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

Rigorous three-dimensional (3D) simulations of neutrino-driven core-collapse supernovae have become highly successful in recent years \citep[e.g.,][]{melson_15b,lentz_15,takiwaki_14,burrows_19}, and have made clear headway in explaining the properties of supernova explosions and the compact objects born in these events \citep{mueller_17,Mueller2019,Burrows2020b,Powell2020, Bollig2020, mueller_20}.
The latest 3D models are able to reproduce a range of explosion energies up to $10^{51}\mathrm{erg}$ \citep{Bollig2020}, and yield neutron star birth masses, kicks, and spins largely compatible with the population of observed young pulsars \citep{Mueller2019,Burrows2020b}.

A number of ingredients have contributed, or have
the potential to contribute,  to make modern
neutrino-driven explosion models more robust.
Various microphysical effects such as
reduced neutrino scattering opacities due
to nucleon strangeness \citep{melson_15b} and nucleon correlations at high densities \citep{horowitz_17,Bollig2017,burrows_18}, muonisation \citep{Bollig2017}, and large effective nucleon masses \citep{yasin_20} can be conducive to neutrino-driven shock revival.

In addition, a particularly important turning point has been the advent of 3D \emph{progenitor} models and the recognition that
asphericities seeded prior to collapse can precipitate ``perturbation-aided'' neutrino-driven explosions
\citep{couch_13,couch_15, mueller_15a, mueller_16b,mueller_17,mueller_20,Bollig2020}. In perturbation-aided explosions, the moderately subsonic solenoidal velocity perturbation
in active convective shells at the pre-collapse stage
with Mach numbers of order $\mathord{\sim}0.1$
\citep{Collins2018} are transformed into strong
density and pressure perturbations at the
shock \citep{mueller_15a,takahashi_14,takahashi_16,abdikamalov_20}, and effectively strengthen the violent non-radial flow behind the shock
that develops due to convective
instability \citep{herant_94,burrows_95,janka_95,janka_96} and the standing accretion shock instability \citep{blondin_03,foglizzo_07}, thereby supporting neutrino-driven shock revival.

The discovery of perturbation-aided explosions has greatly enhanced interest in multi-dimensional models of late convective burning stages in massive stars. Several studies have by now followed the immediate pre-collapse phase of silicon and/or oxygen shell burning to collapse in 3D
\citep{couch_15,mueller_16b,mueller_16c,Mueller2019,Yoshida2019,Yadav2020,McNeill2020,yoshida_20}. In addition, there has been a long-standing strand of research since the 1990s \citep[e.g.,][]{bazan_94,bazan_97,meakin_06,meakin_07,meakin_07b,mueller_16c,jones_17,cristini_17,cristini_19} into the detailed behaviour of stellar convection during advanced burning stages with a view to the \emph{secular}  impact of 3D effects not captured by spherically symmetric stellar evolution models based on mixing-length theory \citep{Biermann1932,Boehm1958}. The details of convective boundary mixing by processes such as quasi-steady turbulent entrainment \citep{Fernando1991,strang_01,meakin_07}
or violent shell mergers \citep{mocak_18,Yadav2020} have received particular attention for their potential to alter the core structure of massive stars and hence affect the dynamics and final nucleosynthesis yields of the subsequent supernova explosion.

Three-dimensional simulations of convection during advanced burning stages have so far largely disregarded two important aspects of real stars -- rotation and magnetic fields. The effects of rotation have been
touched upon by the seminal work of \citet{kuhlen_03}, but more recent studies \citep{arnett_10,chatzopoulos_16} have been limited to axisymmetry (2D). Magnetohydrodynamic (MHD) simulations of convection, while common and mature in the context of the Sun \citep[for a review see, e.g.,][]{charbonneau_14}  have yet to be performed for advanced burning stages of massive stars.

Simulations of magnetoconvection during the late burning stages, both in rotating and non-rotating stars, are a big desideratum for several reasons.
Even in slowly rotating massive stars, magnetic fields may have a non-negligible impact on the dynamics of neutrino-driven explosions \citep{obergaulinger_14,Mueller2020}, and although efficient field amplification processes operate
in the supernova core \citep{endeve_12,Mueller2020},
it stands to reason that memory of the initial fields may not be lost entirely, especially for strong fields in the progenitor and early explosions. A better understanding of the interplay between convection, rotation, and magnetic fields in supernova progenitors
is even more critical for the magnetorotational explosion scenario \citep[e.g.,][]{burrows_07a,Winteler2012a,Mosta2014,moesta_18,Obergaulinger2020,Obergaulinger2020b,kuroda_20,aloy_21}, which probably
explains rare, unusually energetic ``hypernovae'' with energies of up to $\mathord{\sim}10^{52}\,\mathrm{erg}$.
Again, even though the requisite strong magnetic
fields may be generated after collapse by amplification processes like the magnetorotational insstability \citep{balbus_91,akiyama_03} or an $\alpha$-$\Omega$
dynamo in the proto-neutron star \citep{duncan_92,thompson_93,Raynaud2020}, a robust understanding of magnetic
fields during late burning is indispensable for reliable
hypernova models on several heads. For sufficiently
strong seed fields in the progenitor, the initial
field strengths and geometry could have a significant
impact on the development of magnetorotational explosions after collapse \citep{bugli_20,aloy_21}. Furthermore, our understanding of evolutionary pathways towards hypernova explosions
\citep{woosley_06,yoon_05,yoon_10,cantiell_07,aguilera_18,aguilera_20}
is intimately connected
with the effects of magnetic fields
on angular momentum transport in stellar interiors
\citep{spruit_02,heger_05,fuller_19,takahashi_20}.

Beyond the impact of magnetic fields on the pre-supernova
evolution and the supernova itself, the interplay of convection, rotation, and magnetic fields is obviously relevant to the origin of neutron star magnetic fields as well. It still remains to be explained what shapes the distribution of magnetic fields among young pulsars, and why some neutron stars are born as magnetars with extraordinarily strong dipole fields of up to $10^{15}\,\mathrm{G}$
\citep{olausen_14,tauris_15,Kaspi2017,Enoto2019}. Are these strong fields of fossil origin \citep{ferrario_05,Ferrario2009,schneider_20} or generated by
dynamo action during or after the supernova \citep{duncan_92,thompson_93}?
Naturally, 3D MHD simulations of  the late burning stages cannot comprehensively answer all of these questions. In order to connect to
observable magnetic fields of neutron stars, an integrated approach is required that combines stellar evolution over secular time scales, 3D stellar hydrodynamics, supernova modelling, and local simulations, and also addresses aspects like field burial \citep{vigano_13,torres_16} and the long-time evolution
of magnetic fields \citep{aguilera_08,de_grandis_20}.
Significant obstacles need to be overcome until  one
can construct a pipeline
from 3D progenitor models to 3D supernova simulations and beyond.
However, 3D MHD simulations of convective burning can already address meaningful questions despite the complexity of the overall problem.
As in the purely hydrodynamic case, the first step must be to understand the principles governing magnetohydrodynamic convection
during the late burning stages based on somewhat
idealised simulations that are broadly representative of
the conditions in convective cores and shells of massive stars.

In this study, we present a first simulation of magnetoconvection
during the final phase of oxygen shell burning using the
ideal MHD approximation. In the tradition of
semi-idealised models of late-stage convection, we use a setup
that falls within the typical range of conditions in the
interiors of massive stars in terms of convective Mach number
and shell geometry \citep[for an overview see][]{Collins2018}
and is not designed as a fully self-consistent
model of any one particular star.
This simulation constitutes a first
step beyond effective 1D prescriptions in stellar evolution models
to predict the magnetic field strength and geometry
encountered in the inner shells of massive stars at the pre-supernova
stage. We also compare to a corresponding non-magnetic model of
oxygen shell convection to gauge the feedback of magnetic fields
on the convective flow with a particular view to two important issues.
First, the efficiency of the ``perturbation-aided'' neutrino-driven mechanism
depends critically on the magnitude of the convective velocities
during shell burning, and  it is important to determine whether
magnetic fields can significantly slow down convective motions
as suggested by some recent simulations of solar convection
\citep{hotta_15}.
Second, magnetic fields could quantitatively
or qualitatively affect shell growth by turbulent entrainment,
which has been consistently seen in all recent 3D hydrodynamics
simulations of late-stage convection in massive stars.

Our paper is structured as follows. In Section \ref{sec:methods}, we describe the
 numerical methods, progenitor model, and initial conditions
 used in our study and discuss the potential role of non-ideal effects . The results of the simulations are  presented in Section~\ref{sec:results}. We first focus on the strength and geometry of the emerging magnetic field
and then analyse the impact of magnetic fields on the flow, and in particular
on entrainment at shell boundaries. We summarize our results and discuss their implications in Section~\ref{sec:conclusion}.

\begin{figure}
    \centering
    \includegraphics[width=\linewidth]{composition_s_rho.pdf}
    \caption{Profiles of selected mass fractions $X_i$ (top), density $\rho$, and specific
    entropy $s$ in the $18\, M_\odot$ \textsc{Kepler} stellar evolution model at the time
    of mapping to \textsc{CoCoNuT}. The boundaries of the simulated
    domain are indicated by dashed vertical lines. Note
    subtle differences to Figure~1 in \citet{mueller_16c}, which
    shows the same stellar evolution model at the onset of collapse.}
    \label{fig:1d_model}
\end{figure}

\section{Numerical Methods and Simulation Setup}
\label{sec:methods}

We simulate oxygen and neon shell burning
with and without magnetic fields
in a non-rotating $18\,M_\odot$ solar-metallicity star calculated using the  stellar evolution code \textsc{Kepler} \citep{Weaver1978, Woosley2002, Heger2010}. The same progenitor model has previously been used in the shell convection simulation of \citet{mueller_16c}.
The structure of the stellar evolution model at
the time of mapping to 3D is illustrated
in Figure~\ref{fig:1d_model}. The model contains
two active convective shells with sufficiently
short turnover times to make time-explicit simulations feasible.
The oxygen shell extends from
$1.75\, M_\odot$ to $2.25\, M_\odot$ in enclosed
mass and from $3,400\, \mathrm{km}$
to $7,900\,\mathrm{km}$ in radius, immediately
followed further out by the neon shell
out to $3.53\, M_\odot$ in mass and
$27,000\, \mathrm{km}$ in radius.

