text:
Perspective in Worldbuilding
March 25, 2019 March 24, 2019 ~ BYOM
Every character has their own unique psychology — that's why it's so fun to dive into their heads! But no one's worldview is created in a vacuum: the world around us directly affects our personalities, traits, and current mental state.
So imagine something totally far-fetched: A country teetering on the edge of dictatorship. Small accidents lead to bankruptcy; small children are put in cages. Reality TV has subsumed reality. How might this world affect the way characters see the world?
They might be more anxious. They might be more depressed and miserable, all across the land. Perhaps they're gripped by nostalgia, longing for a time when the world felt less bleak. Welcome to your world's general psychology: the average of all its citizens. These traits infiltrate your book's mood and affect the tone — but are not, necessarily, your characters' traits, too.
Even when, psychologically, something is generally true, there's always a bell curve. Let's look at a few examples. First: Trees make people happy. (It's true!) By extension, every child that grows up in the woods must be a delightful, well-adjusted human. (Or woodsy alien — whatever your world demands.) Right? Except, no: gloomy people live in the woods, too. And some people are born in a forested hut, but spend their lives dreaming of the concrete jungle of the nearest big city. So seeing a thick oak with sap dripping down its bark probably just pisses them off. Yes, generally, trees make people happy — but that's not a universal truth.
Or, think about the winter blues. Short days and dark skies contribute to seasonal affective disorder. In other words? Winter can make people gloomy and moody. Surprise! Yet many people excitedly move to Canada, and four out of the top five happiest countries in the world are Nordic. Clearly, "darkness = sadness" isn't true for everyone.
To create a fully-fleshed-out character, roleplay a game of table tennis between your character and the world. Everyone has their own, unique character traits, which clash with the world you've established. The end result? A character singularly affected by your world.
Your characters start with an initial set of traits — and those traits play off the world around them, creating new traits. Score one to your world. Those new traits flesh out your character and cement their perspective on life: the way they think and behave. And, of course, your character's perspective will continue to be affected by the world around them. Character reacts to world, develops new traits, those traits change how the character reacts to the world, and on and on and on, in an endless ouroboros.
Let's take Harry Potter's Statute of Secrecy as an example. J.K. Rowling plopped her super-secretive magical society right in the middle of the muggle world — and then established a government that demanded its citizens stay silent. Psychologically, secret-keeping tends to be stressful and make people feel less authentic. But thinking you're part of the "in-group" makes you believe you're better than those less lucky. That's a tough intersection of traits!
Once you've established your characters' basic traits, you can pit them against the parameters you've set to learn even more about your book's cast. Two people in the same family might approach the same thing in entirely different ways. Arthur Weasley is a creative, curious dude — so it makes sense he'd be intrigued by the muggle world and desperate to replicate their technology. But his son, Percy, is uptight and a teensy bit power-hungry. That Statute of Secrecy? He thinks it's a blessing.
Consider also how your characters' psychological traits are affected by their interactions with other characters, who are in turn reacting to the same worldbuilding constraints. Imagine poor, uptight, anxious young Percy, growing up with a father who glibly ignores all established magical boundaries. He probably spent a lot of nights tossing and turning, worried his careless father might blow himself up — or end up arrested. No wonder he pushes so far toward the other end of the spectrum, and runs straight into the open arms of Cornelius Fudge. (Still a jerk, though. Sorry, Perce.)
Your characters may not even realize they're reacting to something. We start absorbing stress in the womb, so if your fictional country was undergoing a civil war while your main character was hanging out unborn, they may see psychological effects later in life. Or, if they're rather resilient, they may not — but you bet they'll be dealing with the aftereffects of said civil war in some way or another.
Now, let's imagine a family that's spent the last fifteen years hurtling across space on a tiny ship. Port stops are rare and blessed occasions. Think about how close quarters might affect their day-to-day living: generally, they're probably more willing to share food and personal items, and their concept of "personal space" is likely smaller than if they'd grown up in a castle. Dad scoots by in a tight hallway, and then proceeds to hold an extensive conversation with his face mere inches from your main character's.
Maybe that's normal for them. Or maybe your main character has a fierce independent streak and a strong sense of boundaries, and having their personal bubble stepped on again and again makes them so angry they can hardly speak. But where can they go? They live in a tiny spaceship with four annoying family members. Now that's a head we'd love to step inside.
Your homework:
Think about your main character's defining personality traits. Are they optimistic? Patient? Petty? Selfish? Select one or two essential traits.
Write down all of the main aspects of your worldbuilding. If you're writing a contemporary, maybe you'll write down details about your character's family structure or the restrictive administration of their school. For a fantasy or sci-fi, think about the politics, geography, and history of your world.
Think about the overall worldview of the characters who live in your world. If the government is authoritarian, perhaps they feel powerless. Or maybe harsh geography leads to a pervasive feeling of isolation. Look for real-world examples to help you understand how the world affects people's mood and outlook.
How does your character's unique personality collide with the world? If they're optimistic in a pessimistic world, they may fixate more on hope. Think about how the constraints of the world you've established affect their outlook — and make sure to consider how they interact with other people living in your world, too.
Continue this exercise for each of your character's main traits, and each of your world's main building blocks.
A world feels more realistic when it affects your characters directly. Taking the time to consider how your gorgeous newly-built world affects your characters' psychology creates a rich, immersive tapestry — one your readers won't ever want to leave.
Elisabeth Funk is a fantasy writer who lives in Denver, Colorado, with her husband, two cats, one dog, and large collection of succulents. When she's not writing stories about witches, magic, complicated friendships, and ghosts, you can find her on Twitter @e__funk.
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redpajama_set_name: RedPajamaCommonCrawl


I attended a hackathon called GLAMhacks (Galleries, Libraries, Archives, and Museums) at the University of Pennsylvania with my friend Rita Zevallos. We decided to rescuscitate this corpus of 1M syllabi, which was missing a majority of the cached syllabus content (only having URLs and other metadata). Over the next two days we poached the Starbucks wifi across the street to download as many of the syllabi as we could from the Wayback Machine.
Rita built a rails app on top of the corpus, and we planned to call it… (drumroll)… Sylla-search. It was a stupid name, so we thought harder, and considered calling it "The Open Syllabus Project". The name proved fortuitous, because we discovered that a team out of Columbia University had been working on the exact same project. Their progress was a direct superset of ours. They had already taken Dan Cohen's 1M syllabi, and combined it with a variety of dumps, gifts, and scrapes, with the purpose of providing researchers metadata access to what the global syllabi-scape looked like. I joined them as a volunteer. In the time since then, they've hired a fantastic programmer to create a variety of analytics, visualizations, and other interfaces to the underlying data.


