$. These structures would therefore cause an overall reduction in $P$, especially if unresolved. To explore such an effect we made simple numerical models using CLE to compare with observations. These simple calculations (Figure \ref{fig:sim}) show polarization levels $P$ and corresponding polarization vectors. Each case utilizes a similar geometry to CoMP observations, with the plasma-sheet centered around the line $y=-0.073$\arcsec$x-67.53$\arcsec. Sample polarization cross-section profiles are also shown.
The models assume that the plasma contributing mostly to the emission is confined to a narrow region within $10^{-2}R_\odot$ of the POS, to avoid LOS cancellations, and thus to
highlight effects of POS magnetic structure.

Our ``plasmoid'' models (Figures \ref{fig:sim} C\&E) consist of infinite LOS line currents (placed at intervals along the plasma-sheet), combined with the potential field generated from a sub-surface dipole. This 2D configuration is the simplest representation of what might constitute a series of magnetic islands formed by the plasmoid instability in the POS.

Figures \ref{fig:sim}C\&E show calculations of plasmoids with sizes below and above the resolvable limit respectively. In both cases, the interaction between the plasma-sheet edge and surface dipole form a black "V-shaped" structure, where field lines trace an angle close to the Van Vleck angle. The V-shapes
occur here as
magnetic field lines wrap
around the line currents
placed along the LOS within the plasma sheet. This is unlikely the cause of the similar structure in CoMP observations however, as the model relies on the infinite line currents to form this feature. Our primary region of interest is the plasma-sheet above this region.

In the unresolvable plasmoid model (Figure \ref{fig:polarization}C), polarization drops to a minimum of $P\approx0.01$ (Figure \ref{fig:polarization}D). The resolved plasmoid case (Figure \ref{fig:polarization}E) has much more variation in $P$ along the plasma-sheet however, varying greatly between the plasmoid edge and center. In this resolvable case, minimum polarization is calculated as $P\approx0.005$.

In addition to the plasmoid models, we calculated an un-physical model of a randomly orientated field configuration running along the plasma-sheet, again with plasma within $10^{-2}R_\odot$ of the POS
(Figure \ref{fig:sim}G). Across this structure, we calculate a drop in polarization of to $P\approx 0.015$.
In this case, using a random
field structure imitates the signal of physical fields which, when integrated over finite volumes, contain the same distribution of vector
magnetic fields.

Although these models are relatively simple, they provide an analogue for the polarization levels CoMP might observe for representative magnetic topologies. In both the plasmoid and random field cases, magnetic field orientation is shown to be capable of reducing polarization to that observed in this event. With future observations (given an adequate signal-to-noise and integration time), spectropolarimetric measurements can provide observational constraints for the theoretical nature and scale of magnetic substructure in the corona.

\section{Discussion}

In summary,
polarization data from CoMP seem to demonstrate three properties:
\begin{enumerate}
  \item A broad and gradual reduction of linear polarization
  across the plasma-sheet, with lowest amplitudes at the sheet center.
  \item No clear increase in IR intensity, in contrast with EUV emission.
  \item Coherent and large `V-shaped' structures of low polarization below the plasma-sheet, reminiscent of the Van Vleck nulls clear in earlier calculations. \citep{Judge+Casini2001}
  \item Near-tangential polarization vectors beneath the plasma-sheet, roughly aligned with the aforementioned dark `V-shaped' structures.
\end{enumerate}

The near-tangential polarization seen under the plasma-sheet is certainly unusual, as near-radial polarization is found far more frequently \citep[e.g.][]{Arnaud}. This is potentially a LOS integration effect through the plasma, canceling out only radial components of polarization. This could perhaps provide information on the large-scale field structure under the plasma-sheet, but is an area of future study and does not effect the conclusions drawn in this paper.

Although our simple plasmoid models can produce the minimum polarization levels observed by CoMP in the September 10th 2017 flare, they do not replicate the gradual and wide drop in the polarization structure, significantly broader than EUV observations of the plasma-sheet. Recent sophisticated calculations suggest a natural explanation, consistent with the observed behavior of $P$ across the sheet \citep{Stanier}. Cascades of plasmoids caused by fragmentation of finer and finer current-sheets
diffuse from modeled plasma-sheets much faster than the plasma itself. We might expect this to produce a similar polarization signature to that observed by CoMP in the later phases of
this event. It may also explain in part why the sheet was essentially invisible in
the measured Fe~XIII intensity, but visible in $P$.
We speculate that if CoMP had started observing at the start of the flare, we would have observed a polarization structure of similar width to observed intensity, broadening as the process calculated by
\cite{Stanier} evolves.

\section{Conclusions}

We find that the drop of linear polarization measured by CoMP in the September 10th 2017 flare is consistent with the presence of plasmoids and turbulent fluctuations in the magnetic field. While previous work has focused upon spatially resolvable features in images of the dynamic corona, we have shown that linear polarization
can serve as measure for random magnetic structure on sub-resolution scales. Our method provides a diagnostic to analyze the fragmentation of current sheets through the plasmoid instability, which creates a cascade of energy associated with magnetic-field fluctuations toward smaller scales, well below observable limits.

Our work is consistent with theoretical work suggesting the links between current-sheet dynamics, plasmoid fragmentation, and a turbulent cascade of energy associated with magnetic-field fluctuations.

We anticipate that the start of observations with DKIST will provide data of the necessary quality to further disentangle the intriguing physics discussed here. In particular, a spectrograph (in contrast to the CoMP filtergraph), could further explore the mystery of why $P$ is clearly
related to the plasma-sheet
but $I$ is not.

\acknowledgments
R.J.F. thanks the STFC for support via funding from the PhD Studentship, as well as NCAR for funding visits to the High Altitude Observatory via the Newkirk Fellowship. The National Center for Atmospheric Research is sponsored by the National Science Foundation. CoMP data services were provided by MLSO. LvDG and SAM are partially funded under STFC consolidated grant number ST/S000240/1. The authors would also like to thank Daniel Verscharen for his helpful thoughts on theoretical plasma physics.

\bibliographystyle{aasjournal}

redpajama_set_name: RedPajamaArXiv


text:
Baptist Christianity in Sichuan refers to the history and implantation of Baptist Christianity in the Chinese province of Sichuan (formerly romanized as Szechuan or Szechwan; also referred to as "West China").

History

Baptist Christianity was introduced into Sichuan by the American Baptist Missionary Union (ABMU, belonging to the American Baptist Churches USA). The first missionaries to reach the province were Rev. William M. Upcraft and Rev. George Warner, who sailed in 1889. The journey required many weeks before their arrival in Suifu (also, Suichaufu) the following year, where they established the mission's first station. Medical work was started by Rev. C. H. Finch in 1891, in the same year Rev. Robert Wellwood and his wife joined the mission.

At the end of 1892, the ABMU was represented by nine missionaries, with medical work, two preaching places, women's classes, a boys' school, a Sunday school and eleven converts. In 1893, twelve new workers joined the mission, and subsequently the opening of a new station in Jiading (Kiatingfu) in 1894. At that time, the number of missionaries connected with the West China Mission was twenty-two. A small church had been gathered at Xuzhou (Suifu). The remote character of the province and its need of Christian missionary labors lent a romantic and unusual interest to the work of the West China Mission, especially since that was the nearest approach of American Baptists to reaching the people of an unevangelized country, Tibet.