For our 3D simulations we employ the Newtonian magnetohydrodynamic (MHD) version of the  \textsc{CoCoNuT} code as described in \citet{Mueller2020}.
The MHD equations are solved in spherical
polar coordinates using the HLLC (Harten-Lax-van Leer-Contact) Riemann solver \citep{Gurski2004a, Miyoshi2005a}. The divergence-free condition $\nabla\cdot\mathbf{B} = 0$ is maintained using a
modification
of the original hyperbolic divergence cleaning scheme of \citet{Dedner2002} that allows for a variable cleaning speed while still maintaining total energy conservation using an idea similar to \citet{Tricco2016}. Compared to the original cleaning method, we rescale
the Lagrange multiplier $\psi$ to
$\hat{\psi}=\psi/c_\mathrm{h}$, where the cleaning speed $c_\mathrm{h}$ is chosen to be the fast magnetosonic speed. Details of this approach and differences
to \citet{Tricco2016} are discussed in Appendix~\ref{app:eglm}.
The extended system of MHD equations for the density $\rho$, velocity $\mathbf{v}$, magnetic field $\mathbf{B}$, the total energy density $\hat{e}$, mass
fractions $X_i$, and the rescaled Lagrange multiplier $\hat{\psi}$ reads,
\begin{eqnarray}
\partial_t \rho
+\nabla \cdot \rho \mathbf{v}
&=&
0,
\\
\partial_t (\rho \mathbf v)
+\nabla \cdot \left(\rho \mathbf{v}\mathbf{v}-
\frac{\mathbf{B} \mathbf{B}}{4\pi}
+P_\mathrm{t}\mathcal{I}
\right)
&=&
\rho \mathbf{g}
-
\frac{(\nabla \cdot\mathbf{B}) \mathbf{B}}{4\pi}
,
\\
\partial_t {\hat{e}}+
\nabla \cdot
\left[(e+P_\mathrm{t})\mathbf{u}
-\frac{\mathbf{B} (\mathbf{v}\cdot\mathbf{B})
{-c_\mathrm{h} \hat{\psi} \mathbf{B}}}{4\pi}
\right]
&=&
\rho \mathbf{g}\cdot \mathbf{v}
+
\rho \dot{\epsilon}_\mathrm{nuc}
,
\\
\partial_t \mathbf{B} +\nabla \cdot (\mathbf{v}\mathbf{B}-\mathbf{B}\mathbf{v})
+\nabla  (c_\mathrm{h} \hat{\psi})
&=&0,
\\
\partial_t \hat{\psi}
+c_\mathrm{h} \nabla \cdot \mathbf{B}
&=&-\hat{\psi}/\tau,
\\
\partial_t (\rho X_i)
+\nabla \cdot (\rho  X_i \mathbf{v})
&=&
\rho \dot{X}_i
,
\end{eqnarray}
where $\mathbf{g}$ is the gravitational acceleration, $P_\mathrm{t}$ is the total pressure, $\mathcal{I}$ is the Kronecker tensor, $c_\mathrm{h}$ is the hyperbolic cleaning speed, $\tau$ is the damping time scale for divergence cleaning, and $\dot{\epsilon}_\mathrm{nuc}$ and $\dot{X}_i$ are energy and mass fraction
source terms from nuclear reactions. This
system conserves the volume integral of a
modified total energy density $\hat{e}$,
which also contains the cleaning field $\hat{\psi}$,
\begin{equation}
{\hat{e}}
=\rho \left(\epsilon+\frac{v^2}{2}\right)+\frac{B^2+\hat{\psi}^2}{8\pi},
\end{equation}
where $\epsilon$ is the mass-specific internal energy.
Note that the energy equation differs from that in \citet{Tricco2016}
because we implement divergence cleaninng on a Eulerian grid
and do not advect $\psi$ with the flow unlike in their smoothed
particle hydrodynamics approach. If translated to the
Eulerian form of the MHD equations, the approach of
\citet{Tricco2016} would give rise to an extra advection
term in the evolution equation for $\psi$, which then
requires an additional term in the energy equation to ensure
energy conservation. In our Eulerian approach, these extra terms
are not needed.

Viscosity and resistivity are not included explicitly
in the ideal MHD approximation,
and only enter through
the discretisation of the MHD equations,
specifically
the spatial reconstruction, the computation of the Riemann fluxes, and the update of the
conserved quantities in the
case of reconstruct-solve-average
schemes.
\footnote{
For an attempt to quantify the numerical diffusivities,
see, e.g., \citet{rembiasz_17}. One should emphasise,
however, that that the concepts of numerical
and physical viscosity/resistivity must
be carefully distinguished. For one thing,
the numerical viscosity and resistivity
are problem-dependent as stressed by
\citet{rembiasz_17}. In the case of higher-order
reconstruction schemes, they are also
scale-dependent (and hence more akin
to higher-order hyperdiffusivities),
and they are affected by discrete
switches in the reconstruction scheme
and Riemann solver. Because of these
subtleties, the determination of the effective
(magnetic) Reynolds number of a simulation
is non-trivial
\citep[see Section~2.1.2 of][]{mueller_20}.
}
While this ``implicit large-eddy simulation'' (ILES) approach is
well-established for hydrodynamic turbulence \citep{grinstein_07}, the magnetohydrodynamic case
is more complicated because the behaviour in the relevant astrophysical regime of low (kinematic) viscosity
$\nu$ and
resistivity $\eta$ may still depend on the magnetic
Prandtl number $\mathrm{Pm}=\nu/\eta$. Different
from the regime later encountered in the supernova
core where $\mathrm{Pm}\gg 1$, oxygen shell burning is characterised by magnetic Prandtl numbers slightly below unity ($\mathrm{Pm} \sim 0.2$). With an effective Prandtl number of $\mathrm{Pm} \sim 1$
in the ILES approach \citep{federrath_11},
there is a potential concern that spurious small-scale dynamo amplification might arise due to the overestimation of the magnetic Prandtl number, or that saturation field strengths might be too high. The debate about the magnetic Prandtl number dependence in MHD turbulence is ongoing with insights from theory and simulations \citep[e.g.,][]{schekochihin_04,schekochihin_07,isakov_07,brandenburg_11,pietarila_10,sahoo_11,thaler_15,seshasayanan_17}, astrophysical observations \citep[e.g.,][]{christensen_09}, and laboratory experiments \citep{petrelis_07,monchaux_07}. There is, at the very least, the possibility of robust small-scale dynamo action and saturation governed
by balance between the inertial terms and Lorentz force terms down to the low values of $\mathrm{Pm}\sim 5\times 10^{-6}$ in liquid sodium experiments \citep{petrelis_07,monchaux_07}, provided that
both the hydrodynamic and magnetic Reynolds number are sufficiently high. An ILES approach that places the simulation into a ``universal'', strongly magnetised regime \citep{beresnyak_19} thus appears plausible. Moreover, even if the ILES approach were only to provide upper limits for magnetic fields and their effects on the flow, meaningful conclusions can still be drawn in the context of shell convection simulations.

The nuclear source terms are calculated with the 19-species nuclear reaction network of \citet{Weaver1978}. Neutrino cooling is ignored, since it becomes subdominant in the late pre-collapse phase as the contraction of the
shells speeds up nuclear burning.

The simulations are conducted on a grid
with $400\times128\times256$ zones in radius $r$, colatitude $\theta$, and longitude $\varphi$
with an exponential grid in $r$ and uniform
spacing in $\theta$ and $\varphi$.
To reduce computational costs, we excise the non-convective inner core up to $3000\,\mathrm{km}$ and replace the excised core with a point mass. The grid extends to a radius
of $50,000\, \mathrm{km}$ and includes a small part
of the silicon shell, the entire convective oxygen and neon shells, the non-convective carbon shell,
and parts of the helium shell.
Simulations that include the entire iron core
and silicon shell are of course desirable in future,
but the treatment of nuclear quasi-equilibrium
in these regions is delicate and motivates simulations
in a shellular domain instead, with a sufficient ``buffer''
region between the convectively active shells and the inner boundary of the grid. Due to the significant buoyancy jump between
the silicon shell and the oxygen shell, the flow in the convective
shell is largely decoupled from that in the
non-convective buffer region. Hydrodynamic
waves excited at the convective boundary and Alfv\'en waves along
field lines threading both regions can introduce some coupling, but these are excited by the active convective shell and not in the convectively quiet buffer region. No physical flux of waves
\emph{into} the oxygen region from below is expected. Moreover,
there is no strong excitation of waves at the convective
boundary in the first place because of the low convective Mach number
of the flow. It turns out that coupling by Alfv\'en waves can be neglected even more safely than coupling by internal gravity waves because of the Alfv\'en number of the flow; as we shall see
the Alfv\'en number always stays well below unity.

In order to investigate the impact of magnetic fields on late-stage oxygen shell convection, we run a purely hydrodynamic, non-magnetic simulation and an MHD simulation. In the MHD simulation, we impose a homogeneous magnetic field with $B_z = 10^{8}\,\mathrm{G}$
parallel to the grid axis as initial conditions. We implement reflecting and periodic boundary conditions in $\theta$ and $\varphi$, respectively. For the hydrodynamic variables we use hydrostatic
extrapolation \citep{mueller_20} at the inner and outer boundary, and
impose strictly vanishing advective fluxes at the inner
boundary.
Different from
\citet{mueller_16c}, we do \emph{not} contract
the inner boundary to follow the contraction and
collapse of the core.
This means that our models will not (and are not
intended to) provide an accurate representation of the
pre-collapse state of the particular $18 M_\odot$ star
that we are simulating. We would expect, e.g., that
for the particular $18 M_\odot$ model, the burning rate
and hence the convective velocities would increase
until the onset of collapse \citep{mueller_16c} due
to the contraction of the convective oxygen shell. As a consequence
of accelerating convection and flux compression, the magnetic
fields will likely also be somewhat higher at the onset of collapse.
The model is rather meant to reveal the physical principles
governing late-stage magnetoconvection in massive stars,
and to be \emph{representative} of the
typical conditions in oxygen burning shells with the understanding
that there are significant variations in convective Mach
number and shell geometry at the onset of collapse \citep{Collins2018},
which will also be reflected in the magnetic field strengths in the
interiors of supernova progenitors.

The inner and outer boundary conditions for the
magnetic fields are less trivial.
In simulations of magnetoconvection in the Sun,
various choices such as vertical boundary conditions
($B_x=B_y=0$), radial boundary conditions ($B_\theta=B_\varphi=0$), vanishing tangential
electric fields or currents, perfect-conductor
boundary conditions, or extrapolation
to a potential solution have been employed
\citep[e.g.,][]{Thelen2000, Rempel2014,Kapyla2018}.
Since our domain boundaries are separated from
the convective regions by shell interfaces with
significant buoyancy jumps, we opt for the
simplest choice of boundary conditions and merely
fix the magnetic fields in the ghost zones
to their initial values for a homogeneous vertical magnetic field. We argue that due to the buffer regions at our radial boundaries, and the lack of rotational shear, our choice of magnetic boundary conditions should not have a significant impact on the dynamically relevant regions of the star.