text:
\section{Introduction}

The existence of a self-sustained magnetic field by dynamo action constitutes the most obvious signature of the intense fluid dynamics taking place or having taken place in the liquid iron core of terrestrial planets.
It is also a key ingredient for their habitability.
As such, it has been the subject of numerous studies since the seminal work of \citet{larmor1919possible}, and it remains today an active and challenging research domain for theoretical, experimental and numerical approaches \citep[see e.g.,][]{Busse2015239, cardin2015, christensen2015numerical, roberts20158}.
One of the prevailing questions is the source of fluid motions.
On Earth today, it is generally agreed that the dynamo is driven by turbulent flows sustained by convection coming from the combination of thermal and compositional buoyancy, with a major role played by the solidification of the inner core \citep[][]{roberts20158}.
The energy budget is, however, extremely tight with related  unsolved questions regarding the heat flux at the core-mantle boundary (CMB), the age of the inner core, and the presence of stratified layers at the boundaries \citep[see e.g.,][]{labrosse2015thermal}.
The situation is even more complex before the onset of inner core solidification, where dynamo action can hardly be sustained by thermal convection only and necessitates additional effects \citep[][]{badro2016early,o2016powering}.
Besides Earth, the convective dynamo model has been generically applied to other terrestrial bodies, in the context of an often tacitly assumed equivalence between the presence of planetary magnetism and of core convection.
The standard convective dynamo model is however hardly capable of explaining the past or present magnetic field of numerous bodies like the Moon, Ganymede, Mercury, Mars, large asteroids, etc. \citep[][]{Dwyer2011, Lebars2011, sarson1997magnetoconvection, arkani2008tidal, wei2014simplified}. Even if more evolved or specific convective scenarii might provide plausible explanation,  involving for instance thin shell dynamics \citep[e.g.][]{stanley2005thin}, non-homogeneous or time-dependent boundary conditions  \citep[e.g.][]{stanley2005thin, cao2014dynamo, roberts2017effects}, a stably stratified layer \citep[e.g.][]{tian2015magnetic}, iron snow \citep[e.g.][]{christensen2015iron}, this has led some researchers to look for alternative routes for core flows and dynamo.

Following the seminal ideas of \citet{Malkus1963, Malkus:Science1968,Malkus1989}, a huge reservoir of energy is stored in the rotational motion of terrestrial bodies, including their spinning and orbital motions.
If those bodies were rotating with a perfectly constant rotation vector and with a perfectly rigid shape, the fluid in their core, in the absence of convection, would simply follow the rotation of their mantle like a solid body.
However, this is never the case. First, differential rotation might be present in planetary cores, which is capable of sustaining dynamos \citep[e.g.][]{guervilly2010numerical,cao2012saturn}. Then, the rotation of the planetary bodies is always perturbed by gravitational interactions with neighbors. Indeed, the angular velocity of the rotating bodies changes periodically with time, corresponding to longitudinal libration and length of day variation; the direction of the rotational vector changes periodically with time, corresponding to precession and nutation; and the shape of the terrestrial bodies changes periodically with time, corresponding to tidal distortions.
All these perturbations, generically called harmonic or mechanical forcings, are small in amplitude. For example, on Earth, the relative amplitude of the tidal bulge vs. the core radius as well as the relative amplitude of the precession vs. rotation rates are about $10^{-7}$ only.
This smallness of the perturbation amplitude has led to the misinterpretation that the resulting flows are also small \citep[][]{loper1975torque, rochester1975can}.
But beyond the directly forced laminar base flow, harmonic forcings can sustain instabilities via the resonant excitation of the eigenmodes of the rotating (and possibly stratified) bodies, i.e. the so-called (gravito-) inertial waves \citep[][and references therein]{le2015flows}.
Those instabilities take their energy from the huge rotational energy of the system, the weak forcing being only the conveyor: instabilities then potentially drive intense, highly energetic, bulk filling turbulence in the whole core \citep[][]{Kerswell1996}.

Libration, precession and tidal instabilities have been the subject of numerous studies focusing on their threshold and linear growth \citep[][and references therein]{le2015flows}, and more recently on their non-linear saturation \citep[e.g.,][]{barker2013non,lin2015shear, le2017inertial}, combining theoretical, experimental, and numerical approaches.
The relevance of those alternative sources of core turbulence for terrestrial bodies has also been the subject of several studies \citep[e.g.,][]{Seyed2004,Cebron_2012,Grannan:GJI2016, lemasquerier2017libration}, and has given birth to unconventional scenarii to explain past or existing dynamos: e.g., on Io \citep[][]{Kerswell1998}, on Mars \citep[][]{arkani2008tidal}, on the Moon \citep[][]{Dwyer2011, Lebars2011}, on the early Earth \citep[][]{andrault2016deep}.
However, studies of the dynamo capability of the flows resulting from libration, precession and tides, have been up to now sparse and limited to idealized or simplified configurations: i.e. laminar dynamos from the precession base flow \citep[][]{ernst2013}, laminar dynamos for tidal instability with adhoc bulk forcing in a spherical domain \citep[][]{Cebron:AJL2014,vidal2017magnetic}, laminar dynamos in a spheroidal domain for precession and libration instabilities \citep[][]{Wu:GAFD2009, Wu:GAFD2013} \citep[but see also][]{guermond2013remarks}, and turbulent dynamos in a spherical domain for precession \citep[][]{Tilgner:POF2005, tilgner2007kinematic, kida2011turbulent, Lin:POF2016}.
However, relevance to planetary configurations implies considering fully turbulent flows in non-axisymmetric ellipsoidal geometry, accounting for the static and/or dynamic tidal distortions of the CMB.
This is extremely challenging from a numerical point of view. We present here the first realizations of such kinematic tidal, librational, and precessional turbulent dynamos.

\section{Model formulation}

We present in the following only the main features of our numerical model. All technical details and benchmarks can be found in the Supporting Information \citep[][]{Cattaneo:PRL1995,Chan:PEPI2007,Dudley:PRSA1989,Galloway:Nature1992,Iskakov:JCP2004}.