That same year (1894), Upcraft and H. J. Openshaw traveled to Yazhou (Yachowfu) and tried to rent some permanent quarters. This stirred up opposition and vile placards were posted abusing the foreigners. However, the tide was turned in favor of the missionaries after successfully treating the servant of an official bitten by a snake, they were allowed to stay.

In 1895, a serious outbreak of anti-foreign agitation began in the capital Chengdu (Chengtu), and thence spread throughout the province. The missionaries had no choice but to temporarily leave their posts. Work was resumed after their return in the spring of 1896. By the middle of the year 1900, the Church had 68 converts with some 200 names on the enquirers' roll. The year 1900 was marked by the anti-Christian uprising known as Boxer Rebellion. Although this unrest did not affect Sichuan so much as some other parts of China, missionaries were obliged by consular orders to retire to the coast. During their absence, the local converts defended their faith and carried on all the regular services. Two new stations were opened at Ningyuan and Chengdu in 1905 and 1909 respectively; while Rev. Joseph Taylor and his wife were transferred from Yazhou to Chengdu.

In 1910, the ABMU changed its name to American Baptist Foreign Mission Society (ABFMS), and became one of the four founding societies of the West China Union University, together with American Methodist Episcopal Mission (Methodist Episcopal Church), Canadian Methodist Mission (Methodist Church of Canada), and Friends' Foreign Mission Association (British Quakers).

During the 1911 Revolution which overthrew the Qing dynasty, Openshaw took care of the wounded, with his wife as auxiliary. The local Christians later told of Mrs. Openshaw's bravery during the siege of Yazhou, how she would play the organ and sing while bullets whizzed about the house.

In 1919, the ABFMS celebrated the thirtieth anniversary of its West China Mission. In 1920, Rev. A. G. Adams assumed responsibility for the work of the evangelistic field, which had been for several years under the direction of Rev. David Crockett Graham, a polymath Baptist minister who was ordained at the First Baptist Church of Fairport, New York, in 1911, and spent nearly forty years in Sichuan Province, arriving shortly after his ordination. He was also one of the key figures in the discovery of the archaeological site now known as Sanxingdui, when a collection of jade pieces contributed to the Museum of Art, Archaeology and Ethnology at the West China Union University by an English Anglican missionary, Vyvyan Donnithorne, in 1931, drew his attention, subsequently leading to an archaeological excavation in 1934.

By 1913, the American Baptists had 793 church members; and by the end of 1921, 1,263 members.

In 1924, a Swedish American missionary Esther Nelson was sent to Sichuan by the First Swedish Baptist Church of Minneapolis. Between 1924 and 1945, she worked primarily as a nurse and medical educator in various Baptist hospitals. She applied to become a full-time evangelist after the formation of the Baptist General Conference's Foreign Mission Board in 1945. This led her to the city of Huili in Southern Sichuan at the end of 1947, where she worked until 1950, when foreign missionaries were driven out of China by the newly established communist regime.

In 1938, Alfred James Broomhall, an English Baptist missionary, entered China through the China Inland Mission. In 1946, he entered the territory of the Independent Nuosu in Southern Sichuan, with a team to establish a sustained Christian witness among them. He was only able to live among the Nuosu people from 1947 to 1951, and spent his last few months under house arrest before being expelled from China by communist regime; but his team was able to plant seeds that were going to bear fruit in coming decades.

Current situation

After the communist takeover of China in 1949, Protestant Churches in China were also forced to sever their ties with respective overseas Churches, which has thus led to the merging of all the denominations into communist-sanctioned Three-Self Patriotic Church.

The Cooperative Baptist Fellowship (CBF) and Hua Mei International (a non-profit Chinese Christian organization) provided critical relief supplies such as food, blankets and other necessities after the 2008 Sichuan earthquake. Two CBF field personnel Bill and Michelle Cayard also helped three pastors at a Protestant church in Bazhong with its growing congregation, which was ill-equipped to meet the needs of an increasing number of converts.

Surveys published in 1913

See also

 Christianity in Sichuan
 Catholic Church in Sichuan
 Protestantism in Sichuan
 Anglicanism in Sichuan
 Methodism in Sichuan
 Quakerism in Sichuan
 Seventh-day Adventist Church in Sichuan
 Anti-Christian Movement (China)
 Anti-missionary riots in China
 Denunciation Movement
 House church (China)

References

Bibliography

Sichuan
History of Christianity in Sichuan

redpajama_set_name: RedPajamaWikipedia


text:
Xiaomi India ED Case: Company Says All 'Payments' Done Via RBI-Approved Banking Channels
George Mayer October 3, 2022 3 min read
Source: indianexpress.com
Xiaomi India has issued an in-depth statement regarding the assets worth Rs 5,551.27 crore that were seized by the Foreign Exchange Management Act (FEMA) authority
Xiaomi India has issued an in-depth statement regarding the assets worth Rs 5,551.27 crore that were seized by the Foreign Exchange Management Act (FEMA) authority, claiming that nearly 84 per cent of the same is due to be paid as royalties to Qualcomm. Xiaomi's assets were seized for alleged violations of foreign exchange regulations with the ED claiming the company remitted large amounts of money abroad to related entities in the name of royalties without actually utilising any services from them. ED had also questioned Xiaomi's global vice-president Manu Kumar Jain and earlier India managing director over the issue.
The Enforcement Directorate (ED) seized the assets in April this year and the FEMA authority held on September 30 that the ED is right in holding foreign exchange equivalent to Rs 5,551.27 crore.
So what is Xiaomi's defense? Here's a look at the company's response to the latest order
Xiaomi has stated that it is Xiaomi India is an affiliate and one of the Xiaomi Group companies, which entered into a legal agreement with Qualcomm Group (USA) to license intellectual property for manufacturing smartphones. The statement adds that both Xiaomi and Qualcomm "believe that it is a legitimate commercial arrangement for Xiaomi India to pay Qualcomm royalty." Xiaomi says the payments are for Standard Essential Patents (SEPs) and IPs used in our "Indian version of smartphones."
For those who are not aware, Xiaomi and other smartphone manufacturers license several technologies from chipset manufacturers such as Qualcomm, Mediatek, etc, and must pay royalty feeds as part of the agreement. Xiaomi notes in the statement that this is standard practice across the entire global smartphone industry and without it, the smartphones will not work in India.
See also Amazon's Big Fall Product Launch Event Tonight: Here's What To Expect
The statement adds that "all royalty payments made by Xiaomi India were only related to sales done by Xiaomi India, and not for any other countries or regions. This has also been confirmed by the Qualcomm Group (USA)," adding that these payments were done via "RBI-approved and mandated banking channels and are legitimate commercial arrangements."
The company has also denied that it holds any assets outside India, the company, in this case, being Xiaomi Technology India Private Limited. Xiaomi adds that "Section 4 of FEMA does not even apply in this situation," which is the Foreign Exchange Management Act. According to Section 4, no person or entity shall transfer, hold any foreign exchange or immovable property outside of India.
What has ED stated against Xiaomi?
As we had noted in this earlier article, ED's charge is that "Xiaomi India has not availed any service from the three foreign based entities to whom such amounts have been transferred."
"Under the cover of various unrelated documentary façade created amongst the group entities, the company remitted this amount in the guise of royalty abroad which constitutes violation of Section 4 of the FEMA. The company also provided misleading information to the banks while remitting the money abroad," the ED statement had said earlier.
Is India's External Account Becoming Vulnerable?
Ponniyin Selvan Crosses Rs 230 Crore Globally. Here's A List Of Overseas Records Mani Ratnam Film Broke