\section{Results}
\label{sec:results}

\subsection{Evolution of the Magnetic Field}
\label{subsec:magGeometry}

\begin{figure}
 \includegraphics[width=\columnwidth]{OxygenShell_MagneticField.pdf}
 \caption{Evolution of the volume-averaged (solid) and maximum (dashed) magnetic field strength within the oxygen shell.
 }
 \label{fig:B_field}
\end{figure}

\begin{figure*}
 \includegraphics[width=\linewidth]{2D_snapshots_equatorial.pdf}
 \caption{Snapshots of the equatorial plane in
 the MHD simulation at a time of  $500\, \mathrm{s}$,
 showing the inner part of the domain from the inner boundary at a radius of $3000 \, \mathrm{km}$
 out to $12,000\, \mathrm{km}$. The plotted part of the domain corresponds to the range $\mathrm{1.67\, M_\odot - 2.54\, M_\odot}$ in mass coordinate.} The panels display
 a) the ratio of magnetic to thermal pressure (i.e., inverse plasma-$\beta$), b) the magnitude of the magnetic field strength, c) the radial velocity and d) the silicon mass fraction.
 \label{fig:2Dslices}
\end{figure*}

Both the magnetised and non-magnetised model
were run for over 12 minutes of physical time, which
corresponds to about 17 convective turnover times.
Very soon after convection develops in the oxygen shell, the turbulent convective flow starts to rapidly amplify the magnetic fields in this region. To illustrate the growth
of the magnetic field we show the
root-mean-square (RMS) average and maximum value of the
magnetic field in the oxygen shell in Figure~\ref{fig:B_field}.The magnetic field, which we initialised at $10^8\, \mathrm{G}$, is amplified by over two orders of magnitude to over $10^{10} \,\mathrm{G}$ on average within the shell due to convective and turbulent motions. The average magnetic field strength in the shell is still increasing at the end of the simulation, but
the growth rate has slowed down, likely indicating that the model is approaching some level of magnetic field saturation. While we cannot with certainty
extrapolate the growth dynamics without
simulating longer, it appears likely
that RMS saturation field strength will settle somewhere around $\mathord{\approx} 2 \times 10^{10}\,\mathrm{G}$.

A closer look reveals that the magnetic field
is not amplified homogeneously throughout the
convective region. The convective eddies push the magnetic field lines against the  convective boundaries, where the fields are then more strongly amplified by shear flows. This is visualised in Figures~\ref{fig:2Dslices}a and \ref{fig:2Dslices}b, where both magnetic pressure and magnetic field strengths appear concentrated at the convective boundary. The maximum magnetic field strength
shown in Figure~\ref{fig:B_field} (dashed line) therefore essentially mirrors the field at the inner boundary of the oxygen shell
(not to be confused with the inner grid boundary). We observe a very quick rise in magnetic field strength at the boundary at the beginning of the simulation between $20 \texttt{-} 50\,\mathrm{s}$ once
the convective flow is fully developed. The rate of growth of the maximum magnetic field strength after this increases at approximately the same rate as the average magnetic field strength.

\begin{figure}
    \includegraphics[width=\columnwidth]{DipoleMagneticField.pdf}
    \caption{The angle-averaged root-mean-square (RMS) value
(black) and the dipole component (red) of the
radial magnetic field component $B_r$
as a function of mass coordinate at a time of $725\, \mathrm{s}$.
Note that the magnetic field strength drops dramatically
inside the thin, convectively stable  buffer region below
the oxygen shell, but exhibits a peak in the first radial zone,
which is merely a numerical artefact due to imperfect
boundary conditions.
    }
    \label{fig:Dipole}
\end{figure}

\begin{figure}
 \includegraphics[width=\linewidth]{MagneticFieldSpectrum.pdf}
 \caption{Power $\hat{M}_{\ell}^2$ in different multipoles $\ell$ of the radial field component
 of the magnetic field in the oxygen shell at different times. Dotted lines show the slopes
 of Kolmogorov ($k^{-5/3}$) and Kazantsev
 ($k^{3/2}$)  spectra. The low-wavenumber part of the spectrum
 is always distinctly flatter than a Kazantsev spectrum; at
 intermediate $\ell$, we see a Kolmogorov-like spectrum with a break
 around $\ell=30$ to a steeper slope
 in the dissipation range.
 }
 \label{fig:SphericalHarmonics}
\end{figure}

To characterise the geometric structure of the magnetic field, we show a radial profile of the dipole
of the radial magnetic field component\footnote{Strictly speaking, the most rigorous way to extract the dipole component of the magnetic field
 would use a poloidal-toroidal decomposition
$\mathbf{B}=
\nabla\times[\nabla \times (\mathcal{P}\mathbf{r})]
+
\nabla \times (\mathcal{T} \mathbf{r})$
where the scalar functions $\mathcal{P}$ and $\mathcal{T}$
describe the poloidal and toroidal parts of the field,
and consider \emph{all} components
$B_r$, $B_\theta$, and $B_\varphi$
arising from the $\ell=1$ component of
the poloidal scalar $\mathcal{P}$. Since the poloidal-toroidal decomposition cannot be reduced to a straightforward projection onto vector spherical harmonics,  this analysis is left to future papers.
} $B_r$ at the end of the simulation at $\approx 725\,\mathrm{s}$ (Figure~\ref{fig:Dipole}).
The dipole magnetic field in the convective regions is approximately an order of magnitude smaller than the RMS average radial magnetic field, aside from the first radial zone of our grid, where the dipole component is comparable to the total radial magnetic field. This behaviour at the grid boundary is likely an artefact of our choice of homogeneous magnetic fields at the inner boundary.  In general, however, the magnetic fields in the convective zones appear dominated by higher-order multipoles. Disregarding the dipole fields at the inner boundary, the dipole magnetic field of $\mathord{\approx} 10^9 \mathrm{G}$ or below lies in the upper range of observed dipole magnetic fields of white dwarfs \citep{Ferrario2015}, which have often been taken as best estimates for the dipole fields in the cores of massive stars.

\begin{figure}
 \includegraphics[width=\columnwidth]{AngularAverage_Stress.pdf}
 \caption{The radial  (solid) and non-radial (dashed)
 diagonal components of the
 Reynolds stress tensor
 $R_{ij}$ (black) and  Maxwell
 tensor $M_{ij}$ (red)
 for the MHD convection model at $725\,\mathrm{s}$ as a function of enclosed mass.}
 \label{fig:Stress}
\end{figure}

To further illustrate the small-scale nature of
the magnetic field within the oxygen shell, we show angular power spectra, $\hat{M}_{\ell}$ of the radial field strength at different times as a function of the spherical harmonics degree $\ell$ inside the oxygen shell at a radius of $\mathord{\approx} 5000\mathrm{km}$ (Figure~\ref{fig:SphericalHarmonics}).
$\hat{M}_{\ell}$ is
computed as:
\begin{eqnarray}
\hat{M}_\ell &=&
\frac{1}{8\pi}
\sum_{m=-\ell}^\ell \left|\int Y_{\ell m}^*(\theta,\varphi) B_r
\mathrm{d} \Omega\right|^2.
\end{eqnarray}

Very early in the simulation, the spectrum shows a significant
$\ell = 1$ dipole contribution, caused by our choice of homogeneous magnetic fields as an initial condition. It takes several convective turnovers before this contribution is no longer dominant. Throughout the evolution, the spectrum shows a broad plateau at small $\ell$ and a Kolmogorov-like slope at intermediate $\ell$,
which can be more clearly distinguished at late times when the first
break in the spectrum has moved towards lower $\ell$.
High-resolution studies are desirable to extend the inertial
range and confirm the development of a Kolmogorov spectrum at intermediate
wave numbers. The break in the spectrum moves towards smaller wave numbers and
the peak of the spectrum  shifts to larger scales from $\ell \approx  12$ to $ \ell \approx 7$.
Simulations of field amplification by a  small-scale dynamo in isotropic turbulence often exhibit a Kazantsev spectrum
with power-law index $k^{-3/2}$ on large scales.
Our spectra show a distinctly flatter slope below the spectral speak, indicating that field amplification is subtly different from the standard picture of turbulent dynamo amplification.

This is borne out by a closer look at the magnetic
field distribution within the convective region.
Somewhat similar to our recent simulation of field amplification by neutrino-driven convection in core-collapse supernovae \citep{Mueller2020}, field amplification does not happen homogeneously throughout the convective region and appears to be predominantly driven
by shear flows at the convective boundaries.
To illustrate this, we compare the
spherically-averaged diagonal components of the
kinetic (Reynolds) and magnetic (Maxwell) stress tensors
$R_{ij}$ and $M_{ij}$
in the MHD model at the final time-step of the simulation at $\mathord{\approx} 725\,\mathrm{s}$ (Figure~\ref{fig:Stress}).
$R_{ij}$ and $M_{ij}$ are computed as
\begin{eqnarray}
R_{ij}&=& \langle \rho v_i v_j\rangle, \\
M_{ij}&=& \frac{1}{8\pi}\langle B_i B_j\rangle,
\end{eqnarray}
where angled brackets denote volume-weighted
averages.\footnote{Note that no explicit decomposition of the velocity field into fluctuating components and a spherically averaged  background state is required since the background state is hydrostatic.}
The magnetic fields clearly remain well below
equipartition with the total turbulent kinetic
energy, and appear to converge to saturation
levels about one order of magnitude below, although
longer simulations will be required to confirm this.
The non-radial
diagonal components
$R_{\theta\theta}+R_{\varphi\varphi}$ and
$M_{\theta\theta}+M_{\varphi\varphi}$
are generally higher than the respective radial components $R_{rr}$ and $M_{rr}$. Throughout
most of the domain, the Maxwell stresses are
considerably smaller than the Reynolds stresses,
but it is noteworthy that the profile of the non-radial components of $M_{ij}$ runs largely parallel to those of
$R_{ij}$, just with a difference of slightly more than
an order of magnitude. Peaks of the magnetic
stresses at the shell interfaces suggest
that field amplification is driven  by shear
flow at the convective boundaries. Convective motions
then transport the magnetic field into the interior
of the convective regions and also generate radial
field components. The humps of $M_{rr}$ within the convection zones are less pronounced than in $R_{rr}$, which indicates that little
amplification by convective updrafts
and downdrafts takes place within the convection region.

At the outer boundaries of
the oxygen and neon shell, we observe
rough equipartition  between
$R_{rr}$ and $M_{\theta\theta}+M_{\varphi\varphi}$. The fact that the growth of the field slows down once the model approaches
$M_{\theta\theta}+M_{\varphi\varphi}\approx R_{rr} $ suggests that this ``partial equipartition'' may determine the saturation field strength, but
the very different behaviour at
the inner boundary with
 $M_{\theta\theta}+M_{\varphi\varphi}\gg R_{rr}$ argues against this. It is plausible, though, that the saturation
 field strength is (or rather will be) determined at the boundary. Linear stability analysis of the magnetised Kelvin-Helmholtz instability \citep[e.g.][]{chandrasekhar_61,Sen1963,Fejer1964,Miura1982,frank_96, keppens_99, ryu_00,obergaulinger_10, Liu2018} shows that shear instability, which is critical for efficiently generating small-scale fields, are suppressed by magnetic fields parallel to the direction of the shear flow as long as the Alfv\'en number
 is smaller than two. With kinetic fields well below equipartition
 (cp.~Figure~\ref{fig:Stress}), our models fall into the regime of low Alfv\'en
 number; hence the generation of non-radial fields at the boundaries may be self-limiting as a result of the stabilising impact
 of magnetic fields on the Kelvin-Helmholtz instability. A naive
 application of the principle of marginal stability would suggest saturation occurs
 once the Alfv\'en velocity at the boundary equals the shear velocity jump across the shell interface, which would imply
 $M_{\theta\theta}+M_{\varphi\varphi}\approx R_{\theta\theta}+R_{\varphi\varphi}$. Our simulation suggests that saturation probably occurs at significantly smaller values, and a more quantitative analysis of the saturation mechanism will clearly be required in future to elucidate the relation between the shear velocity (and possibly the width of the shear layer) and the saturation field strength.

 \begin{figure}
 \includegraphics[width=\columnwidth]{OxygenShell_KineticEnergy.pdf}
 \caption{Evolution of the total radial (solid) and non-radial (dashed) convective kinetic energy within the oxygen shell for the purely hydrodynamic (purple) and MHD (black) model, respectively.}
 \label{fig:E_kin}
\end{figure}

\begin{figure*}
 \includegraphics[width=\linewidth]{OxygenShell_subplots.pdf}
 \caption{Effects of entrainment on the oxygen shell for both the MHD model (black) and the equivalent purely hydrodynamic model (purple).  The panels show
 a) the inner and outer  oxygen shell radii, b) the total mass within the oxygen shell, c) the entrainment rate $\dot{M}$ into the oxygen shell, and
 d) the volume-integrated nuclear energy generation rate throughout the shell..
}
 \label{fig:OShellValues}
\end{figure*}

\subsection{Impact of Magnetic Fields on Convective Boundary Mixing}
\label{subsec:entrainment}

The slowing growth of the magnetic field indicates that feedback effects on the flow should become important during the later phase of the simulation. It is particularly interesting to consider the effect of the strong fields tangential to the oxygen-neon shell interface on convective boundary mixing, though we also consider potential effects on the flow in the
interior of the convective regions.