\subsection{Inner fluid Domain}

We consider the motion of an incompressible, electrically-conducting fluid enclosed in an ellipsoidal cavity surrounded by a large insulating domain.
The density $\rho$, kinematic viscosity $\nu$ and magnetic diffusivity $\eta$ of the fluid are assumed constant.
The outer surface of the ellipsoidal fluid cavity is generally defined using Cartesian coordinates $(x,y,z)$ as $(x/a)^2+(y/b)^2+(z/c)^2=1$ where $a$, $b$ and $c$ are constants.
Following \citet{Grannan:GJI2016}, we non-dimensionalize our problem using the mean equatorial radius $R=\sqrt{(a^2+b^2)/2}$, leading to the following dimensionless definition of the ellipsoidal boundary
\begin{linenomath*}
\begin{equation}
\label{Eq:Ellip_f}
\frac{x^2}{1+\beta} + \frac{y^2}{1-\beta} +\frac{z^2}{c_*^2} = 1 \ ,
\end{equation}
\end{linenomath*}
with the equatorial ellipticity $\beta=(a^2-b^2)/(a^2+b^2)$ and the axial length $c_*=c/R$.

We work in a non-inertial frame of reference rotating with a dimensionless angular velocity $\bm{\Omega}(t)$, normalized by an average rotation rate $\Omega_0$.
The definition of $\bm{\Omega}(t)$ depends on the case of interest and will be detailed in the following sections.
In all cases, we choose to work in the frame in which the mantle shape is fixed in space and time.
Scaling time with ${\Omega^{-1}_0}$, space with $R$, and vector potential field with $R^2\Omega_0\sqrt{\rho \mu_0}$, where $\mu_0$ is the vacuum magnetic permeability, the nondimensionalised MHD equations in the fluid domain, where the dynamo action takes place, are
\begin{eqnarray}
\frac{\partial\mathbf{u}}{\partial t} + (\mathbf{u}\cdot\nabla)\mathbf{u}
 &=& -\nabla \Pi +  E\nabla^2 \mathbf{u}+\mathbf{F}_i \label{Eq:NS} \\
\frac{\partial\mathbf{A}}{\partial t}  &=&  {\mathbf{ u \times(\nabla \times A})} + \frac{E}{Pm}\nabla^2 \mathbf{A} \label{Eq:VP_f} \\
\nabla \cdot \mathbf{u} &=& 0 \label{Eq:incom} \\
\nabla \times \mathbf{A} &=& \mathbf{B}
\end{eqnarray}
where $\mathbf{u}$, $\mathbf{A}$, and $\mathbf{B}$ are the non-dimensional velocity, vector potential and magnetic field, respectively.
$\Pi$ is the modified pressure including the centrifugal acceleration and the gravitational potential.
We have neglected the Lorentz force in equation~(\ref{Eq:NS}), focusing on the kinematic problem.
This general problem involves two dimensionless parameters: the magnetic Prandtl number $Pm=\nu/\eta$ and the Ekman number $E=\nu/(\Omega_0 R^2)$.
We use the vector potential approach \citep{Matsui:EPS2004,Matsui:IJCFD2004,Cebron:GAFD2012} for numerical reasons (see details in the Supporting Information), thus exactly satisfying the divergence-free condition for the magnetic field.
$\mathbf{F}_i$ stands for the fictitious Coriolis and Poincar{\'e} forces, generally given by
\begin{linenomath*}
\begin{equation}
\mathbf{F}_i=-\underbrace{2\boldsymbol{\Omega}(t)\times \mathbf{u}}_\mathrm{Coriolis}-\underbrace{\frac{\partial \boldsymbol{\Omega}(t)}{\partial t} \times \mathbf{r}}_{\textrm{\scriptsize Poincar\'e}} \ ,
\end{equation}
\end{linenomath*}
where $\mathbf{r}$ is the position vector. We now detail the three cases of interest and their respective inertial forces and frame of reference (see also Figure~\ref{Fig:schema}).

\begin{figure}[ht!]
\centerline{\includegraphics[width=\linewidth]{Figure_1}}
\caption{Schematic of the three configurations considered here. a) Tides: in the orbital frame rotating with the ellipsoidal deformation (i.e. where the tidal bulge is fixed), the fluid is entrained by a tangential velocity at the ellipsoidal boundary. b) Libration: the mantle is rotating with the sum of a constant rotation rate $\Omega_0$ and a periodic modulation, driving the fluid through Coriolis and Poincar\'e forces. c) Precession: the mantle is rotating around two different axes, $\hat{\mathbf{z}}$ and $\hat{\mathbf{z}}_p$, at two different rates given by the Poincar\'e number $Po=\Omega_p/\Omega_0$.}
\label{Fig:schema}
\end{figure}

\subsubsection{Tides}

We consider an idealized tidally-driven flow as detailed in \cite{CEBRON2010} and \citet{Grannan:GJI2016}.
The frame of reference is attached to the elliptical distortion which is rotating at a constant rate $\Omega_{\mathrm{orb}}\mathbf{\hat{z}}$, hereby named as orbital frame.
The dimensionless inertial force $\mathbf{F}_i$ in equation (\ref{Eq:NS}) is therefore just a Coriolis force given by
\begin{linenomath*}
\begin{equation}
\mathbf{F}_i = -2 \gamma\mathbf{\hat{z}}\times\mathbf{u},
\end{equation}
\end{linenomath*}
where $\gamma = \Omega_\mathrm{orb}/{\Omega}_0$ is the ratio between the rotation rate of the ellipsoidal deformation and the absolute spin rate ${\Omega}_0$ of the mantle.
In this orbital frame, the core--mantle boundary rotates at a differential rotation rate $\Omega_0-\Omega_{\mathrm{orb}}$.
Following \citet{CEBRON2010}, a no-slip condition is thus imposed at the inner domain boundary, given by
\begin{linenomath*}
\begin{equation}
\label{eq:uc_tide}
\mathbf{u}_\mathrm{b.c.} = (1-\gamma)\sqrt{1-\frac{z^2}{c_*^2}}\hat{\boldsymbol{\tau}} \ ,
\end{equation}
\end{linenomath*}
where $\hat{\boldsymbol{\tau}}$ is the normalized horizontal tangent vector along the ellipsoidal boundary.
In this letter, we fix $\gamma=-1$, which corresponds to the extreme case where the spin rate of the fluid is exactly opposite to that of the elliptic deformation.
The geometry is given by a tri-axial ellipsoid with $\beta=0.16$ and $c_*=1$.
This particular case was thoroughly documented both numerically and experimentally in \citet{Grannan:GJI2016}.