redpajama_set_name: RedPajamaCommonCrawl


text:
Justia Regulation Tracker Executive Office Of The President Presidential Documents National American Indian Heritage Month, 2006, 64617-64618 [06-9061]
National American Indian Heritage Month, 2006, 64617-64618 [06-9061]
Download as PDF Federal Register / Vol. 71, No. 212 / Thursday, November 2, 2006 / Presidential Documents 64617 Presidential Documents Proclamation 8076 of October 30, 2006 National American Indian Heritage Month, 2006 By the President of the United States of America A Proclamation During National American Indian Heritage Month, we honor the generations of American Indians and Alaska Natives who have added to the character of our Nation. This month is an opportunity to celebrate their many accomplishments and their rich ancestry and traditions. America is blessed by the character and strength of American Indians and Alaska Natives, and our citizens are grateful for the countless ways Native Americans have enriched our country and lifted the spirit of our Nation. We are especially grateful for the Native Americans who have served and continue to serve in our Nation's military. These brave individuals have risked their lives to protect our citizens, defend our democracy, and spread the blessings of liberty to people around the world. My Administration is working to ensure that American Indians and Alaska Natives have access to all the opportunities of this great land. My fiscal year 2007 budget proposes more than $12.7 billion for government programs for Native Americans. Education is vital to ensuring all citizens reach their full potential, and my budget includes funding to help Native-American schools succeed and meet the requirements of the No Child Left Behind Act. The Bureau of Indian Affairs is providing education for approximately 46,000 American-Indian and Alaska-Native children. To help keep Native Americans safe, I have also proposed to increase law enforcement personnel and improve law enforcement facilities in American-Indian communities. My Administration will continue to work on a government-to-government basis with tribal governments, honor the principles of tribal sovereignty and the right to self-determination, and help ensure America remains a land of promise for American Indians, Alaska Natives, and all our citizens. hsrobinson on PROD1PC76 with PROPOSALS4 NOW, THEREFORE, I, GEORGE W. BUSH, President of the United States of America, by virtue of the authority vested in me by the Constitution and laws of the United States, do hereby proclaim November 2006 as National American Indian Heritage Month. I call upon all Americans to commemorate this month with appropriate programs and activities. VerDate Aug<31>2005 16:18 Nov 01, 2006 Jkt 211001 PO 00000 Frm 00001 Fmt 4790 Sfmt 4790 E:\FR\FM\02NOD2.SGM 02NOD2 64618 Federal Register / Vol. 71, No. 212 / Thursday, November 2, 2006 / Presidential Documents IN WITNESS WHEREOF, I have hereunto set my hand this thirtieth day of October, in the year of our Lord two thousand six, and of the Independence of the United States of America the two hundred and thirty-first. [FR Doc. 06–9061 Filed 11–1–06; 8:45 am] VerDate Aug<31>2005 16:18 Nov 01, 2006 Jkt 211001 PO 00000 Frm 00002 Fmt 4790 Sfmt 4790 E:\FR\FM\02NOD2.SGM 02NOD2 GWBOLD.EPS hsrobinson on PROD1PC76 with PROPOSALS4 Billing code 3195–01–P
[Federal Register Volume 71, Number 212 (Thursday, November 2, 2006)]
[FR Doc No: 06-9061]
Federal Register / Vol. 71, No. 212 / Thursday, November 2, 2006 /
Proclamation 8076 of October 30, 2006
National American Indian Heritage Month, 2006
During National American Indian Heritage Month, we
honor the generations of American Indians and Alaska
Natives who have added to the character of our Nation.
This month is an opportunity to celebrate their many
accomplishments and their rich ancestry and traditions.
America is blessed by the character and strength of
American Indians and Alaska Natives, and our citizens
are grateful for the countless ways Native Americans
have enriched our country and lifted the spirit of our
Nation. We are especially grateful for the Native
Americans who have served and continue to serve in our
Nation's military. These brave individuals have risked
their lives to protect our citizens, defend our
democracy, and spread the blessings of liberty to
people around the world.
My Administration is working to ensure that American
Indians and Alaska Natives have access to all the
opportunities of this great land. My fiscal year 2007
budget proposes more than $12.7 billion for government
programs for Native Americans. Education is vital to
ensuring all citizens reach their full potential, and
my budget includes funding to help Native-American
schools succeed and meet the requirements of the No
Child Left Behind Act. The Bureau of Indian Affairs is
providing education for approximately 46,000 American-
Indian and Alaska-Native children. To help keep Native
Americans safe, I have also proposed to increase law
enforcement personnel and improve law enforcement
facilities in American-Indian communities. My
Administration will continue to work on a government-
to-government basis with tribal governments, honor the
principles of tribal sovereignty and the right to self-
determination, and help ensure America remains a land
of promise for American Indians, Alaska Natives, and
all our citizens.
NOW, THEREFORE, I, GEORGE W. BUSH, President of the
vested in me by the Constitution and laws of the United
States, do hereby proclaim November 2006 as National
American Indian Heritage Month. I call upon all
Americans to commemorate this month with appropriate
thirtieth day of October, in the year of our Lord two
thousand six, and of the Independence of the United
States of America the two hundred and thirty-first.
[FR Doc. 06-9061
Filed 11-1-06; 8:45 am]