To this end, we compare the MHD model to a purely hydrodynamic simulation of oxygen and neon shell convection.
Figure~\ref{fig:E_kin} compares the total kinetic energy in convective motions in the
oxygen shell between the models.
The radial and non-radial components
$E_r$ and $E_{\theta, \varphi}$
of the kinetic energy are defined as
\begin{eqnarray}
E_r &=&\frac{1}{2} \int\limits_{r_- \leq r \leq r_+} \rho v_r^2 \,\mathrm{d}V,
\\
E_\mathrm{\theta, \varphi} &=&\frac{1}{2} \int\limits_{r_- \leq r \leq r_+} \rho (v_\mathrm{\theta}^2 + v_\mathrm{\varphi}^2 ) \,\mathrm{d}V,
\end{eqnarray}
where $r_-$ and $r_+$ are the inner and outer radii of the oxygen shell. We compute the inner
and outer shell radii $r_-$ and $r_+$ as the midpoints of the steep,
entropy slope between the oxygen shell and the silicon and neon shells below and above.  Due to shell
growth by entrainment, $r_-$ and $r_+$
are time-dependent (Figure~\ref{fig:OShellValues}a).

For both models most of the turbulent kinetic energy is in the non-radial direction. This
is different from the rough equipartition
$E_r \approx E_\mathrm{\theta, \varphi}$ seen in many simulations of buoyancy-driven convection
\citep{arnett_09}. There is, however,
no firm physical principle that dictates
such equipartition; indeed a shell burning simulation of the same $18\, M_\odot$ progenitor with the \textsc{Prometheus} code also showed significantly more kinetic energy in non-radial motions \citep{mueller_16c}. Ultimately, the high ratio $E_{\theta,\varphi}/E_r$ merely indicates that the fully developed flow happens to predominantly select eddies with larger extent in the horizontal than in the vertical direction.
\footnote{In the low-Mach number regime, the anelastic condition
$\nabla \cdot(\rho \mathbf{v})\approx 0$
implies a relation between the aspect
ratio of convective cells and the horizontal and vertical kinetic energy of any mode.}

Discounting stochastic variations, the radial component $E_r$ of the turbulent  kinetic energy for both the hydrodynamic and MHD model are  similar until the final $\mathord{\approx} 300\, \mathrm{s}$, at which point they start to deviate more significantly. Clearer differences
appear in the non-radial component $E_{\theta,\varphi}$, with the hydro model showing irregular episodic bursts in kinetic energy which are not mirrored in the MHD model. Since the only difference in
the setup of the two runs is the presence or absence of magnetic fields, this points to feedback of the magnetic field on the flow as the underlying reason, unless the variations are purely stochastic. Closer examination
suggests that feedback of the magnetic field on the flow is
the more likely explanation, and
the nature of this feedback will become more apparent as we analyse convective boundary mixing in the models.

To this end, we first consider the
evolution of the boundaries $r_-$ and $r_+$ of the
oxygen shell and the total oxygen
shell mass $M_\mathrm{O}$.
For computing the oxygen shell mass,
we take the (small) deviation of the boundaries from spherical symmetry into account more accurately than when
computing  $r_-$ and $r_+$, and integrate the mass contained in cells within
the entropy range
$3.8 \texttt{-}5.2 \, k_\mathrm{B}/\mathrm{nucleon} $.
As shown by Figure~\ref{fig:OShellValues}
(panels a and b), the oxygen
shell in the non-magnetic model grows slightly, but perceptibly faster without magnetic fields than
in the MHD model, starting
at a simulation time of about
$300\, \mathrm{s}$. The presence
of relatively strong magnetic fields
in the boundary layer apparently
reduces entrainment in line
with the inhibiting effect of
 magnetic fields parallel to the
 flow on shear instabilities
discussed in Section~\ref{subsec:magGeometry}.

The entrainment rate $\dot M=\mathrm{d} M_\mathrm{O}/\mathrm{d} t$
(Figure~\ref{fig:OShellValues}c)
is only slightly higher in the purely hydrodynamic model
most of the time, but the entrainment rate exhibits
occasional spikes, which do not occur in the MHD model. We note that these spikes in $\dot{M}$ occur at around the same times as the bursts in non-radial kinetic energy (Figure~\ref{fig:E_kin}). It appears that the
stabilisation of the boundary by magnetic fields
mostly suppresses rarer, but more
powerful entrainment events
that mix bigger lumps of material into
the oxygen shell. A comparison with the
shell burning simulations of \citet{mueller_16c} provides confidence that this effect is robust.
Because \citet{mueller_16c} contract the
inner boundary condition, convection grows more vigorous with time and their entrainment rates
are higher, adding about $0.05\, M_\odot$ to the
oxygen shell within $300\, \mathrm{s}$.
Their resolution test (Figure~20 in \citealt{mueller_16c}) only showed variations of $0.004\, M_\odot$ in the entrained mass
between different runs of the same progenitor model. In our
simulations, the oxygen shell only grows by
about $0.03\, M_\odot$ from $300\, \mathrm{s}$
to $700 \, \mathrm{s}$ (i.e, when the magnetic
field does not grow substantially any more),
yet we find a difference in shell growth
of about $0.01\, M_\odot$ between the
magnetic and non-magnetic model. It therefore
seems likely that there is indeed an appreciable systematic effect of magnetic fields on entrainment. Our simulations qualitatively illustrate such an effect,
but models at higher resolution are of course desirable
to more reliably quantify the impact of magnetic fields on turbulent entrainment.
The resolution requirements for accurate entrainment
rates are hard to quantify. Findings from extant numerical studies of the magnetised Kelvin-Helmholtz instability \citep[e.g.,][]{keppens_99} cannot be easily
transferred because of important physical differences (e.g., the lack
of buoyant stabilisation of the boundary). In purely
hydrodynamic simulations of entrainment during oxygen shell burning, resolving the
shear layer between the oxygen and neon shell with $\mathord{\approx} 15\texttt{-}22$ radial zones
as in our model was found to be sufficient for quantitatively credible,
but not fully converged results \citep{mueller_16c}.

The different entrainment rate also explains long-term, time-averaged differences in convective kinetic energy between the two simulations. The convective
kinetic energy is determined by the total nuclear
energy generation rate, which is shown in
Figure~\ref{fig:OShellValues}d.
Both models show an overall trend downwards over time in nuclear energy generation, which can be ascribed
to a slight thermal expansion of the shell and the depletion of fuel. After about $200\,\mathrm{s}$, the purely
hydrodynamics model exhibits a higher energy
generation rate, which persists until the end of the simulations and becomes more pronounced.
The higher energy generation rate
in the non-magnetic model is indeed mirrored
by a stronger decrease in the neon mass on the grid (Figure~\ref{fig:NeonMass}) of about
the right amount to explain the average
difference in energy generation rate
at late times. We note, however, that
the strong episodic entrainment events
in the purely hydrodynamic model are
\emph{not} associated with an immediate
increase in nuclear energy generation rate.
This is mainly because the energy release from the dissociation of the entrained neon is delayed and spread out in time as the entrained material is
diluted and eventually mixed down to regions
of sufficiently high temperature.

The overall effect of magnetic fields
on the bulk flow is rather modest.
We do not see a similarly strong quenching
of the convective flow by magnetic fields
as in  recent MHD simulations of the solar convection zone \citep{hotta_15}, who reported
a reduction of convective velocities
by up to $50\%$ at the base of the convection zone. Such an effect is not expected as long
as the magnetic fields stay well below kinetic
equipartition in the interior of convective shells as in our MHD simulation. Longer simulations will be required to confirm that  magnetic fields during late shell burning stages indeed remain ``weak'' by comparison and do not
appreciably influence the bulk dynamics of convection.

\begin{figure}
 \includegraphics[width=\columnwidth]{TotalNeonMass.pdf}
 \caption{Total mass of neon in the entire computational domain for the purely hydrodynamic simulation (purple) and the MHD simulation (black).}
  \label{fig:NeonMass}
\end{figure}

\section{Conclusions}
\label{sec:conclusion}
We investigated the amplification and saturation of magnetic fields during convective oxygen shell burning and the backreaction of the field on the convective flow by conducting a 3D MHD simulation
and a purely hydrodynamic simulation of an $18\, M_\odot$ progenitor shortly before core collapse.
The simulations were run for about 12 minutes of physical time (corresponding to about
17 convective turnover times), at which point field amplification
has slowed down considerably, though a quasi-stationary state has not yet been fully established.

The magnetic field in the oxygen shell is amplified to
$\mathord{\sim}10^{10}\, \mathrm{G}$ and dominated
by small-to-medium-scale structures with angular
wavenumber $\ell \sim 7$. The dipole component
is considerably smaller with $\mathord{\sim}10^9\, \mathrm{G}$ near the inner boundary of
the oxygen shell and less further outside.
The profiles of the radial and non-radial diagonal components $M_{rr}$ and  $M_{\theta\theta}+M_{\varphi\varphi}$ of
the Maxwell stress tensor mirror the corresponding
components $R_{rr}$ and
$R_{\theta\theta}+R_{\varphi\varphi}$ of the Reynolds stress tensor, but remain about an order of magnitude
smaller, i.e., kinetic equipartition is not reached.
However, $M_{\theta\theta}+M_{\varphi\varphi}$
can approach or exceed the radial
 component $R_{rr}$ at the convective boundaries.
The saturation mechanism for field amplification needs
to be studied in more detail, but we speculate that
saturation is mediated by the inhibiting effect of non-radial magnetic fields on shear instabilities at shell boundaries, which appear to be the primary driver of field amplification.

We find that magnetic fields do not have an appreciable effect on the interior flow inside the oxygen shell, but
observe a moderate reduction of turbulent entrainment at
the oxygen-neon shell boundary in the presence of magnetic fields. Magnetic fields appear to suppress stronger episodic entrainment events, although they do not quench entrainment completely. Through the reduced entrainment rate, magnetic fields also indirectly affect the dynamics inside the convective region slightly because they reduce the energy release through the dissociation of ingested neon, which results in slightly smaller convective velocities in the MHD model.