\subsubsection{Longitudinal libration}
The ellipsoid boundary is rotating around the $\hat{\mathbf{z}}$-axis with a time varying angular velocity given by
\begin{linenomath*}
\begin{equation}
\boldsymbol{\Omega}(t) = \left(1+\frac{\Delta\phi\omega_\mathrm{l} }{\Omega_0} \sin(\omega_\mathrm{l} t)\right)\hat{\mathbf{z}},
\end{equation}
\end{linenomath*}
where $\Omega_0$ is the mean rotation rate, $\omega_\mathrm{l}$ the libration frequency and $\Delta \phi$ the libration amplitude.
It is natural to work in the frame of reference attached to the rigid boundary of the ellipsoidal cavity, called librating frame in the following.
There, the dimensionless inertial force $\mathbf{F}_i$ is
\begin{linenomath*}
\begin{equation}
\mathbf{F}_i = -2\big[1+\epsilon \sin(ft)\big]\hat{\mathbf{z}}\times \mathbf{u} - \epsilon f \cos(ft)\hat{\mathbf{z}}\times\mathbf{r},
\end{equation}
\end{linenomath*}
where we have introduced the libration frequency $f=\omega_\mathrm{l}/\Omega_0$ and the libration amplitude $\epsilon=\Delta\phi\, f$. We impose no-slip boundary conditions for the velocity field on the fixed boundary of the ellipsoidal cavity.
In this letter, we fix $f=4$, $\epsilon=0.8$ and the geometry is a non-axisymmetric spheroid with $\beta=0.34$ and $c_*=0.81$, which was studied in detail both experimentally by \citet{Grannan:PoF2014} and numerically by \citet{Favier:POF2015}.

\subsubsection{Precession}

The ellipsoid spins at $\boldsymbol{\Omega}(t)=\hat{\mathbf{z}}+P_o\hat{\mathbf{z}}_p(t)$ where $\hat{\mathbf{z}}$ and $\hat{\mathbf{z}}_p(t)$ are the unit vectors along the spin and precession axes, respectively.
$\hat{\mathbf{z}}_p(t)$ is inclined with respect to the vertical $\hat{\mathbf{z}}$ with an angle $\alpha_p$ and is given by
\begin{linenomath*}
\begin{equation}
\hat{\mathbf{z}}_p(t)=\sin(\alpha_p)\cos(t)
\hat{\mathbf{x}}-\sin(\alpha_p)\sin(t)\hat{\mathbf{y}}+
\cos(\alpha_p)\hat{\mathbf{z}}.
\end{equation}
\end{linenomath*}
Following \cite{Tilgner:POF2005,Lin:POF2016}, we work in the reference frame attached to the rigid ellipsoidal cavity, referred to as the mantle frame, and the dimensionless force $\mathbf{F}_i$ acting on the fluid is
\begin{linenomath*}
\begin{equation}
\mathbf{F}_i=-2(\hat{\mathbf{z}}+P_o\hat{\mathbf{z}}_p)\times\mathbf{u}-P_o(\hat{\mathbf{z}}_p \times \hat{\mathbf{z}})\times \mathbf{r},
\end{equation}
\end{linenomath*}
where $P_o=\Omega_p/\Omega_0$ is the Poincar{\'e} number.
Following the recent dynamo study in spherical geometry of \cite{Lin:POF2016}, we consider the case $\alpha_p=\pi/2$ and $P_o=-0.1$. We impose no-slip boundary conditions for the velocity field.
Knowing that such a flow is dynamo capable in spherical geometry, we here focus on the effect of the ellipticity on the onset of dynamo action in the turbulent regime.
We therefore consider several cases, from a spherical one with $\beta=0$ and $c_*=1$ to non-axisymmetric ones with $\beta>0$ and $c_*=1/\sqrt{1-\beta^2}$, keeping the fluid volume unchanged as the domain is deformed elliptically.

\subsection{Numerical method and outer insulating domain}

Running numerical simulations in ellipsoidal containers remains a tremendous challenge challenging task.
There have been several attempts using spectral methods for purely hydrodynamical cases \citep[see for example][]{lorenzani2001,SCHMITT2004} but very few results for the magnetohydrodynamical case \citep[see][]{Ivers2017}.
Local methods based on finite elements or finite volumes are more common due to their inherent flexibility for the geometry \citep[see for example][]{Wu:GAFD2009,Cebron:GAFD2012,ernst2013,van2016}, but insulating boundary conditions are then more difficult to consider.
Here, we numerically solve equations~(\ref{Eq:NS})-(\ref{Eq:incom}) using Nek5000, a highly-parallelised spectral-element code developed by Fischer {\it et al.} \citep{FISCHER1997,FISCHER2007,nek5000-web-page}.
Spectral elements can be seen as an intermediate between fully-spectral and local methods.
They combine the geometrical flexibility of finite elements with the exponential convergence of spectral methods.
Nek5000 has been used to study flows driven by tides \citep{favier2014,Grannan:GJI2016,barker2016} and libration \citep{Favier:POF2015}.
Here, we extend these results by also solving for the magnetic potential. All numerical details, as well as several MHD benchmarks and convergence tests, are shown in Supporting Information.

Ideally, one would enclose the fluid cavity in a perfectly insulating outer domain.
This case is usually considered when solving the problem in spherical geometries since the outer potential magnetic field can be implicitly solved using spherical harmonics.
For local methods, this is not possible since the boundary conditions for the magnetic field become non-local.
We choose here to enclose the fluid domain in a larger outer domain with small but finite conductivity \citep{Chan:PEPI2001,Matsui:EPS2004,Guermond:JCP2009}.
The outer surface of the surrounding ellipsoid is given by
\begin{linenomath*}
\begin{equation}
\frac{x^2}{1+\beta} + \frac{y^2}{1-\beta} +\frac{z^2}{c_*^2} = \chi^2,\label{Eq:Ellip_s}
\end{equation}
\end{linenomath*}
where $\chi>1$ is the aspect ratio between the outer and inner domains.
The velocity field is numerically solved only in the inner domain, whereas the vector potential is solved over the two domains with a jump of magnetic diffusivity defined by a factor $\lambda$ at the interface {(i.e. the CMB)}.
In the insulating outer domain, we thus solve
\begin{linenomath*}
\begin{equation}
\frac{\partial\mathbf{A}}{\partial t} = {\mathbf{ u_\mathrm{s} \times(\nabla \times A})} +  \lambda\frac{E}{Pm}\nabla^2 \mathbf{A}.\label{Eq:VP_s}
\end{equation}
\end{linenomath*}
For both precession and libration cases, the mantle is not moving so that $\mathbf{u_\mathrm{s}=0}$ in equation~(\ref{Eq:VP_s}).
For tidally-driven flows however, the outer domain is moving with a constant horizontal tangential velocity so that we cannot neglect the advection term (although it has a negligible contribution since magnetic diffusion is dominant anyway).
{Consistently, the outer magnetic field is advected with a prescribed velocity field given by equation (\ref{eq:uc_tide}), generalised along any elliptical streamline in the outer domain homothetic to the CMB. Note however that this advection term has a negligible contribution since magnetic diffusion is dominant anyway.}