Hi, this is Marcus, creator of Skatessentials and fellow skate fanatic.
Over many years of skating I have come to realize that while skateboarding evolves continually, there are also certain basics, or essentials, the starting point for any great skater, that remain basically the same. I'm sure you are aware that there is no shortage of skateboarding sites on the internet, however the quality of information and interest to help fellow skaters is sometimes lacking.
This is where Skatessentials enters the scene. Here you will find a wealth of information designed to guide you to both learn how to skateboard and to improve and master your skate technique, articles on the different parts of a skateboard and their functions, skateboarding trends, clothing, pro skater bios and from time to time, interviews and exclusives from the most influential names in skateboarding, contests, prizes and giveaways.
Skatessentials is a community for skaters, a community for you. I encourage you to take part in conversation, leave your comments on each and every article that you love, article that you hate or even a suggestion or request. Don't see what you would like to see? Drop me a note.
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text:
Parameterized Complexity
by Rod G. Downey, Michael R. Fellows, Rolf Niedermeier, Peter Rossmanith, Rod G. Downey (wellington, New Zeal, Michael R. Fellows (newcastle, Rolf Niedermeier (tubingen, Peter Rossmanith (tu Munchen , 1998
"... the rapidly developing systematic connections between FPT and useful heuristic algorithms | a new and exciting bridge between the theory of computing and computing in practice. The organizers of the seminar strongly believe that knowledge of parameterized complexity techniques and results belongs ..."
on parameterized complexity, and it hopefully serves as a driving force in the development of the eld. 1 We had 49 participants from Australia, Canada, India, Israel, New Zealand, USA, and various European countries. During the workshop 25 lectures were given. Moreover, one night session was devoted to open
Content-based image retrieval at the end of the early years
by Arnold W. M. Smeulders, Marcel Worring, Simone Santini, Amarnath Gupta, Ramesh Jain - IEEE TRANSACTIONS ON PATTERN ANALYSIS AND MACHINE INTELLIGENCE , 2000
"... The paper presents a review of 200 references in content-based image retrieval. The paper starts with discussing the working conditions of content-based retrieval: patterns of use, types of pictures, the role of semantics, and the sensory gap. Subsequent sections discuss computational steps for imag ..."
. In the concluding section, we present our view on: the driving force of the field, the heritage from computer vision, the influence on computer vision, the role of similarity and of interaction, the need for databases, the problem of evaluation, and the role of the semantic gap.
Adolescence-limited and life-course-persistent antisocial behavior: Adevelopmental taxonomy
by Terrie E. Moffitt - Psychological Review , 1993
"... A dual taxonomy is presented to reconcile 2 incongruous facts about antisocial behavior: (a) It shows impressive continuity over age, but (b) its prevalence changes dramatically over age, increasing almost 10-fold temporarily during adolescence. This article suggests that delinquency conceals 2 dist ..."
A dual taxonomy is presented to reconcile 2 incongruous facts about antisocial behavior: (a) It shows impressive continuity over age, but (b) its prevalence changes dramatically over age, increasing almost 10-fold temporarily during adolescence. This article suggests that delinquency conceals 2
Self-discrepancy: A theory relating self and affect
by E. Tory Higgins - Psychological Review , 1987
"... This article presents a theory of how different types of discrepancies between self-state representa-tions are related to different kinds of emotional vulnerabilities. One domain of the self (actual; ideal; ought) and one standpoint on the self (own; significant other) constitute each type of self-s ..."
with agitation-related emotions (e.g., fear, threat, restlessness). Differences in both the relative magnitude and the accessibility of individu-als ' available types of self-discrepancies are predicted to be related to differences in the kinds of discomfort people are likely to experience. Correlational
Being There -- Putting Brain, Body, and World Together Again
by Andy Clark , 1997
The moderator–mediator variable distinction in social psychological research: Conceptual, strategic, and statistical considerations
by Reuben M. Baron, David A. Kenny - Journal of Personality and Social Psychology , 1986
"... In this article, we attempt to distinguish between the properties of moderator and mediator variables at a number of levels. First, we seek to make theorists and researchers aware of the importance of not using the terms moderator and mediator interchangeably by carefully elaborating, both conceptua ..."
In this article, we attempt to distinguish between the properties of moderator and mediator variables at a number of levels. First, we seek to make theorists and researchers aware of the importance of not using the terms moderator and mediator interchangeably by carefully elaborating, both conceptually and strategically, the many ways in which moderators and mediators differ. We then go beyond this largely pedagogical function and delineate the conceptual and strategic implications of making use of such distinctions with regard to a wide range of phenomena, including control and stress, attitudes, and personality traits. We also provide a specific compendium of analytic procedures appropriate for making the most effective use of the moderator and mediator distinction, both separately and in terms of a broader causal system that includes both moderators and mediators. The purpose of this analysis is to distinguish between the properties of moderator and mediator variables in such a way as to clarify the different ways in which conceptual variables may account for differences in peoples ' behavior. Specifically, we differentiate between two often-confused functions of third variables: (a) the moderator function of third variables, which
Attention and the detection of signals
by Michael I. Posner, Charles R. R. Snyder, Brian J. Davidson - Journal of Experimental Psychology: General , 1980
"... Detection of a visual signal requires information to reach a system capable of eliciting arbitrary responses required by the experimenter. Detection latencies are reduced when subjects receive a cue that indicates where in the visual field the signal will occur. This shift in efficiency appears to b ..."
Detection of a visual signal requires information to reach a system capable of eliciting arbitrary responses required by the experimenter. Detection latencies are reduced when subjects receive a cue that indicates where in the visual field the signal will occur. This shift in efficiency appears to be due to an alignment (orient-ing) of the central attentional system with the pathways to be activated by the visual input. It would also be possible to describe these results as being due to a reduced criterion at the expected target position. However, this description ignores impor-tant constraints about the way in which expectancy improves performance. First, when subjects are cued on each trial, they show stronger expectancy effects than when a probable position is held constant for a block, indicating the active nature of the expectancy. Second, while information on spatial position improves per-formance, information on the form of the stimulus does not. Third, expectancy may lead to improvements in latency without a reduction in accuracy. Fourth, there appears to be little ability to lower the criterion at two positions that are
Intrinsic and extrinsic motivations: Classic definitions and new directions
by Richard M. Ryan, Edward L. Deci - Contemporary Educational Psychology , 2000
"... Intrinsic and extrinsic types of motivation have been widely studied, and the distinction between them has shed important light on both developmental and educational practices. In this review we revisit the classic definitions of intrinsic and extrinsic motivation in light of contemporary research a ..."
Intrinsic and extrinsic types of motivation have been widely studied, and the distinction between them has shed important light on both developmental and educational practices. In this review we revisit the classic definitions of intrinsic and extrinsic motivation in light of contemporary research and theory. Intrinsic motivation remains an important construct, reflecting the natural human propensity to learn and assimilate. However, extrinsic motivation is argued to vary considerably in its relative autonomy and thus can either reflect external control or true self-regulation. The relations of both classes of motives to basic human needs for autonomy, competence and relatedness are discussed. © 2000 Academic Press To be motivated means to be moved to do something. A person who feels no impetus or inspiration to act is thus characterized as unmotivated, whereas someone who is energized or activated toward an end is considered motivated. Most everyone who works or plays with others is, accordingly, concerned with motivation, facing the question of how much motivation those others, or oneself, has for a task, and practitioners of all types face the perennial