Our findings have important implications for core-collapse supernova modelling. We predict initial fields in the oxygen shell of non-rotating progenitors that are significantly stronger than assumed in our recent simulation of a neutrino-driven explosion aided by dynamo-generated magnetic fields \citep{Mueller2020}. With relatively strong seed-fields, there is likely less of a delay until magnetic fields can contribute the additional ``boost'' to neutrino heating
and purely hydrodynamic instabilities seen in
\citet{Mueller2020}. This should further contribute to the robustness of the neutrino-driven mechanism for non-rotating and slowly-rotating massive stars. Our simulations also suggest that the perturbation-aided mechanism \citep{couch_13,mueller_15a} will not be substantially affected by the inclusion of magnetic fields. Since magnetic fields do not become strong enough to substantially alter the bulk flow inside the convective region, the
convective velocities and eddy scales as the key parameters for perturbation-aided explosions remain largely unchanged.

The implications of our results for neutron star magnetic fields are more difficult to evaluate since the observable fields will, to a large degree, be set by processes during and after the supernova and cannot be simply extrapolated from the progenitor stage by magnetic flux conservation. That said, dipole fields of order $10^9\, \mathrm{G}$ at the
base of the oxygen shell -- which is likely to end up as the neutron star surface region -- are not in overt conflict with dipole fields
of order $10^{13}\, \mathrm{G}$ in many young pulsars inside supernova remnants \citep{Enoto2019}. However, considering the
relatively strong small-scale fields
of $\mathord{\sim}10^{10}\, \mathrm{G}$
with peak values over $10^{11}\,\mathrm{G}$,
it may prove difficult to produce neutron stars without strong small-scale fields at the surface. There is a clear need for an integrated approach towards the evolution of magnetic fields from the progenitor phase through the supernova and into the compact remnant phase in order to fully grasp the implications of the current simulations.

Evidently, further follow-up studies are also needed on the final evolutionary phases of supernova progenitors.
Longer simulations and resolution studies will be required to better address issues like the saturation field strength, the saturation mechanism, and the impact of magnetic fields on turbulent entrainment.
Full models that include the core and self-consistently follow the evolution of the star to collapse will be required to generate
accurate 3D initial conditions for supernova simulations.
The critical issue of non-ideal effects and the behaviour of turbulent magnetoconvection for magnetic Prandtl numbers slightly smaller than one at very high Reynolds numbers deserves particular consideration. Some findings of our ``optimistic'' approach based on the ideal MHD approximation should, however, prove robust, such as the modest effect of magnetic fields on the convective bulk flow and hence the reliability of purely hydrodynamic models \citep{couch_15,mueller_16c,Yadav2020,mueller_20,Fields2020a} and even 1D mixing-length theory \citep{Collins2018} to  predict pre-collapse perturbations in supernova progenitors.
Future 3D simulations will also have to address rotation and its interplay with convection and magnetic fields.

\section*{Acknowledgements}
We thank A.~Heger for fruitful conversations.
BM was supported by ARC Future Fellowship FT160100035.
We acknowledge computer time allocations
from NCMAS (project fh6) and ASTAC. This research was undertaken with the assistance of resources and services from the National Computational Infrastructure (NCI), which is supported by the
Australian Government.  It was supported by resources provided by the Pawsey Supercomputing Centre with funding from the Australian Government and the Government of Western Australia.

\section*{Data Availability}
The data underlying this article will be shared on reasonable request to the  authors, subject to considerations of intellectual property law.

redpajama_set_name: RedPajamaArXiv


text:
Science teacher who tackled school shooter identified by students, parents
Posted 4:12 pm, May 25, 2018, by Tribune Media Wire
NOBLESVILLE, Ind. -- The teacher who tackled a shooter at Noblesville West Middle School and swatted the gun away was identified by numerous parents and students as seventh-grade science teacher and middle school football coach Jason Seaman, according to WXIN.
Photo of science teacher Jason Seaman from his LinkedIn page
A seventh-grader who was in the classroom where the shooting took place told WXIN the students were in class when the suspect asked to be excused. He later returned with two handguns and opened fire. Students said a 13-year-old girl was hit.
That's when Seaman bravely tackled the shooter and swatted the gun away from him, possibly saving others from getting injured.
Police say the teen victim was transported to Riley Hospital for Children, and Seaman was transported to IU Health Methodist Hospital. Officials say they will not yet release the conditions of the victims.
A student who wished to not be identified told WXIN he was in the classroom and sitting near a student who was shot.
"He took about four to five, maybe six shots, one of them hitting a girl that was about 10 feet from me," the student told WXIN. "Mr. Seaman started running at him, he's a teacher, a science teacher -- he tackled him to the ground, we were all hiding in the back of a classroom behind some desks, then he was yelling to call 911 to get out of the building as fast as we could, so we ran down the stairs and just ran down here, we ran down the sidewalk into Prairie Crossing."
The student described his teacher's actions as heroic.
"He's a hero," the student said. "If he didn't do anything he probably would have continued shooting and a lot more of us would have been injured and possibly killed, so it was just something that not most people would have done but he was really brave to do it."
The student said this is the type of person the teacher and football coach is.
"I'd say it's something I'd see from him, he would do this type of thing, he's a really good guy," he said.
Seaman played football for Southern Illinois University.
Head SIU football coach Nick Hill played a season with Seaman.
"He was a great teammate, one of the team's hardest workers. You could always trust him to do the right thing," Hill said.
Topics: hero, school shooting, teacher
1 dead, 8 students injured in Colorado school shooting; 2 suspects in custody
Teen killed in Colorado shooting charged gunman, is credited with saving classmates' lives
This sixth-grader wanted to 'go down fighting' so he grabbed a bat during a school shooting
WARRANT: UNC Charlotte accused shooter used phone to record actions
Teacher adopts sick student to help him get kidney transplant
New York teacher fired after making black students act as slaves in mock auctions
Student who helped stop Colorado school shooter says he's no hero
Former Smith High School science teacher drowns in rip current
2 juveniles, teacher charged after gun on campus at Paisley Magnet School in Winston-Salem
Burlington teacher accused of indecent liberties with a student
'Hero' student knocked UNC Charlotte shooter off his feet and saved lives, police say
School apologizes after boy with autism given 'most annoying' award
3 victims of Burlington triple homicide identified

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Google has been busy rolling out a number of new additions to it Chrome browser this week, together with its new version created for Android devices. Now Google has rolled out a new update for its desktop Chrome browser client, bringing with it extra speed and added security.
The update has been released into the latest stable Chrome version and now includes a pre-rendering features that will start to load pages as you start typing in the Chrome omnibox.
On the security side Google has now added stricter protection for users against malicious downloads. As well as checking a list of known bad files, Chrome also does checks on executable files (like ".exe" and ".msi" files).
If the executable doesn't match a whitelist, Chrome checks with Google for more information, such as whether the website you're accessing hosts a high number of malicious downloads, etc and then notifies you of the problem.
Google also says that it will be rolling out a new image editor, that will enable Chrome browser users to quickly view, edit and share photos on the web. As more information becomes available for the new editing feature we will keep you updated.


Just a 1-minute walk from Kitanomine Gondola Station, Chalet Fuyuri offers 1 and 2 bedroom apartment-style accommodations with a living room and kitchen. Free wired Wi-Fi is available and guests can sit on the spacious sofa and watch DVDs on the flat-screen TV. A free shuttle is available from JR Furano Train Station, which is a 10-minute drive away. Each apartment has it's own kitchen, bathroom and laundry.


text:
Q: Globally Fix Font Size for System Fonts in iOS 14+ I want to use system fonts in my SwiftUI text, but these fonts automatically scale with the user's accessibility settings.
Text("abc").font(.system(size: 12))

Non-system fonts have this fixedSize initializer which allows it to not adjust to user settings, but there's no equivalent version for system fonts.
Text("abc").font(.custom("Arial", fixedSize: 12))

Another answer on here proposes using the environment to fix the font size, but unfortunately this doesn't apply to sheets. (This might be a bug similar to the one with environment objects not being passed into sheets). So I have to add this line for every view that is presented modally, plus the root view of my app.
var body: some View {
    VStack {
        ...
    }
    .environment(\.sizeCategory, .large)
}

Is there a more elegant way to globally fix the font sizes for my app, rather than setting the environment key for every possible view that could be presented modally?