The absence of gauge in (\ref{Eq:VP_f}) and (\ref{Eq:VP_s}) limits us from having a perfectly insulating outer domain surrounding the fluid \citep{Matsui:EPS2004,Cebron:GAFD2012}.
At the interface, all components of the magnetic field and the tangential component of the electric field are continuous \citep{Chan:PEPI2001,Matsui:EPS2004,Matsui:IJCFD2004,Guermond:JCP2009}.
For an infinitely large outer domain, we have asymptotically
\begin{eqnarray}
\mathbf{B}=O(r^{-3}) \quad \textrm{when} \quad  r\rightarrow \infty \ ,\\
\mathbf{A}=O(r^{-2}) \quad \textrm{when} \quad  r\rightarrow \infty \ .\label{Eq:A_inf}
\end{eqnarray}
For sufficiently large outer domain $\chi\gg1$, the condition (\ref{Eq:A_inf}) can be replaced by
\begin{linenomath*}
\begin{equation}
\mathbf{A=0} \label{Eq:A_bc}
\end{equation}
\end{linenomath*}
on the outer boundary \citep{Matsui:IJCFD2004, Chan:PEPI2007}.
Hence we apply the boundary condition (\ref{Eq:A_bc}) on the surface of the boundary given by (\ref{Eq:Ellip_s}).
The initial problem of an infinite insulating outer domain is recovered when both $\lambda\gg1$ and $\chi\gg1$.
A large $\chi$ results in a larger number of grid points and a large $\lambda$ puts  limitations on the convergence properties of our numerical scheme.
In the Supporting Information, we show that the values $\lambda=100$ and $\chi=8$ used in the following are sufficient to reach convergence \citep[see also][]{Chan:PEPI2001}.

\section{Results and Discussion}

\begin{table}
 \caption{Parameters of all performed simulations, with T, L and P standing for tides, libration and precession, respectively.

Input parameters: Magnetic Prandtl number $Pm$, Ekman number $E$, ellipticity $\beta$, and non-dimensional axial length $c_*$.

Response parameters:

 kinetic Reynolds numbers $Re_{z}=U^\mathrm{rms}_{z}/E$ and $Re_\mathrm{tot}=U^\mathrm{rms}/E$, where $U^\mathrm{rms}_{z}=\sqrt{2\langle E_z\rangle}$ and $U^\mathrm{rms}=\sqrt{2\langle E_u\rangle}$, $\langle \cdot \rangle$ representing the time-averaged quantity and $E_u$ the volume-averaged total kinetic energy; and mean growth rate $\sigma$ of the magnetic energy with its standard deviation, determined from the data given in the supporting information. }
 \label{Tab:param}
 \centering
 \begin{tabular}{c c c c c c | c c c c c}
 \hline
 Forcing & Case & $Pm$ & $E\times10^{4}$ & $\beta$ & $c_*$    & $Re_z$ & $Re_\mathrm{tot}$ & $\sigma\times10^{3}$ & Dynamo\\
 \hline
 Tides & T1 & $0.2$ & $2$ & 0.16 & 1.0      & $433$ & 5989 &$-3.04\pm1.5$  &No\\
 Tides &   T2 & $0.5$ & $2$ & 0.16   & 1.0   & $433$ & $5989$ &$1.12\pm0.81$  &Yes\\
 Tides &   T3 & $1.0$ & $2$  & 0.16 & 1.0     & $433$ & $5989$ &$19.6\pm1.6$  &Yes\\
 Tides &   T4 & $2.0$ & $2$ & 0.16  & 1.0     & $433$ & $5989$ &$55.6\pm2.1$  &Yes\\
  \hline
Libration & L1 & $1.0$ & $1.34$ & $0.34$ & 0.81 & $264$ & $2886$ &$-4.2\pm0.41$  &No\\
Libration & L2 & $2.0$ & $1.34$  & $0.34$ &0.81 &  $264$ & $2886$ &$-0.12\pm0.39$  &No\\
Libration & L3 & $3.0$ & $1.34$ & $0.34$ & 0.81  &  $264$ & $2886$ &$2.11\pm0.48$  &Yes\\
Libration & L4 & $4.0$ & $1.34$ & $0.34$  & 0.81 &  $264$ & $2886$ &$5.74\pm0.54$  &Yes\\
  \hline
Precession & P0 & $1.0$ & $1$ & 0.0 & 1.0  &  1138 & $6280$    & $24.1\pm1.1$ &Yes\\
Precession & P1 & $1.0$ & $1$ & 0.1 & 1.005  &  1159 & $6289$   & $36.8\pm1.1$ &Yes\\
Precession & P2 & $1.0$ & $1$ & 0.2 & 1.021  &  1677 & $6239$  & $53.6\pm1.9$ &Yes\\
 \hline
 \end{tabular}
\end{table}

\color{black}

For the libration and tides cases considered in this letter, we fix the geometry, forcing amplitude, and Ekman number following previous studies, then we gradually vary the magnetic Prandtl number.
For the precession forcing where dynamo action was already shown in the sphere \citep[][]{Tilgner:POF2005,kida2011turbulent, Lin:POF2016}, we fix the forcing amplitude, Ekman number and magnetic Prandtl number following those previous studies, then we gradually vary the ellipticity to see how it affects the dynamo capability.
All the parameters are detailed in Table \ref{Tab:param}.
For tides, we consider $E=2\times10^{-4}$ \citep[case $N6$ of][]{Grannan:GJI2016}.
For libration, we choose $E=1.34\times10^{-4}$ \citep[case {$A6$} of][note the different reference length-scale used here]{Favier:POF2015}.
For precession, we choose $E=10^{-4}$ \citep[see Table 1 in][for the spherical equivalent]{Lin:POF2016}.
For all cases, we start with a purely hydrodynamic simulation until it reaches a quasi-steady turbulent state, checked to be consistent with the results previously obtained with a single fluid domain only.
The details of the mechanism responsible for the turbulent motions have been discussed in details in previous papers \citep[see][and references therein]{le2015flows, Lebars:PRF2016} and we focus here on the magnetohydrodynamic properties of these flows.
We then restart the simulation at a fixed magnetic Prandtl number and solve simultaneously for the magnetic potential including {an initial magnetic perturbation} in the form of an axial dipole in the fluid part of the domain.
This particular magnetic initial condition {(as well as its amplitude)} is irrelevant for the linear kinematic problem and is used here for simplicity.
We have checked that the growth rate of the dynamos presented in this paper does not depend on this arbitrary choice.
 Simulations are pursued until observing exponential growth or decay over many decades (see e.g. Figure~\ref{Fig:growth}(a)). Then, the simulations are restarted using a higher-spectral order and more constraining convergence tolerance in order to check that the results are converged (see more details in the Supporting Information).