text:
Humanities › Geography
Culture Hearths and Diffusion
The Source and Distribution of Cultural Ideas Around the Globe
Christopher Corr/Ikon Images/Getty Images
Key Figures & Milestones
Urban Geography
Amanda Briney
Geography Expert
M.A., Geography, California State University - East Bay
B.A., English and Geography, California State University - Sacramento
Amanda Briney, M.A., is a professional geographer. She holds a Certificate of Advanced Study in Geographic Information Systems (GIS) from California State University.
The word "culture" generally refers to a specific group's particular way of life. Culture includes the social meanings of various aspects of life, such as race, ethnicity, values, languages, religions, and clothing styles.
Though many distinct cultures are prevalent around the world today, those that are the most dominant have origins in one of a few areas called "culture hearths." These are the heartlands of various cultures and, historically, there are seven main locations from which the most dominant cultural ideas have spread.
Early Culture Hearth Locations
The seven original culture hearths are:
The Nile River Valley
The Indus River Valley
The Wei-Huang Valley
The Ganges River Valley
These regions are considered culture hearths because such key cultural practices as religion, the use of iron tools and weapons, highly organized social structures, and the development of agriculture started and spread from these areas. In terms of religion, for example, the area around Mecca is considered the culture hearth for the Islamic religion and the area from which Muslims initially traveled to convert people to Islam. The spread of tools, social structures, and agriculture spread in a similar manner from each of the culture hearths.
Culture Regions
Also important to the development of early culture centers are culture regions. These are areas that contain dominant cultural elements. Though not everyone in the culture region has the same cultural traits, they are often influenced by the center's traits in some way. Within this system, there are four components of influence:
The Core: the heart of the area that shows the most strongly expressed culture traits. It is usually the most heavily populated and, in the case of religion, features the most famous religious landmarks.
The Domain: surrounds the Core. Though it has its own cultural values, it is still strongly influenced by the Core.
The Sphere: surrounds the Domain.
The Outlier: surrounds the Sphere.
Cultural Diffusion
Cultural diffusion is the term used to describe the spread of cultural ideas from the Core (in the case of culture regions) and the culture hearth. There are three methods of cultural diffusion.
The first is called direct diffusion and occurs when two distinct cultures are very close together. Over time, direct contact between the two leads to an intermingling of the cultures. Historically this occurred through trade, intermarriage, and sometimes warfare because members of the various cultures interacted with each other for long periods. An example today would be the similar interest in soccer in some areas of the United States and Mexico.
Forced diffusion or expansion diffusion is the second method of cultural diffusion and takes place when one culture defeats another and forces its beliefs and customs onto the conquered people. An example of this would be when the Spanish took over lands in the Americas and later forced the original inhabitants to convert to Roman Catholicism in the 16th and 17th Centuries.
The term "ethnocentrism" is often related to forced diffusion. Ethnocentrism refers to the idea of looking at the world only from one's own cultural vantage point. As a result, people participating in this form of diffusion often believe that their cultural beliefs are superior to those of other groups and, in turn, force their ideas upon those they conquer.
In addition, cultural imperialism is usually placed into the category of forced diffusion as it is the practice of actively promoting cultural characteristics such as language, food, religion, etc., of one nation in another. Cultural imperialism normally occurs within forced diffusion because it frequently happens through military or economic force.
The final form of cultural diffusion is indirect diffusion. This type of diffusion happens when cultural ideas are spread through a middleman or even another culture. An example here would be the popularity of Italian food throughout North America. Technology, mass media, and the internet are all playing a huge role in promoting this type of cultural diffusion around the world today.
Modern Culture Hearths and Cultural Diffusion
Because cultures develop over time, new dominant areas of dominant culture have done so as well. Today's modern culture hearths are places such as the United States and world cities like London and Tokyo.
Areas such as these are considered modern culture hearths because of the prevalence of their cultural aspects now present throughout much of the world. Examples of modern cultural diffusion include the popularity of sushi in Los Angeles, California, and Vancouver, British Columbia and the presence of Starbucks in places like France, Germany, Moscow, and even in China's Forbidden City.
Direct diffusion has certainly played a role in this new spread of cultural values and products, and people are now moving around frequently because of today's ease of travel. Physical barriers such as mountain ranges and oceans no longer hinder people's movement, and there is a resultant spread of cultural ideas.
It is indirect diffusion, though, which has had the largest impact on the spread of ideas from places like the United States to the rest of the world. The internet and advertising through the many forms of mass media have allowed people worldwide to see what is popular in the U.S. As a result, blue jeans and Coca-Cola products can be found even in remote Himalayan villages.
In whatever ways cultural diffusion occurs now or in the future, it has happened many times throughout history and will continue to do so as new areas grow in power and pass on their cultural traits to the world. The ease of travel and modern technology will only aid in speeding up the process of modern cultural diffusion.
Briney, Amanda. "Culture Hearths and Diffusion." ThoughtCo, Dec. 6, 2021, thoughtco.com/culture-hearths-and-cultural-diffusion-1434496. Briney, Amanda. (2021, December 6). Culture Hearths and Diffusion. Retrieved from https://www.thoughtco.com/culture-hearths-and-cultural-diffusion-1434496 Briney, Amanda. "Culture Hearths and Diffusion." ThoughtCo. https://www.thoughtco.com/culture-hearths-and-cultural-diffusion-1434496 (accessed January 29, 2022).
Watch Now: How Money and Geography Impact Longevity
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What Is Identity Diffusion? Definition and Examples
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Vietnam Facts, History, and Profile
The Indus Valley Civilization


text:
Market Research and Development Appraisals
Project Management and Sales Support
Specification Solutions
Workplace student inspired to pursue a career in construction
This week, Slough Urban Renewal (SUR), is celebrating the success of a local student, who has just been awarded a permanent position with one of its sub-contractors, after successfully completing a series of work placements across a number of its development sites.
Callum Smith was previously a student at Langley College, where he was studying a BTEC Level 3 qualification in Construction & the Built Environment. To support the course, SUR offered the students an opportunity to take part in a two-week site office placement with Lovell Partnerships Ltd on its residential housing project at Wexham Green.
Callum was quick to put himself forward and after taking so much from the placement, he proactively pursued further opportunities to gain hands-on experience across SUR's sites.
Callum went on to complete a series of placements, firstly with Stepnell and then with Morgan Sindall Construction on the former library site in the heart of the town. Callum has since returned to complete a fourth work placement with SUR small sites contractor Life Build Solutions on the Alpha Street project. It is with Life Build that he has now received an offer of employment and he has been appointed as a Trainee Assistant Site Manager.
Ged Humphries, Training & Skills Coordinator for Slough Urban Renewal (SUR), said: "At SUR, it is important to us that we work together with our supply chain to create employment and skills opportunities for local residents. From offering work placements and trainee/graduate positions to attending careers/information days and industry events, we have been able to reach out to a wide audience, helping to raise awareness among young people about the vast and varied career opportunities available within the construction industry.
"Callum has been a fantastic student who has worked hard and shown great commitment, great enthusiasm and great promise. His new role is very much deserved, and we wish him every success in his future career in construction."
Alan Vaux, Construction Manager, LIFE Build added: "Callum is a welcome addition to our site team and in these troubled times, shows that LIFE Build take seriously its commitment to Social Value and local employment"
Earlier this year, Callum was awarded the SUR Gold Star Work Experience Award for being an outstanding work experience student and for successfully completing a series of work placements to an exceptionally high standard. Callum is now attending Uxbridge College where he is taking a HNC (Higher National Certificate) in Construction & the Built Environment, Level 4 course, which he will complete alongside his new role with Life Build.
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text:
Aulacidea hieracii est une espèce d'insectes hyménoptères galligènes de la famille des Cynipidae. Cette espèce européenne est inféodée aux Épervières.

Description et biologie

La galle provoquée par Aulacidea hieracii englobe la tige et peut atteindre  de diamètre, la partie de la plante située au dessus de la galle étant souvent avortée. Elle peut être lisse ou recouverte de poils blancs dressés. Une galle contient plusieurs larves blanches, chacune ayant sa propre loge. A. hieracii hiberne et nymphose à l'intérieur de sa galle. La reproduction sexuée n'a lieu qu'une seule fois par an ; une reproduction par parthénogénèse est également possible, la femelle créant alors une galle aux œufs non fécondés d'où émerge uniquement des mâles (arrhénotoque).

Les plantes hôtes de la larve dA. hieracii sont principalement des Hieracium dont Hieracium alpinum, H. inuloides subsp. tridentatifolium, H. lachenalii subsp. cruentifolium, H. laevigatum, H. maculatum, H. murorum, H. racemosum subsp. tenuifolium, H. sabaudum subsp. boreale, H. ubcaesium, H. tomentosum, H. umbellatum et H. virosum ainsi que Schlagintweitia intybacea.

Agent de régulation
À l'instar des nombreux phytopathogènes qui sont également des agents de régulation de leurs plantes hôtes, Aulacidea hieracii limite la diffusion des Épervières. Or, certaines espèces des genres Hieracium et Pilosella, peu problématiques sur leur aire de répartition d'origine, sont devenues des pestes végétales dans les régions où elles ont été importées artificiellement, en particulier dans les écozones australasienne et néarctique. Aulacidea hieracii, ou encore Aulacidea subterminalis et le Syrphidae Cheilosia psilophthalma, sont actuellement étudié afin de connaître leurs capacités de régulation de ces plantes invasives.

Répartition
Aulacidea hieracii est une espèce présente en Europe et plus précisément en Andorre, en Autriche, Grande-Bretagne, France, Allemagne, Hongrie, Pologne et Suède.