redpajama_set_name: RedPajamaStackExchange


text:
University-Wide Committee on Sexual Misconduct
Information for Parties
Home > Policies & Procedures > Policy on Teacher-Student Consensual Relations
Policy on Teacher-Student Consensual Relations
The integrity of the teacher-student relationship is the foundation of the University's educational mission. This relationship vests considerable trust in the teacher, who, in turn, bears authority and accountability as a mentor, educator, and evaluator. The unequal institutional power inherent in this relationship heightens the vulnerability of the student and the potential for coercion. The pedagogical relationship between teacher and student must be protected from influences or activities that can interfere with learning and personal development.
Whenever a teacher is or in the future might reasonably become responsible for teaching, advising, or directly supervising a student, a sexual relationship between them is inappropriate and must be avoided. In addition to creating the potential for coercion, any such relationship jeopardizes the integrity of the educational process by creating a conflict of interest and may impair the learning environment for other students. Finally, such situations may expose the University and the teacher to liability for violation of laws against sexual harassment and sex discrimination.
Therefore, teachers (see below) must avoid sexual relationships with students over whom they have or might reasonably expect to have direct pedagogical or supervisory responsibilities, regardless of whether the relationship is consensual. Conversely, a teacher must not directly supervise any student with whom he or she has a sexual relationship. Undergraduate students are particularly vulnerable to the unequal institutional power inherent in the teacher-student relationship and the potential for coercion, because of their age and relative lack of maturity. Therefore, no teacher shall have a sexual or amorous relationship with any undergraduate student, regardless of whether the teacher currently exercises or expects to have any pedagogical or supervisory responsibilities over that student.
Teachers or students with questions about this policy are advised to consult with the University's Title IX Coordinator, the Title IX Coordinator of his or her school, the department chair, the appropriate dean, the Provost, or one of his or her designees. A student or other member of the community may lodge a formal or informal complaint regarding an alleged violation of this policy with the University's Title IX Coordinator, with the Title IX Coordinator of his or her school, or with the University-wide Committee on Sexual Misconduct.
Violations of the above policies by a teacher will normally lead to disciplinary action. For purposes of this policy, "direct supervision" includes the following activities (on or off campus): course teaching, examining, grading, advising for a formal project such as a thesis or research, supervising required research or other academic activities, serving in such a capacity as Director of Undergraduate or Graduate Studies, and recommending in an institutional capacity for admissions, employment, fellowships or awards. "Teachers" includes, but is not limited to, all ladder and non-ladder faculty of the University.
It also includes graduate and professional students and postdoctoral fellows and associates only when they are serving as part-time acting instructors, teaching fellows or in similar institutional roles, with respect to the students they are currently teaching or supervising. "Students" refers to those enrolled in any and all educational and training programs of the University. Additionally, this policy applies to members of the Yale community who are not teachers as defined above, but have authority over or mentoring relationships with students, including athletic coaches, supervisors of student employees, advisors and directors of student organizations, Residential College Fellows, as well as others who advise, mentor, or evaluate students.
Yale Policy on Relationships Between Staff Members
Staff are expected to avoid romantic or sexual relationships with employees and trainees for whom they have or might reasonably expect to have supervisory or reporting responsibilities.
Under no circumstances can a supervisor directly supervise or evaluate any employee or trainee with whom they have or have had a romantic or sexual relationship. If such a relationship exists or develops, the supervisor and employee must promptly disclose it to the Department Head or the Human Resources Generalist. Arrangements, which may include reassignment or relocation, will be made to address any issue of conflict of interest. Any decision affecting any aspect of employment (for example, transfer, promotion, salary, termination) must be made by disinterested and qualified supervisory personnel.
Violations of this policy will normally lead to disciplinary action, up to and including termination.
Individuals with questions about this policy or staff concerned about a romantic or sexual relationship in violation of this policy are encouraged to speak with their supervisor, Human Resources Generalist, or any Title IX Coordinator. See Staff Workplace Policies.
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Thanks so mu ch for your prayers last Saturday as Grandview Church made her public debut at Mead's Annual Community Day festivities while 2,000 people milled around Mead's Downtown Park!
We had purchased our tent, table, banner, and promotional materials, including five gift certificates for our Prize Drawing. We had rented the Longs Peak Baptist Association "Celebration Station Trailer" which included a Snow Cone machine and popcorn popper, and all the necessary supplies to go with them.
We started out with 60 pounds of ice, but by the time the day was almost over, we had made and given out 600 Free Snow Cones (using 180 pounds of ice total)! We also estimate we made and gave away 300 Free bags of popcorn! While Lisa, my sister Nancy and her husband Jerry made and gave away the free eats, I manned the front table and encouraged people to fill our cards and enter the Prize Drawings.
While they filled out the card I told them a little about Grandview Church and answered their questions. By the end of the day we had 91 cards in our "fish bowl!" Besides basic contact info (email address or cell number), the card had three crucial questions: 1) "May we contact you when we are ready to begin our meetings?" 2) "Would you be interested in serving in our church?" Praise the Lord, 51 (over half) indicated we could contact them when we start meeting, and 11 indicated that they would be interested in serving in our church! 3) "May we pray for you? If so, do you have any special requests you would like to share with us?" The vast majority of the cards indicated that they would like us to pray for them, and many of them wrote out special prayer requests for us.
These contacts, along with the ones we have gathered along the way, will provide us a database that our church communications can easily travel. We also offered free copies of "The Story of Jesus," a small paperback that takes scripture passages out of all four gospel accounts to provide a concise, chronological su mmary of Christ's birth, life and ministry, death and resurrection! Thirteen people took "The Story of Jesus" home with them, and each of them had one of our business cards stuck inside so they could contact us later!
Pray for each one of the lives that we touched! Pray some will come to know Christ personally. Pray some will step up and become church planting partners here in Mead with us. Pray that Christ will be glorified and that His Kingdom will grow and expand in Mead and beyond!
←Sharing Our Vision of Supernatural Multiplication!


text:
För boken Folkets hus av Jan Myrdal, se Folkets hus (bok).

Folkets hus är inte ett namnskyddat begrepp, men används i huvudsak för lokaler som erbjuder allmänna samlingslokaler med mötesplatser för kulturevenemang och aktiviteter i nära anslutning till arbetarrörelsens organisationer. Vanligast är att varje enskilt hus drivs av en fristående och självständig förening.

Historik
Upprinnelsen till att Folkets hus bildades över hela landet var behoven av gemensamma möteslokaler. Både för regelrätta möten och för studieverksamhet och kulturella evenemang.

Idén med Folkets hus spreds från söder till norr. Sveriges första Folkets hus öppnades i Kristianstad, men det första Folkets hus som byggdes för ändamålet låg på Skolgatan 10 och Torpgatan 21 i Malmö och öppnade 1893. Många av de tidiga Folkets hus låg i industrisamhällen, där det fanns ett stort behov av möteslokaler för bl.a. facklig verksamhet. Ett av de tidigaste Folkets hus kom till var Tors lokal på Alnön i Sundsvalls sågverksdistrikt. Över 20 folketshusföreningar bildades under sent 1800-tal. Tidiga folkets hus förlades ofta utanför centrum. Folkets hus i Stockholm invigdes 1901 på Barnhusgatan 14 och revs i samband med Norrmalmsregleringen 1955.

Organisation
År 1905 bildades för folkparkerna Folkets Parkers Centralorganisation och 1933 Folkets Husföreningarnas Centralorganisation, 1937 ombildad till Folkets Husföreningarnas riksorganisation. De två organisationerna slogs samman år 2000 till Folkets Hus och Parker.

Verksamhet
Inriktningen på utbudet är i stort detsamma idag som när rörelsen startade. Föreningarna driver ofta vissa verksamheter i egen regi, men upplåter också lokalerna för andra arrangörer. Även om verksamheten drivs i föreningsform av självständiga juridiska personer betraktas lokalerna som offentliga lokaler med de krav på säkerhet vid brand och olyckor som gäller då.

Enskilda Folkets Hus i Sverige i urval

Folkets hus, Borlänge
Bromölla Folkets Hus
Folkets hus, Fräntorp
Folkets hus, Göteborg
Folkets hus, Helsingborg
Härnäsets Folkets hus
Folkets hus, Jönköping
Folkets hus, Kallhäll
Folkets hus, Lindesberg
Folkets hus, Mölndal
Folkets hus, Umeå
Folkets hus i Stockholm
Söråkers Folkets Hus
Folkets hus, Örebro
Folkets hus, Iggesund

Se även
Folkets Hus och Parker
Sveriges Folkbiografer
 Bygdegård
Kulturhus
Medborgarhus

Vidare läsning

Larmet från ett Folkets hus: Ligger sömnlös. SvD 9 augusti 2020.

Referenser

Noter

Externa länkar
Folkets hus och parker i Sverige
Bilder på Folkets hus från norr till söder. SvD 9 augusti 2020.

Byggnadstyper

Svensk arbetarrörelse

redpajama_set_name: RedPajamaWikipedia


Academic advising is vital to successful completion of a degree program. Students are assigned academic advisers once admitted to a degree program. In addition to assisting with academic issues, advisers also can provide referrals to appropriate resources for social and personal issues.
Academic honesty is taken very seriously at the University. It is each student's responsibility to learn how academic dishonesty is defined. The academic integrity policy can generally be found in the course syllabus. Questions about what is considered academic dishonesty, such as plagiarism, should be directed to the course instructor.
If there is a need to see all courses previously taken at the University or those that may have been transferred from other colleges attended, you can request a copy of your academic profile be sent to your university email.
To help students participate fully in the learning experience, the University of Missouri Disability Center serves as a valuable resource for providing services and accommodations to students that need specific assistance. Students wishing to make use of academic accommodations must be registered with the Disability Center. Registration is required for each semester that academic accommodations are to be used.
EdReady is a personalized college math readiness application designed to help students test their college readiness, see study options and gain a personalized learning path to fill in knowledge gaps. EdReady is a free resource and is maintained by the NROC Project, a community-guided, nonprofit project funded by the William and Flora Hewlett Foundation and the Bill and Melinda Gates Foundation.
Students taking writing intensive courses or online courses that require writing assignments and who need help with their writing skills can check out the Online Writery. Tutoring sessions also are available for students that are able to travel to campus on occasion.
MU has contracted with NetTutor to provide online tutoring to MU students free of charge. The tutors are trained to not just provide answers but help you understand how to work through problems. They use the Socratic method so they will ask you a lot of questions to help lead you through the process. You may work with a live tutor, submit a question to the Q&A center, or review archives of previous tutoring sessions.
If you access NetTutor through a course in Canvas or Mizzou Online, you will not need to create an account.
After you click on the link for NetTutor and choose a content area, you will see a section called Group Notes that has a link to Mizzou's Online Writery and a couple of introductory videos.
You should watch the videos "Brief Overview of NetTutor" and "How to Submit a Question" at the bottom of the NetTutor page to see how the service works.
Check out the resources offered through the MU Career Center. Academic advisers and faculty advisers also are good resources for finding out about career opportunities. Additionally, check with your academic home; some schools and colleges have career fairs or career resources for their academic majors.
"Time Management" is key to success in online courses. Another key is having adequate computer and word-processing skills. You are encouraged to explore ways of ensuring your learning experience is valuable, rewarding and successful.
Explore the broad spectrum of undergraduate, graduate and certificate programs that are available.


text:
La terza stagione della serie televisiva The Intern, composta da 8 episodi, è stata trasmessa in Francia dal 27 febbraio al 20 marzo 2018 sul canale France 3.

In Italia, la stagione è andata in onda dal 14 giugno al 5 luglio 2018 sul canale a pagamento Fox Crime.