For the first time we obtain self-consistent turbulent kinematic dynamos driven by mechanical forcings in an ellipsoidal geometry.
In Figure~\ref{Fig:growth}(a), we show a typical example corresponding to the tidally-driven case T4 in Table \ref{Tab:param}.
We consider the time evolution of volume-averaged quantities such as the squared vertical velocity component ($E_z$) and magnetic energy ($E_b$) computed using the following definitions
\begin{eqnarray}
E_z(t) &=& \frac{1}{2V}\int_V u_z^2dV,\\
E_b(t) &=& \frac{1}{2V}\int_V \mathbf{B}^2 dV,
\end{eqnarray}
where $V$ is the total volume of the ellipsoidal fluid cavity and $u_z$ is the vertical component of the velocity.
We observe that the magnetic field grows exponentially for $Pm=2$, which clearly shows that our tidally-driven flow is dynamo capable.
Note that the magnetic field growth is non-monotonic.
This is a direct consequence of the very intermittent nature of the underlying turbulent flow, with burst of intense turbulence separated by more quiet phases.
This is characteristic of the saturation of the hydrodynamical instability responsible for the turbulence, the so-called elliptic instability (at least for the tidally-driven and libration-driven cases).
This inevitably leads to significant uncertainties when estimating the growth rate from a finite time series.
We therefore run the simulations for several hundreds of rotation times so that the growth rate can be estimated with a reasonable accuracy.

The main result of this paper is shown in Figure~\ref{Fig:growth}(b, c, d). For  all the mechanical forcings, we obtain kinematic dynamo action.
The critical magnetic Prandtl number is typically around unity for these moderate Reynolds numbers simulations.
Note that the kinetic Reynolds number varies between the different forcings (see Table \ref{Tab:param}) so that it is too early to discuss the relative dynamo efficiency between different cases.
For the precession forcing, we first recover the growth rate obtained in the spherical case ($\beta=0$) by \cite{Lin:POF2016}.
Additionally, we observe that the growth rate of the dynamo increases with $\beta$.
This positive effect of the ellipticity of the dynamo capability of precessional flows could play a major at very low Ekman number where the viscous coupling between the mantle and the fluid becomes less and less important, and only topographic coupling remains {\citep[][]{Jault2007}}.

\begin{figure}[ht!]
\centerline{\includegraphics[width=\linewidth]{Figure_2}}
\caption{(a) Evolution of the vertical kinetic and magnetic energies of the tidally driven dynamo for $Pm=2$ (case T4, see Table \ref{Tab:param}). (b, c) Growth rate $\sigma$ of the magnetic field for kinematic dynamo driven by tides and libration as a function of the magnetic Prandtl number. (d) growth rate $\sigma$ of the magnetic field for precession dynamo as a function of the equatorial ellipticity $\beta$ of the domain. The hollow circle and square show the mean growth rate in the sphere from \citet{Lin:POF2016} and our case P0, respectively. The black error bars represent one standard deviation and the gray bars represent maximum and minimum estimates.}
\label{Fig:growth}
\end{figure}

\begin{figure}
\centerline{\includegraphics[width=\linewidth]{Figure_3}}
\caption{(a, b, c) meridional {(x,z)} slices of the magnitude of the vorticity $|\boldsymbol{\omega} |$, (d, e, f) meridional {(x,z)} slices of the magnitude of  of the magnetic field $|\mathbf{B}|$, and (g, h, i) amplitude of the normal component of the magnetic field at the inner domain boundary (i.e. the CMB) $B_{n,CMB}$, for dynamos driven by tides, libration, and precession in the first, second and third columns, respectively (see cases T4, L4 and P2 in Table \ref{Tab:param}).
}
\label{Fig:visus}
\end{figure}

Finally, we show in Figure~\ref{Fig:visus} visualizations for each forcing. The magnitudes of the vorticity and magnetic field in a meridional plane, as well as the normal magnetic field at the CMB, are shown. Both tides and libration are very similar, which is not surprising since they rely on the same hydrodynamic elliptical instability mechanism to drive the bulk turbulent flow: vorticity and magnetic field are then spread over the whole domain. Although the kinematic nature of these dynamos does not allow us to perform a detailed analysis of the shape of the magnetic field, we observe, during the exponential growth of the magnetic field and in the absence of any Lorentz force, a dominantly multipolar structure, as also reported for some kinematic precession dynamos in the sphere \citep{tilgner2007kinematic}. For our precession cases, most of the vorticity and magnetic field are concentrated close to the boundary, similarly to the turbulent ring dynamo first shown by \cite{kida2011turbulent} in the sphere: the precessional flow shown here is still strongly related to the viscous coupling between the mantle and the fluid. A bulk instability similar to the two other forcings is, however, expected at lower Ekman number \citep{kerswell1993instability}, which should be explored by additional simulations.