Synonymie
Selon le Muséum national d'histoire naturelle, situé à Paris :
 Aulacidea cacaliae Belizin, 1959
 Aulacidea hieracii (Bouché, 1834)
 Aulax artemisiae Thomson, 1877
 Aulax crassinervis Thomson, 1877
 Aulax foveiger Thomson, 1877
 Aulax graminis Cameron, 1875
 Aulax pigeoti Kieffer, 1898 (serait plus un synonyme dA. scorzonerae)
 Aulax schlechtendali Rübsaamen, 1896
 Aylax sabaudi Hartig, 1877
 Cynips hieracii Bouché, 1834
 Cynips hieracii Linnaeus, 1758

Liens externes

 Photographies de galles, larves, nymphes et adultes dAulacidea hieracii dans la galerie du monde des insectes.

Notes et références

Espèce d'Apocrites (nom scientifique)
Insecte cécidogène


Here you have a list of opinions about Brassiere measurement and you can also give us your opinion about it.
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Brassiere measurement (also called brassiere size, bra size or bust size) refers to determining what size of bra a person wears and mass-producing bras that will fit most people. Bra sizes usually consist of a number, indicating a band size around the person's torso, and one or more letters indicating the breast cup size. Bra cup sizes were invented in 1932 and band sizes became popular in the 1940s.
Bra sizes vary from one manufacturer to another, and from country to country. People's bodies and breasts may not conform to the sizes offered by companies. As a result, some people have a difficult time finding a properly fitted bra. Up to 80% of women wear the wrong size bra, causing 40% to 60% to experience pain of one kind or another.
Bra sizing systems are typically used to label off-the-shelf bras and are not used for custom-made bras or bras built into other garments. Bra size labeling systems vary from country to country, while manufacturers do not adhere to international standards. Some manufacturers have been found to deliberately mis-state the band size. One study found that the label size was consistently different from the measured size. Furthermore, the shape, size, symmetry, and spacing of people's breasts vary considerably, and can differ greatly from the standard off-the-shelf bra shapes and sizes, especially if the breasts have been augmented, are tubular shaped, or if they sag.
In the image below, you can see a graph with the evolution of the times that people look for Brassiere measurement. And below it, you can see how many pieces of news have been created about Brassiere measurement in the last years.
Thanks to this graph, we can see the interest Brassiere measurement has and the evolution of its popularity.
What do you think of Brassiere measurement?
You can leave your opinion about Brassiere measurement here as well as read the comments and opinions from other people about the topic.


Detective Will Trent is standing in a Georgia convenience store, waiting on an obstinate ICEE frozen-drink machine. To the surveillance cameras and bored staff of the Lil' Dixie Gas-n-Go, however, Will appears to be someone very different - the menacing ex-con Bill Black. Going undercover as Bill, the Georgia Bureau of Investigation agent is about to infiltrate the most corrupt town in the most corrupt county in the new American South. But first: his ICEE.
If you're current on your Will Trent info, you know Will has a poor diet. He likes his sweets. Breakfast sometimes involves a donut and for lunch usually a hotdog.
In Busted, Will stops at a convenience store to get himself an ICEE frozen drink when bullets start flying. But Will is not dressed with his usual 3-piece-suit. Instead, he's in disguise as his undercover character, ex-con Bill Black.
Will's bad luck has him there at the wrong time and at the wrong place. Or maybe he's at the right place and he's there to prevent further damage. The aftermath leaves too many bodies for the GBI. Piecing together the reason for the crime and the culprit is up to Will, Faith, and Amanda.
As always, I love Will's character. Amanda gives him such a hard time but the truth is that Will's brain is amazing. He has a great partner in Faith, making them a great team of investigators.
Busted also gives you the idea where the next book is going. Lena will return in the next book: Unseen.


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Vandy Beth Glenn was fired from her job with the state of Georgia after transitioning from male to female.
After years-long legal battle, transgender woman returns to work
By Emma Lacey-Bordeaux, CNN Radio
Atlanta, Georgia (CNN) - Four years on, Vandy Beth Glenn still gets choked up thinking about the day she was fired from her perfect job.
The petite brunette recalls exactly what her boss said that October day, how the reasons behind the termination sparked a lawsuit that could have far-reaching implications about how transgender people are treated at work.
Vandy Beth Glenn was born Glenn Morrison. At a young age, she says, she knew she wasn't a man.
"It's like a constant voice in the back of your head telling you 'This is wrong. This isn't the life you are supposed to be living,'" she said.
The voice grew louder as the years went on, but the Georgia native moved through life, earning a journalism degree from the University of Georgia and serving as an officer in the U.S. Navy. She's fascinated by language, she says, loves to see how government works. In 2005, she landed her perfect job as a legislative editor at the Georgia General Assembly.
Around that time, Glenn's life outside work began to change, too.
Filed under: Discrimination • Gender • How we look • Who we are
Engage: Kwanzaa celebrations dwindling says poll
A poll shows Kwanzaa may be a holiday past its prime - The Root
Opinion: After a large turnout in 2008, the youth vote looms large in 2012 - Colorlines
With Aisha Khan found safe, people demand answers - CBS News
How other faiths celebrate on December 25th - CNN
Posted by Dan Merica -- CNN
Monji Dolon's immigration status makes it impossible to accept full-time work in the technology field.
Despite immigration reforms, many young immigrants still in limbo
By Yasmin Amer, CNN
(CNN) - It wasn't until his senior year of high school in North Carolina that Monji Dolon found out about his murky immigration status.
His family had emigrated from Bangladesh in 1991 when Dolon was 5 years old and since then Dolon, his mother and his brother have lived without legal residency in the United States.
Uncertain of what to check under "residency" on his college applications, Dolon learned at the age of 18 that he was in an ongoing battle to stay in the country he had grown up in.
"I remember having a huge sense of panic at the time," say Dolon, now 25.
The Department of Homeland Security announced reforms this year that would halt the deportations of young immigrants who pose no threat to security. It said it also would review almost 300,000 cases on an individual basis - something it had not been done before.
Individuals without a criminal record are considered low priority for forced or immediate deportation. But without permanent relief, many like Monji Dolon are still in immigration limbo.
Filed under: Education • How we live • Immigration


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NRP to Build Lone Star Brewery's First Apartments
The $300 million redevelopment project will include at least 750 residential units.
Anca Gagiuc
Lone Star Brewery
San Antonio—After receiving approval from the Zoning Commission earlier this month to turn the abandoned Lone Star Brewery into a mixed-use development, announcements continue with the developer selected for the first apartment building in the $300 million redevelopment project.
Cleveland-based NRP Group is under contract to acquire approximately 2.5 acres of land in the complex along the Mission Reach trail, reported San Antonio Express-News. The developer plans to build a five-story apartment building encompassing approximately 250 units; construction is scheduled to begin next summer and completed by late 2018.
Lone Star Brewery's lead developers, Aqualand Development of San Marcos and CBL & Associates Properties of Chattanooga, Tenn., have plans to include three multifamily properties in the 32-acre project, as well as 376,000 square feet of retail and office space. The residential component will total about 750 units, but it's not carved in stone as the project's developers might increase the space allocated for the residential segment as they buy more land.
Rendering courtesy of Aqualand Development
Allied Orion Breaks Ground on San Antonio-Area Community
GVA Real Estate Expands San Antonio Footprint
Goldmark Property Management Sells San Antonio Community
Passco Buys 380-Unit San Antonio Community
GVA Real Estate Group Acquires San Antonio Community