Note


League City's Premiere Carpet Cleaning Service!
You have found League City's premier carpet cleaning company. We strive to ensure you receive the best in quality and service at a mid-range price. We know there is more to providing professional work than just getting good cleaning results. Building good relationships with our customers throughout the experience is just as important. We pay attention to the small things that create a good service experience. Our staff is knowledgeable and helpful, the cleaning specialist is punctual, makes sure the job is done correctly, and respects your home or office.
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I read an item in the Chatham Daily News December 18th issue that caused me some concern.
It seems that we have another crow problem, and the contract with BCI has ended for the year. The News reported that John Cryderman has written to Wayne Pollock, municipal director of public works, recommending that the municipality take charge of crow control.
Now perhaps Cryderman ought to be commended for bringing community concerns and suggestions forward. However, a deeper examination within a broader context gives this recommendation the appearance of circumventing due process.
The first question I ponder is how this letter became public domain and worthy of front page news. The article in question implies that John Cryderman is some sage source of municipal advice. While his brand of negativity has indeed often cluttered the opinion columns, I'm sure many citizens have similarly interesting correspondence concerning the municipality that doesn't routinely make the first page, nor even the editorial section. I've certainly attempted to present my concerns and suggestions from time to time, but those were handled quite differently by elected officials and the media.
Even more disconcerting is the fact that the article marks at least the second time in a year that the Chatham Daily News has reported on Cryderman's recommendations to municipal officials. Last I checked, John Cryderman was not elected to represent us (despite persistent rumours that he has been de facto mayor since 2006), nor is he employed in any capacity by the municipality.
What business does a private citizen have of short-circuiting the due process of municipal governance whereby recommendations normally go before elected officials, who then debate the matter during a public council meeting and then direct administration to implement their decision? It looks like unelected persons are attempting to govern through the media.
It is not the role of a private citizen, nor even any individual council member to substitute their own "recommendations" for the obligation of our elected council members to exercise their collective will based on the best interests of the municipality - councillors who must remain responsive to the entire community. Unfortunately, a few of them, mayor Hope in particular, would rather have somebody else do the thinking for them.
This particular private citizen has a record of issuing directions and instructions directly to administration and council members under circumstances that may not have been so benevolent. Perhaps the Chatham media would look into some of the correspondence that didn't make the news, in which he attempts to rewrite administration's reports to council, or threatens council members and municipal staff with litigation and criminal charges if they don't implement his wishes.
If that's not enough, then why not investigate how this individual has used legal threats and actual million-dollar lawsuits against innocent citizens to stifle and chill any opinions critical of Mayor Hope (such criticism being most curiously absent during Hope's flaccid and nondescript term as a direct result). And I think the public would be concerned to learn of allegations that confidential correspondence to elected officials has been divulged to this individual which was then used in pursuit of a rather scurrilous agenda, in violation of Council's Code of Ethics.
I also sent a letter to the municipality recently. However my letter wasn't published by the media as front page news. I requested some MFIPPA documents from Mayor Hope, head of municipal freedom of information requests, with respect to a closed session of council that was allegedly conducted without the authority of the Municipal Act. As a result, I was informed in writing by the municipal solicitor that he would be my "sole contact" with the municipality. I am not allowed to contact my elected officials directly, and all my municipal correspondence must be addressed through his office, presumably for filtration.
Mayor Hope refused to provide the requested reply to my letter, thereby abdicating his obligations of office under the Municipal Act and as municipal head of the MFIPPA. Consequently, I did not get the information to which I was legally entitled. There seems to be a double standard where only certain people are permitted access (and responses) to those elected to represent everyone equally.
I'm curious how such a situation can exist. It's disconcerting that one certain private citizen has direct access to city hall, and uses it consistently to obtain information that may even circumvent the MFIPPA process, and to instruct municipal staff and elected officials to implement personal recommendations, while I am banned from even contacting my elected representatives and exercising my democratic rights and obligations as a citizen. I would think this to be more newsworthy than a friend of the Mayor's opinion about crows.
The optics of this situation are very poor indeed, and would certainly invite public concerns if they ever found out. Our municipal government has been anything but open and transparent since Randy Hope became mayor, and too much is being done in secret behind closed doors (and perhaps over the mayor's personal kitchen table).
Private citizens are certainly entitled to voice opinions, but having those opinions heard is not an exclusive right belonging only to a small vocal group. The democratic system (and media oversight thereof) only works if every citizen has equal unbiased access - without the fear of reprisals or being sued if an opinion doesn't happen to meet with the mayor's approval. It's time to put an end to this rampant nepotism and grant every citizen equal access to our government and media.
There is only one year left before the next mayoral campaign starts. My candidacy, if offered, would provide an antidote to the secrecy and stagnation championed by the current mayor who is more concerned about photo opportunities, favouritism, and stifling criticism than addressing the economic future of our community. Let's hope that my platform of positive ideas won't also have to serve to inform the public about any dirty little secrets that have never been given proper scrutiny by the media.


Lakefront Marina on Lake Erie offers a friendly, family oriented atmosphere with all the amenities of a yacht club. At Lakefront Marina you will find a heated in-ground swimming pool, pavilion with grills, community room, modern restroom/shower facilities, updated laundry room, security gate, and blacktop throughout the entire marina. The marina is located on historic Lake Erie in Port Clinton, Ohio providing a one of a kind experience for our boaters. Put-n-Bay and Kelleys islands are just minutes away, and fishermen love to come here for the spring/fall Walleye along with the perch fishing during the summer months. Lakefront Marina is located one mile west of the Jet Express with a variety of restaurants and pubs within a couple miles from the marina. No matter what your boating interests are, we are here to make your experience as enjoyable and memorable as possible!
We offer wet slips & in/out rack service.
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text:
Mediacheck
Postmedia Expects at Least $8 Million in Taxpayer Subsidies
Focus is still on cutting costs, says CEO. Big winners seem to be US hedge funds.
Paul Willcocks 11 Jul 2019TheTyee.ca
Paul Willcocks is a journalist and former publisher of newspapers, and now an editor with The Tyee.
Government subsidies for media could be a good thing. But in Postmedia's case, it's not clear the funds will help journalists. Photo via Shutterstock.
It's not surprising that the first real information about the federal government's subsidies for news media would come from Postmedia. Traditional media organizations have been lobbying for a bailout.
The floundering corporation released its quarterly results Wednesday. They were bleak, as they have been every quarter since 2010 when Postmedia became Canada's major newspaper owner.
But the corporation shared good news, at least from its perspective. Postmedia expects to get $8 million to $10 million this year from taxpayers under the federal government's subsidy program to support "a strong and independent news media."
Based on a Bloomberg News report, that is about 20 per cent of total program funding in year one.
And it's an interestingly precise forecast, since no details about the subsidies have been released and the panel to establish eligibility was created less than two months ago.
Once I would have scorned the idea that news media companies should accept government subsidies. Readers would never be able to trust our impartiality if we counted on them.
These are desperate times. Maybe we bend, and look for smart ways to support reporting and commentary essential for a functioning democracy, including government supports.
But handing money to Postmedia doesn't seem smart.
Not because journalists employed by the corporation don't do important work. In Vancouver and across Canada, Postmedia journalists report on issues that matter, and would otherwise be ignored. Their ranks are diminished and their owners have undermined their credibility. But as a society we are better off with their work.
But the government's money — your money — won't pay for more reporting, or journalists. Postmedia gets the subsidy even if it continues to cut jobs. And that appears to be its plan.
In the corporation's conference call on the quarterly results, Postmedia CEO Andrew MacLeod touted the continued double-digit growth in digital revenues.
But that growth added $3 million in revenues in the most recent quarter. Print advertising fell by $13.8 million, subscription revenue by $3.4 million.
So revenue fell by $14 million. Operating expenses were cut by $11 million. MacLeod said the solution was more cuts. And Postmedia's future looked bleaker.
Subsidizing Postmedia might make sense if the goal was to preserve its 15 daily newspapers while the corporation found a new path forward.
But there is no clear path. Postmedia's primary goal is to generate enough cash each quarter to pay the interest on the loans from its U.S. hedge fund owners.
Will Ottawa's News Fund Be Wasted Keeping Postmedia Afloat?
Postmedia's calls on quarterly results have attracted few questions. The usual participants are analysts tracking stocks, but Postmedia is really privately owned.
But Wednesday, Leon Cooperman called in. He's a 76-year-old billionaire who owns about 14 per cent of Postmedia. Could MacLeod and the management team say when the corporation would return to profitability, he asked?
No, said MacLeod. Postmedia will keep cutting costs, and see what happens.
Which should worry Canadian taxpayers. The $8 million to $10 million a year Postmedia expects to collect should create new jobs for journalists. How do they know the money won't simply be sent as interest payments to U.S. hedge funds that saw an opportunity in a failing media company?
They don't.
Read more: Media


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Westown Treasure
Historic Second Ward Savings Bank is Home to Milwaukee County Historical Society
At the corner of State Street and Old World Third Street, one of Milwaukee's finest examples of lovingly restored and repurposed vintage architecture reins over the adjacent riverside Pere Marquette Park.
Originally founded at a different downtown location in the 1850s, the Second Ward Savings Bank – now home to the Milwaukee County Historical Society – was patronized by the leading brewers of Milwaukee: Valentine Blatz, Joseph Schlitz, Philip Best, Emil Schandein, and August Uihlein and became known as the "Brewers' Bank."
In 1866, the bank was reorganized and moved to its present location, where a stunning new building in the style of Beaux-Arts Classicism opened later in 1913. The building featured an intricate chandelier, ornamental iron and concrete work, stunning windows, marble staircases, and ornate brass vault doors. Tops of grand pillars were adorned with clusters of hops, symbolizing the patronage of the beer barons.
The bank remained in operation until 1965, when the building was donated to the county to be used for the Milwaukee County Historical Society. Extensive restoration of the building's original elements, including opulent decorative plasterwork, was completed in recent years.
Located on Milwaukee's popular RiverWalk and Pere Marquette Park, this historical treasure is used as the Society's headquarters, housing a museum open to the public, an extensive artifact collection, and an archival research library.
In 2008, Hollywood set designers temporarily restored the 1913 bank teller stations to film scenes from the movie Public Enemies starring Johnny Depp. Although the movie portrays John Dillinger (Depp) robbing the bank, the Second Ward Savings Bank never had a single robbery in its time of service.
Milwaukee County Historical Society
(414) 273-8288 [email protected] Learn More
Anatomy of the Zoo
Bay View Printing Co
Deer District
The Care and Keeping of a Tropical Dome
Harley-Davidson Museum
Tripoli Shrine Center
American Family Insurance Amphitheater
Northwestern Mutual Community Park


The focus group will provide an opportunity for you to find out about Unified Communication Platform, UCP, is the core platform, and is application that provides Unified Communication through linkage IP-PBX. UCP brings together various applications and communication tools so you can easily work and serve your customers effectively. Unified Communication systems simplify your business communication and improve productivity by linking voice and other communication aware application under a single intuitive user interface.


Uique bracelet made out of 19 pieces , each on of them different from the other.
The material is silver oxid , but ut was mads in a speacial process of heating that added shades to the natural color: blue, brown, purple and gray.
An artistic , one of a kind piece.