\section{Conclusion}

In conclusion, we have presented the first self-consistent numerical proofs of the existence of mechanically-driven dynamos in geophysically relevant settings, including non-axisymmetric core geometries and fully turbulent flows.
Obviously, as for (even the most recent) convectively-driven dynamos {\cite[see e.g.,][]{schaeffer2017turbulent}}, the dimensionless parameters of our simulations, like the Reynolds and the Ekman numbers, remain far from the planetary ones: turbulence and dynamo thresholds have thus been reached by artificially increasing the amplitude of the mechanical forcings and of the magnetic Prandtl number, respectively.
Also, our results remain up to now limited to kinematic dynamos with no retro-action of the generated magnetic field on the turbulent flow: in this context, no systematic study of the magnetic field topology nor intensity is yet possible.
But we want to stress the following three points.
First, the results presented here already constitute a challenging numerical task, even for the most advanced high performance computing.
Second, the results presented here  aposteriori validate various exotic scenarii of planetary magnetic fields that have been debated during the recent years: e.g., on Mars \citep[][]{arkani2008tidal}, Moon \citep[][]{Lebars2011}, early Earth \citep[][]{andrault2016deep}.
Finally, the results presented here are expected to open new horizons and stimulate additional studies, that we hope will lead to rapid progress in our understanding of those mechanically-driven dynamos. Note in particular that while the models of convectively-driven and mechanically-driven dynamos are often presented as antithetical, they could actually co-exist and even collaborate to produce planetary magnetism \citep[][]{wei2016combined}, a behavior up to now largely unexplored.

Studies of mechanically-driven dynamos are still in their infancy. Meanwhile, it is tempting to already extrapolate on the expected magnetic fields, and more specifically on the possibility of obtaining a large-scale magnetic field of interest for planetary applications. As studied in details by \citet{le2017inertial}, the non-linear saturation of mechanically-driven turbulence can give rise either to large-scale structures or to an inertial wave turbulence. In the former case, the large-scale structures are due to an inverse cascade mechanism from the small scale patterns excited at the instability onset, as classical in rotating turbulence \citep[see also][]{barker2013non, lin2015shear, barker2016turbulence}. Large-scale structures are then capable of sustaining powerful and large-scale magnetic fields \citep[][]{Lin:POF2016}, even if Joule dissipation tends to limit the inverse cascade efficiency \citep[][]{barker2013mag}. The situation is more complex in the later case, where the flow is made of a continuous spectrum of weakly interacting, small-scale inertial waves. But in this case also, the seminal theoretical work of \citet{moffatt1970dynamo} \cite[see also][]{davidson2014dynamics,galtier2014weak} actually predicts the emergence of a large-scale dynamo, which remains to be studied in the context of mechanically-driven flows. Those speculative, but positive conclusions clearly deserve more investigation.

\acknowledgments

This research is funded by the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program through grant agreement No 681835-FLUDYCO-ERC-2015-CoG. We gratefully acknowledge the computational hours provided on Turing and Ada (Project No. A0020407543) of IDRIS and on HPC resources (Project No. 017B020) of Aix-Marseille Universit\'e financed by the project Equip@Meso (ANR-10-EQPX-29-01) of the program Investissements d'Avenir supervised by the Agence Nationale de la Recherche. We thank Yufeng Lin for providing us with the numerical data of his precessional dynamo in a sphere and David C\'ebron for his comments on an earlier version of this manuscript.
The spectral element solver Nek5000 is available online \cite[][]{nek5000-web-page}. All numerical results are available upon request from Benjamin Favier (e-mail: favier@irphe.univ-mrs.fr).

\section{Numerical implementation in Nek5000}

Nek5000 is able to solve MHD problems using the Elsasser variables.
This severely constrains the available boundary conditions for the magnetic field: typically, the  boundary conditions for the velocity and magnetic fields have to be the same.
This is the main reason why we use the magnetic vector potential instead of the magnetic field.
This allows us to use the conjugate solver of Nek5000 where the hydrodynamic flow is solved in a sub-domain while magnetic vector potential equations can be solved in both the inner fluid and outer domains.
Working with the magnetic vector potential also has the advantage of implicitly imposing a divergence-free magnetic field.

We divide the computational domain into $\mathcal{E}$ hexahedral elements.
Within each element, the velocity, vector potential and pressure are represented as the tensor-product Lagrange polynomials of the orders $N$ and $N-2$ based at the Gauss-Lobatto-Legendre and Gauss-Legendre points, respectively.
The degree of freedom scales as $N^3\mathcal{E}$, the numerical convergence is algebraic with increasing the number of elements $\mathcal{E}$ and exponential with increasing the polynomial order $N$.
We use a third-order implicit integration scheme for diffusive terms and a third-order explicit scheme for all remaining nonlinear and inertial terms.
The spectral order we use varies from $N=7$ for tides and libration to $N=9$ for precession (see the numerical convergence tests below) and we use the $3/2$ dealiasing rule to accurately compute the nonlinear terms.
The code is MPI parallelized and we performed our simulations on $1024$ processors typically.

In Figure~\ref{fig:mesh} we show the high-resolution mesh divided into 28672 elements. Coupled with a polynomial order $N=9$, this leads to approximately $2\times10^7$ degrees of freedom.
The fluid mesh contains $19456$ elements and is naturally more refined than the much more diffusive outer domain.
To resolve the viscous boundary layers and to resolve the sharp gradients in the magnetic vector potential $\mathbf{A}$ at the interface, we refine the grid on both sides of the boundary of the fluid domain.

\begin{figure}[h!]
\setfigurenum{S1}
\noindent\includegraphics[width=\linewidth]{S_Figure1}
\caption{Cut through the global ellipsoidal mesh. In the zoomed part we show the mesh for the fluid domain only, which is more densely packed than for the outer domain.}
\label{fig:mesh}
\end{figure}

\section{Benchmarks}

\subsection{Galloway-Proctor Dynamo}

In order to validate our implementation of the magnetic vector potential equations, we consider the case of the Galloway-Proctor dynamo \citep{Galloway1992,Cattaneo:PRL1995}.
We solve the kinematic dynamo problem in a 3D-periodic Cartesian domain of length $(2\pi,2\pi,2\pi/k_z)$, where $k_z=0.57$ is the optimal wave-number for dynamo action.
The imposed velocity field is given by
\begin{eqnarray}
u_x &=& -\sin(y+\sin\omega t),\\
u_y &=&-\cos(x+\cos \omega t),\\
u_z &=&\sin(x+\cos\omega t)+\cos(y+\sin \omega t) \ .
\end{eqnarray}
This kinematic problem is solved both with our magnetic vector potential approach and with the native MHD solver available with Nek5000 based on Elsasser variables. The domain is made of 128 elements and the order of polynomial used within each element is $N=5$.
Our results are also compared with results obtained using classical pseudo-spectral methods \citep{Cattaneo:PRL1995}.
The initial condition is given by $\mathbf{A}=(0,0,\cos(y) \sin(k_z z))$.
The growth rates for various magnetic Reynolds numbers are shown in Figure~\ref{fig:GP_growth}.
The agreement between the different methods is excellent and validates our implementation of the MHD equations for an idealized periodic case.