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View Google Analytics reporting within the application
Adding generic link tracking code
» Adding personalization to tracking code values
Adding Google Analytics tracking code
» Customizing Google Analytics tracking values
Viewing Google Analytics reporting within the application
You can automatically add tracking code to your campaigns' link URLs. For example, if you want to track where your traffic comes from, and your website has that
capability, then you can automatically have our system add a query string to links such as ?Ref=email
Link tracking can be custom tracking code (as above), or it can be Google Analytics tracking code, or you can edit and customize Google Analytics tracking values.
Tracking code allows you to gather valuable information on how your links are being used and how effective they are. Any Google Analytics data can also be pulled through into the application's reporting area.
All in all, adding tracking code to your links provides you with better site analytics.
To access Site analytics, select Campaigns > Advanced Features and then select the Site analytics tab.
To add a single generic query string to your outbound links (using analytics other than Google), click Add new under link tracking. The 'Link Tracking' window will open, enabling you to enter the link tracking field and the value you require.
For example, setting the field as 'Ref' and the value as 'email' will generate the following:
http://www.example.com/Ref=email
Adding personalization to tracking code values
You also have the ability to add contact data field personalization to values, by clicking on the personalization icon . This means a contact-specific value can be added into the link tracking code.
For example, if you set the field as 'country' and select the contact data field 'COUNTRY' from the personalization dropdown, you will generate the following:
http://www.example.com/country=@COUNTRY@
Thus, if ' 'United States' is stored against the contact's 'COUNTRY' data field, United States will be added to the tracking code in place of @COUNTRY@.
Once happy with your new string, click on Save.
It will then appear under 'Link tracking', which is where all of your link tracking query strings will be listed.
From here you can delete and edit your link tracking query strings at any time.
Please note: When adding, removing or updating link tracking query strings and their values, changes will only take effect for existing campaigns once the campaigns are modified and re-saved. New campaigns that are subsequently created will have these values automatically applied, however. You will also be reminded of this within the application after having made the change.
To enable Google-friendly links, click the Google Analytics Tracking button positioned to the right. A window will appear to confirm the field and values you're adding:
Clicking Continue will add these under 'Link Tracking'. By doing this, you will have automatically added the following to your links:
utm_campaign=Your campaign name - noting which campaign it was that referred the user to the site
utm_medium=email - noting the medium by which someone arrived on the site
utm_source=Your company name - noting the name of the company referring the visitor to the site; this is the company name set under the 'My details' section in your 'Account settings'
As with generic link tracking code, you can also delete and edit (see below) Google Analytics tracking code.
Again, remember to modify and re-save any existing campaigns for any changes to take effect.
Customizing Google Analytics tracking values
If you don't want to use our default values for Google Anaytics tracking, you have the ability to customize them by clicking on Edit alongside the value you want to change.
For instance, you might want to customize a couple of the values as follows:
utm_medium=MyEmailMarketingProvider - the name of your email marketing provider/medium, so that will be us!
utm_source=email marketing
Clicking on Edit will open the 'Link Tracking' window, allowing you to enter your own value in the 'Value' field. Again, you can use the personalization function for contact-specific values.
Click Save to confirm any changes made and, once again, remember to modify and re-save any existing campaigns for any changes to take effect.
When checking your campaign reports in the application, you'll also want to see your Google Analytics data in there too, rather than having to also have Google Analytics open alongside your reporting. For your convenience, we've ensured that you can do this too.
To allow us to pull your Google Analytics data into reporting, you'll need to authorize the connection to Google Analytics.
Simply click the Authorize connection button. If you're logged into your Google account already, a box will pop up asking you to accept the connection request; if not, you'll need to enter your username and password before being asked to accept the connection request.
Now, when you go to reporting, you'll see a Google Analytics report option in the More reports... menu.
When you first open it we'll ask you which Google Analytics profile the campaign was for, and we'll remember this for next time. But you can always change it, this is handy for campaigns that may affect more than one of your profiles.
It's worth waiting at least 48 hours before checking your statistics because as well as waiting for users to receive your email, you may need to wait for Google Analytics to process any visiting activity.
Note: this feature is not available on all accounts. If you would like to upgrade to enable this feature, please speak to your account manager.


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Dealing With Anger Quotes
Reading and share top 11 famous quotes and sayings about Dealing With Anger by famous authors and people.
Top Dealing With Anger Quotes
Browse top 11 famous quotes and sayings about Dealing With Anger by most favorite authors.
Favorite Dealing With Anger Quotes
1. "At this juncture it is important to say something about Exodus 12:7. This verse implies that we are dealing with a ritual that did not involve atoning for sin, but rather was a rite of protection for God's people, a different though not unrelated matter. It involved a blood ritual to avoid God's last blow against the firstborn. Thus Passover and atonement were not originally associated, though apparently by Jesus' day there were some such associations. Notice that nothing at all is said or suggested here about Israel's sin, or about forgiveness. This ceremony is more like an insurance policy. Yes, the blood is to avert divine wrath, but it is not wrath against Israel's particular sins. In this case they simply happened to be too close to the danger zone, or in the line of fire. We must assume that this blood ritual arose before there even was a fully formed priesthood, for it is highly unusual to have such a ritual without any mention of involvement of priests."
Author: Ben Witherington III
2. "When you're in New York City or Los Angeles, even if you're not dealing with show business, there's still this sense that it's the center of the universe. And I think that's a really dangerous, limiting mindset."
Author: Ed Helms
3. "On the lowest level, this loss of soul turns the man into the hen-pecked husband who lives with his wife as though she were his mother upon whom he is solely dependent in all things having to do with emotions and the inner life. But even the relatively positive case where the woman is the mistress of the inner domain and mother of the home who simultaneously has the responsibility for dealing with all the man's questions and problems having to do with emotions and the inner life, even this leads to a lack of emotional vitality and sterile one-sidedness in the man. He discharges only the "outer" and "rational" affairs of life, profession, politics, etc. Owing to his loss of soul, the world he has shaped becomes a patriarchal world that, in its soullessness, presents an unprecedented danger for humanity. In this context we cannot delve further into the significance of a full development of the archetypal feminine potential for a new, future society."
Author: Erich Neumann
4. "The questioners had that beautiful detachment and devotion to stern justice of men dealing in death without being in any danger of it."
Author: Ernest Hemingway
5. "Be careful in dealing with a man who cares nothing for comfort or promotion, but is simply determined to do what he believes to be right. He is a dangerous uncomfortable enemy, because his body, which you can always conquer, gives you little purchase upon his soul."
Author: Gilbert Murray
6. "But it is well to remember that we are dealing with nations every one of which has a direct individual interest to serve, and there is grave danger in an unshared idealism."
Author: Henry Cabot Lodge
7. "My recipe for dealing with anger and frustration: set the kitchen timer for twenty minutes, cry, rant, and rave, and at the sound of the bell, simmer down and go about business as usual."
Author: Phyllis Diller
8. "Never assume that the person you are dealing with is weaker or less important than you are. Some people are slow to take offense, which may make you misjudge the thickness of their skin, and fail to worry about insulting them. But should you offend their honor and their pride, they will overwhelm you with a violence that seems sudden and extreme given their slowness to anger. If you want to turn people down, it is best to do so politely and respectfully, even if you feel their request is impudent or their offer ridiculous."
Author: Robert Greene
9. "We're dealing here," said Vimes, "With a twisted mind.""Oh, no! You think so?""Yes.""But... no... you can't be right. Because Nobby was with us all the time.""Not Nobby," said Vimes testily. "Whatever he might do to a dragon, I doubt if he'd make it explode. There's stranger people in this world than Corporal Nobbs, my lad."Carrot's expression slid into a rictus of intrigued horror."Gosh," he said."
10. "And I told him that a man's life is always dealing with permanence - that the most dangerous kind of irresponsibility is to think of your doings as temporary. That, anyhow, is what I've tried to keep before myself. What you do on the earth, the earth makes permanent."
Author: Wendell Berry
11. "A man's life is always dealing with permanence, that is the most dangerous kind of irresponsibility is to think of your doings as temporary."
Dealing With Anger Quotes Pictures
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[Our] first and foremost duty [is] to seek the Lord until we open the path of communication from God to our own soul."
Author: Brigham Young
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Cossack 124 Manufacture and sale of nets constructions. Mesh netting, netting welded masonry, armopoyas, plastering mesh welded mesh woven. Fencing systems welded galvanized mesh coating. Making metaloizdely under the order. Installation, delivery. Sell waste oil stoves, cast iron stoves sales burzhuiki solid fuel.