text:
Storys zum Thema Pharma
Keine Story zum Thema Pharma mehr verpassen.
Debiopharm International SA
DEBIOPHARM APPLIES EXTENDED-RELEASE FORMULATION EXPERTISE TO REDUCE TREATMENT FREQUENCY BURDEN FOR ACROMEGALY & GEP-NET PATIENTS
Lausanne, Switzerland (ots) - - Acromegaly and gastroenteropancreatic neuroendocrine tumors (GEP-NETs) are rare diseases that require life-long chronic treatment. Monthly somatostatin analog (SSA) injections are the standard of care as first-line medical treatment. - Debiopharm is developing Debio 4126, a novel ...
Acousia Therapeutics GmbH
Hearing loss company Acousia Therapeutics to present data for lead candidates ACOU085 & ACOU082 at ARO 2023 MidWinter Meeting February 11–15
Tübingen, Germany (ots) - Acousia Therapeutics GmbH, and its partners from the Translational Hearing Research Group at the Tübingen Hearing Research Center (Department of Otolaryngology, Head and Neck Surgery, University of Tübingen), will present data on its lead candidates — clinical stage ACOU085 and late ...
Debiopharm leads $6M round for YonaLink to Scale Global Growth and Fuel Expansion of Platform Designed to Stream Clinical Trial Data
Boston, USA and Lausanne, Switzerland (ots) - - SaaS Platform Provides Missing Link in Clinical Trial Data Collection, Securely Automating Real-Time Transfer of Up-to-Date Patient Data Directly from EHRs to EDC Systems - Technology Brings New Levels of Speed, Quality and Efficiency to Clinical Trial Data Collection ...
DEBIOPHARM REINFORCES THE BOND BETWEEN SWISS AND JAPANESE CANCER RESEARCH WITH THE 2022 JCA MAUVERNAY AWARD CEREMONY
Lausanne, Switzerland (ots) - Debiopharm awards the winning scientists for the JCA (Japanese Cancer Association) Award for innovative, disruptive, and translational oncology research Debiopharm (www.debiopharm.com), a Swiss-based global biopharmaceutical company, today announced the two winners of JCA Mauvernay ...
BIG IMPACT, SMALL PACKAGE: DEBIOPHARM LAUNCHES A WAZOKU OPEN-INNOVATION CHALLENGE FOR SMALL ANTIBODY DRUG CONJUGATE TECHNOLOGY
Lausanne, Switzerland (ots) - · Currently approved Antibody-Drug Conjugates (ADCs) are large molecules (150 kDa) composed of an antibody, a cytotoxic payload, and a linker connecting the two precedent elements · Debiopharm has launched an ADC Innovation Challenge to a pool of international "problem Solvers" ...
ONE DRUG FOR ONE BUG: DEBIOPHARM TO DISCUSS THE POTENTIAL OF PATHOGEN-SPECIFIC ANTIBIOTICS AT THE 2022 WORLD AMR CONGRESS
Lausanne, Switzerland (ots) - - International health authorities, such as the WHO and the CDC are warning of the emerging danger of bacterial infections resistant to current antibiotics - The 2022 World Anti-Microbial Resistance (AMR) Congress in the greater Washington D.C. area is serving as a forum to openly ...
Grünenthal Group
Grünenthal, Uniklinik RWTH Aachen and RTWH Aachen University collaborate to advance pain research
Aachen (ots) - Grünenthal, Uniklinik RWTH Aachen and RWTH Aachen University announced a collaboration to advance the development of next-generation pain medicines. The collaboration involves the institutes of Dr Angelika Lampert, Professor of Physiology at the Uniklinik RWTH Aachen and Dr Marc Spehr, ...
Acousia Therapeutics to present its first-in-class hearing loss treatment program with ACOU085 at the 2nd Inner Ear Therapeutics Summit in Boston
Tübingen (ots) - Acousia Therapeutics GmbH will be presenting data on the company's clinical stage, first-in-class lead candidate ACOU085 at the Hanson Wade 2nd Inner Ear Therapeutics Summit to be held in person in Boston (MA) from June 20–23, 2022. ACOU085 is a proprietary, first-in-class, small-molecule ...
Series A financing round lays foundation for international growth of digital cancer therapeutics Mika
Berlin/Lausanne/Barcelona/Munich (ots) - New investors with a successful track record in digital oncology support German Digital Therapeutics (DTx) company Fosanis to broaden patient access of Mika - an app-based DTx platform empowering people affected by cancer. Berlin-based digital health company Fosanis, the ...
Hearing loss company Acousia Therapeutics: first patient with age-related hearing loss treated with ACOU085
Tübingen (ots) - ACOU085, the lead candidate from Acousia Therapeutics, has been administered to the first patient with age-related hearing loss (presbycusis) in a Phase 1b clinical study in Germany. The pre-screening of patients matching the comprehensive in/exclusion criteria for the ongoing trial is almost ...
DEBIOPHARM ANNOUNCES ONCOLOGY RESEARCH ADVANCEMENTS AT AACR 2022 FOR NOVEL CANCER COMPOUNDS AND DRUG DELIVERY TECHNOLOGIES
VIVOSENSE ANNOUNCES CLOSING OF $25M SERIES A FINANCING
Newport Beach (ots) - Proceeds to accelerate the collection and use of wearable sensor data in clinical trials along with the development of novel digital biomarkers Funding round co-led by the Perceptive Xontogeny Venture (PXV) Fund and Switzerland-based Debiopharm Innovation Fund VivoSense, Inc., ("VivoSense") an agile end-to-end scientific solutions company developing novel digital endpoints from wearable sensor ...
Grünenthal and NovaQuest enter agreement to advance the resiniferatoxin global Phase III program in osteoarthritis
Aachen, Germany, and Raleigh, North Carolina (ots) - Grünenthal and NovaQuest announced today that they have entered into an agreement to advance the global clinical Phase III programme of Grünenthal's asset resiniferatoxin (RTX). The investigational medicine is being developed with the aim of providing patients ...
DEBIOPHARM AND ASPEN PARTNER TO LAUNCH PROSTATE CANCER DRUG TRELSTAR® IN SOUTH AFRICA
Lausanne, Switzerland and Durban, South Africa (ots) - Debiopharm (www.debiopharm.com), a Swiss biopharmaceutical company and Aspen, a South African headquartered multinational pharmaceutical company announced today their partnership to launch Trelstar® (Triptorelin) in South Africa for the treatment of locally advanced and metastatic hormone dependent prostate ...
DEBIOPHARM IINVESTS IN VERISIM LIFE'S $15M SERIES A ROUND TO ADVANCE AI-ENABLED DRUG RESEARCH
Lausanne, Switzerland - San Francisco (ots) - Funding to support BIOiSIMTM computational platform to reduce the need for animal testing by selecting compounds showing promise to cure a disease prior to research in humans Debiopharm (www.debiopharm.com), a Swiss biopharmaceutical company, announced today their co-investment in California-based start-up VeriSIM Life's ...
VeriSIM Life Secures $15 Million Series A Funding
San Francisco, CA (ots) - Financing led by Morpheus Ventures supports further revenue growth for the company's next-generation AI platform, redefining the preclinical translational drug development landscape by accurately predicting and accelerating clinical outcomes VeriSIM Life (VeriSIM) www.verisimlife.com, the leading artificial intelligence (AI)-enabled, unique R&D decisions de-risker for breakthrough drug ...
FDI World Dental Federation
FDI World Dental Federation: Prescribing of dental antibiotics up 22% in England during first year of COVID-19 / Prescriptions of all other antibiotics fell during the same period
Swiss-based Debiopharm co-invests in the future of cell therapies on a chip through the latest $25 million Series A round for Mekonos
Lausanne, Switzerland - San Francisco (ots) - Funding to accelerate the development of Mekonos' System on a Chip (SoC), expand commercial partnerships Debiopharm (www.debiopharm.com), a Swiss biopharmaceutical company, announced today having invested $4M inMekonos, a biotech company building the future of cell ...
Roche and the Zur Rose Group announce collaboration to offer innovative health journeys for people living with diabetes
Basel (ots) - - Roche, a world leader in integrated Personalised Diabetes Management, and the Zur Rose Group, provider of a European digital healthcare ecosystem, announce their collaboration to improve everyday therapy management and better address the needs of 60 million people living with diabetes in Europe [1] - ...
CARB-X FUNDS THE 3RD ROUND OF DEBIOPHARM'S TARGETED ANTIBIOTIC PROGRAM TO COMBAT RESISTANT N. GONORRHOEAE INFECTIONS
Lausanne, Switzerland / Boston, USA (ots) - Debiopharm (www.debiopharm.com), a Swiss-based global biopharmaceutical company announced today having been awarded the third phase funding to advance the development of its antibiotic program, Debio 1453, by the Combating Antibiotic-Resistant Bacteria Biopharmaceutical ...
DEBIOPHARM & DEXA MEDICA LAUNCH TRIPTORELIN COLLABORATION TO BRING NEW HOPE TO WOMEN WITH ENDOMETRIOSIS
Lausanne, Switzerland – Tangerang, Indonesia (ots) - Debiopharm (www.debiopharm.com), a Swiss-based, global biopharmaceutical company, and Dexa Medica, a leading Indonesian pharmaceutical company, today announced the Indonesian launch of triptorelin for the treatment of women with gynecological disorders, ...
DEBIOPHARM AND UBIX THERAPEUTICS LAUNCH RESEARCH TO DEVELOP A NEW ANTI-CANCER MODALITY - ANTIBODY DEGRADUCER® CONJUGATES
Lausanne, Switzerland, Seoul, Republic of Korea (ots) - Debiopharm (www.debiopharm.com), a Swiss-based global biopharmaceutical company and Ubix Therapeutics (en.ubixtrx.com), a South Korea-based biotech company today announced their co-research agreement combining two novel proprietary technologies to specifically ...
DEBIOPHARM'S CD37 ANTIBODY DRUG CONJUGATE SHOWS PROMISING PHASE II RESULTS FOR THE TREATMENT OF B-CELL MALIGNANCIES
Lausanne, Switzerland (ots) - - Diffuse large B-cell lymphoma (DLBCL) is the most common aggressive form of Non-Hodgkin's Lymphoma (NHL), representing 30-40% of cases. Nearly half of DLBCL patients are not cured by first-line treatment, leaving a large number of patients at risk of worsening disease1 - Naratuximab ...
DEBIOPHARM COLLABORATES WITH INNOCENTIVE FOR THE LAUNCH OF A GLOBAL CHALLENGE TO DEVELOP A SINGLE-DOSE mRNA COVID-19 VACCINE
Lausanne, Switzerland (ots) - - Currently approved COVID-19 vaccines based on messenger RNA (mRNA) technology require two injections, given several weeks apart, for optimal protection against the virus - Debiopharm has launched a vaccine innovation challenge to a pool of international "problem Solvers" within ...
Grünenthal is Recognized for its Strong Management of Environmental, Social and Governance (ESG) Risks
Aachen, Germany (ots) - - Leading global ESG ratings agency Sustainalytics notes Grünenthal is in the top five percent among its peers in the pharmaceutical subindustry - Grünenthal is categorized as "medium risk", placing it ahead of its key subindustry peers and in the same league as multinational companies ...
Semdor Pharma Group
Semdor Pharma adds Global Pharmaceutical Executive Rolf Hoffmann to its Board of Directors
Cologne (ots) - 30-year pharma veteran Rolf Hoffmann, formerly senior global executive at Amgen and Eli Lilly, joins Semdor Pharma as investor and commercial expert. Semdor Pharma Group announced today that it has added Rolf Hoffmann, a seasoned global pharma executive and advisor, to its Board of Directors, as well as an investor in the company. Mr. Hoffmann ...
DG-Nika AG
First pocket inhaler for Covid-19 and other viral mutations
DEBIOPHARM AND GENOME & COMPANY JOIN FORCES TO CREATE NEW HIGHLY SPECIFIC THERAPIES FOR CANCER PATIENTS
Lausanne, Switzerland and Seongnam-si Gyeonggi-do, Republic of Korea (ots) - Korean and Swiss based companies leverage their oncology expertise to initiate a research collaboration to formulate novel antibody-drug conjugate (ADC) candidates Genome & Company (314130, CEO: Jisoo Pae, Hansoo Park), a global leading ...
NLS Pharmaceutics Ltd
NLS Pharmaceutics Ltd. Announces Pricing of $20.0 Million Initial Public Offering
Stans, Switzerland (ots) - NLS Pharmaceutics Ltd. (Nasdaq: NLSP, NLSPW) ("NLS" or the "Company"), a Swiss clinical-stage pharmaceutical company focused on the discovery and development of innovative therapies for patients with rare and complex central nervous system disorders, announces the pricing of its initial public offering of 4,819,277 units at a price of ...
ForaCare Suisse AG releases Rapid COVID-19 Antigen Test / Test Results in 15 Minutes, No Laboratory Processing Required, Highly Accurate & Reliable Results
ST. GALLEN, Switzerland (ots) - ForaCare Suisse AG announced the release of its antigen test, FORA COVID-19 Antigen Rapid Test, that provides fast, accurate and easy-to-interpret test results. The test can be administered by trained professionals and doesn't rely on laboratory-processing. Approved by Swissmedic, ...