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Home Software Browsers Chrome for Android vs Opera Browser – Which one should be your...
Chrome for Android vs Opera Browser – Which one should be your default browser on your Android Smartphone
Opera has always been an underrated Browser, a decade ago, when smartphones who are only capable of opening wap versions of websites, Opera browser that made its entry to the Mobile World. It was one of the first browsers to give complete browsing experience on mobile phones, especially Nokia.
But with the downfall of Nokia and rise of Android smartphone, Opera wasn't fast enough to switch sides to stay relevant.
It was too late when Opera made its entry into the Android ecosystem, it's really is for the iOS was delete the folder.
Despite having a delayed entry, the Opera browser has been working very hard to bring amazing features to it's Android. We have seen a lot of iterations of its Android browser over the last few years.
The current version that is available in 2018 looks matured and drinks features required in a modern mobile browser.
But, does having all that functionality, make it a suitable browser that can replace Chrome for Android? Let's compare them both.
Let's talk about the user interface
The look and feel of both the browsers, Chrome for Android might look more familiar to you in case if you are using it already, but if you look at Opera browser after installing it or maybe giving it a few hours of usage, you will realize that the user interface of Opera browser is actually better than Chrome for Android.
The Homepage of Chrome for Android and Opera Browser (Night Mode Enabled)
The navigation buttons in Chrome for Android or on the top while they are at the bottom of the Opera browser. Having the navigation buttons at the bottom makes it easier to switch between the tabs.
Though there is a workaround to move the navigation buttons in Chrome for Android at the bottom, which also brings the address bar town. It makes things easier especially when you have a smartphone with larger screen size, and mostly all the smartphones in the market these days have 6-inch of screen size on an average.
Both the browsers have personalized home page, with a reading section where news appears based on your browsing activity. In Opera, it also has a location-based section for articles.
Let's talk about exclusive features
Talking about exclusive features of Chrome for Android, the password manager is going to be really helpful if you use Google Chrome on your desktop as well. And it is perhaps one of the biggest reasons why people use Chrome for Android.
While Opera also has a similar type of feature where the bookmarks and login details on websites are synced across various platforms, we all know the market share of Opera on desktops, so you hardly be using this particular future if you are using Opera only on your mobile phone.
There isn't too much to talk about in both the browser since both are quite minimal and focus on giving a better browsing experience. However, the Opera browser has a night mode which is quite useful if you have a habit of browsing the web When The Lights Are Off.
Apart from the dark mode, Opera browser also supports themes and currently, it's Light, Dark, Red.
The browser also has a feature of blocking ads which can be enabled or disabled using a toggle button.
Other features include options to customize the way browser appears. Such as, you can choose to open tabs in background or foreground. You can also choose the app Layout, one will keep the navigation at the bottom and the address bar on the top and the other will stacks them together on the top.
You can turn on the full-screen option to browse pages in full-screen mode, with the notification bar is hidden unlike in the Chrome.
Despite all the similarities and differences between these Browsers, it all boils down to just one point. The choices aren't that tough to make, if you use Google Chrome on your PC, your pick should be Chrome for Android, and if you use Opera browser on your PC, it should be the Opera Browser on your Android.
If you are not dependent on Google Chrome to log you into several accounts, then I feel Opera browser brings more features for you to have a better browsing experience on your smartphone.
If I talk about myself, I rely heavily on Google Chrome's Password Manager and autofill, which makes Chrome for Android my primary Browser, but I have also kept the Opera browser just for the night mode and the full-screen browsing option.
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Windows Smart Security is a new scareware. This fake security application detects nonexistent infections to push users into buying a license. It is a clone of Total Security 2009 rogue.
Once registered, the detected infections have disappeared without any cleaning. Updating the database displays a balloon message, but no network activity.
BleepingComputer Windows Smart Security removal guide.


Midi Dirndl Mirelle for ladies by Stockerpoint in anthracite and spring. Provided with exclusive traditional patterns, the high-quality jacquard dirndl enchants with numerous loving details. The bodice is finished with delicate lace and the classic round neckline convinces with simple elegance. The traditional, silver-coloured buttons harmonize and set the unmistakable trend. The feminine, pleated skirt is equipped with a side pocket. The stylish apron in stripe design is wonderfully combined and refines this classic model.


Home > birds>Products for pigeons>Calcium for pigeons>Avizoon Natur Calcium-100 gr, (calcium enriched with phosphorus and amino acids).
- Excellent source of calcium and phosphorus - Essential for good shell quality of the eggs.
Product Name:Avizoon Natur Calcium-100 gr, (calcium enriched with phosphorus and amino acids).
Description: Avizoon Natur Calcium-100 gr, (calcium enriched with phosphorus and amino acids).
Path: Home > birds > Products for pigeons > Calcium for pigeons > Avizoon Natur Calcium-100 gr, (calcium enriched with phosphorus and amino acids).
Pantex Calcium Tab is a compound in tablets, calcium concentrate.
Nutritional supplement Calcium Vit. D3 Bayer Calcium Vit. D3 is indicated for use in females pregnant and lactating, in periods of growth and deficiency states of varying etiology in both dogs and cats. Covers the requirements of calcium, phosphorus and vitamin D3 in all cases in which the body needs an extra supply for the reasons mentioned above.
Quiko concentrated calcium is a liquid supplement daily, which helps and prevents calcium deficiency for birds. Calcium is essential for bones and feathers healthy, with less egg binding, egg shells quality, and the reduction of the plucking of the feather.


Tiffany Trump and Marla Maples both took to Instagram on Christmas Day to flaunt two charming pics of themselves cheerfully hanging out.
Tiffany Trump, 25, appeared to be upbeat to spend Christmas in New York City with her mother Marla Maples, 55, when she took to Instagram to flaunt a sweet pic of both of them presenting together. The preview included Christmas-themed channels of creature ears, a smaller than expected Santa Claus and a scaled down sweet stick as the mother-little girl pair grinned for the camera before a quite lit-up tree. Marla took action accordingly when she additionally posted an alternate pic of both of them spending the occasion together and in her photograph, they're grinning while at the same time wearing wreath-themed headband channels.
Tiffany and Marla's new pics are two of a couple of they've modeled for together consistently. Back toward the finish of Oct., the little girl of Donald Trump took to Instagram to share a few pics out of appreciation for Marla's birthday. In one pic, the blonde delights looked lovely while presenting in a lodging together, and in another, they were looking revived and cool as they presented before water.
It's incredible to realize that Tiffany appeared to make the most of her vacation with family. We can't resist the urge to think about how she'll commend acquiring the new year!