\begin{figure}[h!]
\setfigurenum{S2}
\noindent\includegraphics[width=\linewidth]{S_Figure2.pdf}
\caption{Growth rates of the magnetic field for the Galloway-Proctor kinematic dynamo problem versus the magnetic Reynolds number. $+$ correspond to the vector potential method used in this study. Crosses and hollow circles represent the growth rates obtained from the MHD solver of Nek5000 using Elsasser variables and from \citet{Cattaneo:PRL1995}, respectively.}
\label{fig:GP_growth}
\end{figure}

\subsection{Freely decaying modes in a conducting sphere}

In order to check our implementation of the insulating boundary conditions, we consider the purely diffusive decay of a magnetic field inside a conducting sphere of unit radius surrounded by an insulating infinite domain.
We thus solve the simple equation $\partial_t\mathbf{B}=\nabla^2\mathbf{B}$.
This linear equation has an infinite set of eigensolutions. The slowest decay occurs for an axial dipole and is given by \citep[see][]{Iskakov:JCP2004}
\begin{equation}
\label{eq:decay}
{\bf B} = {\bf B}_0\exp(-\pi^2 t) \ .
\end{equation}
Numerically, we solve this problem in a unit sphere surrounded by a larger sphere with radius $\chi=8.5$ and with a magnetic diffusivity increased by a factor $\lambda$. At the outer sphere boundary, we impose $\mathbf{A}=\mathbf{0}$, as in the simulations shown in the paper.
The entire domain is made of 1120 elements, including 448 elements for the inner domain, and the order of polynomial used within each element is $N=5$.
Our initial condition is an axial dipole of arbitrary amplitude and we consider different diffusivity ratio $\lambda$.
Figure~\ref{fig:decay_sphere} shows the relative error between the measured growth rate $\sigma$ from our simulation and the theoretical prediction $\sigma_\mathrm{th}$ given by equation~(\ref{eq:decay}).
As expected, we observe a rapid decrease of the error as $\lambda$ increases, and the relative error is less than $1\%$ when $\lambda=100$, which is the typical value used throughout this paper.
This test validates our implementation of the insulating boundary conditions using a multi-domain approach with a jump in the magnetic diffusivity at the boundary of the fluid domain.

\begin{figure}[h!]
\setfigurenum{S3}
\noindent\includegraphics[width=\linewidth]{S_Figure3}
\caption{Relative error on the decay rate of an axial dipole in a unit sphere as a function of the diffusivity ratio $\lambda$ between the outer and inner domains.}
\label{fig:decay_sphere}
\end{figure}

\subsection{Dudley-James dynamos}

We now consider a test problem when both advection and diffusion of the magnetic field are involved in a confined domain: the so-called Dudley and James dynamos \citep{DudleyJames1989}.
The induction equation is solved in a unit sphere surrounded by an insulating domain.
The imposed flow corresponds to the so-called $s_2t_2$ case of \cite{DudleyJames1989} (see their equation (24) p.421), which is a simple superposition of selected spherical harmonics with prescribed radial structures.
Again, we solve this problem using our numerical approach, fixing $\chi=8.5$, $\lambda=100$ and varying the magnetic diffusivity.
The entire domain is made of 1120 elements, including 448 elements for the inner domain, and the order of polynomial used within each element is $N=5$.
The initial condition is an equatorial quadrupole of arbitrary amplitude.
We compare the growth rate from the eigenproblem solved by \cite{DudleyJames1989} and those obtained with our initial value numerical integration in Figure~\ref{fig:dj}.
Despite the moderate numerical resolution used, the agreement is excellent, which further confirms that our values of $\chi$ and $\lambda$ are large enough to efficiently mimic an insulating boundary in a kinematic dynamo configuration.

\begin{figure}[h!]
\setfigurenum{S4}
\noindent\includegraphics[width=\linewidth]{S_Figure4}
\caption{Growth rate of the magnetic field for the kinematic dynamo driven by the  $s_2t_2$ flow. Black triangles represent the growth rates extracted from Fig. 8a of \citet{DudleyJames1989}. Black circles correspond to growth rates obtained from our simulations. }
\label{fig:dj}
\end{figure}

\section{Numerical convergence}

We now discuss how the results shown in this letter depend on our particular choice of numerical and geometric parameters.
We focus on the effect of the spatial resolution through the polynomial order $N$.
The impact of the aspect ratio $\chi$ and diffusivity ratio $\lambda$ are then considered.
In all cases, we consider the particular case $T4$ in Table 1 of the main text, which is a tidally-driven dynamo at $Pm=2$.
This case is particularly demanding due to the large magnetic Prandtl number and due to the fact that the outer domain is actually moving (\textit{i.e.} $\mathbf{u}_s\neq\mathbf{0}$ in equation~(14)) so that large diffusivity ratio is required to accurately model the outer insulating boundary.

\subsection{Convergence with $N$}

For case $T4$ in Table 1 of the main text, we performed three simulations which only differ by the polynomial order $N$ to check whether our numerical results are converged. As shown in  Figure~\ref{fig:Conv_N},
the resulting growth rate $\sigma$ is nearly the same for $N=7$ and $N=9$.
We conclude that the order of polynomial $N=7$ is sufficient to numerically resolve this problem, and use it for the tidally-driven and libration-driven simulations presented in the main paper.
For the more requiring precession cases, a similar convergence study led us to use $N=9$.

\begin{figure}[h!]
\setfigurenum{S5}
\noindent\includegraphics[width=\linewidth]{S_Figure5}
\caption{Growth rate $\sigma$ of the magnetic energy as a function of the order of polynomial $N$ within each element of the total domain, for the case T4 in Table 1 of the main text. The black error bars represent one standard deviation and the gray bars represent maximum and minimum estimates.}
\label{fig:Conv_N}
\end{figure}

\subsection{Convergence with $\chi$}

We now consider the effects of changing the aspect ratio $\chi$ on the solution.
We consider different aspect ratios from $\chi=4$ up to $\chi=12$ and compute the growth rate $\sigma$ of the resulting dynamo.
The total number of elements in the mesh for $\chi=4$, $8$ and $12$ are $27136$, $28672$ and $30208$, respectively.
We keep the number of elements in the fluid the same and fix $N=7$ and $\lambda=100$.
In Figure~\ref{fig:Conv_chi}, we show the convergence of $\sigma$ with $\chi$.
While $\chi=4$ slightly underestimates the growth rate, $\chi=8$ and $\chi=12$ are very similar.
We conclude that the choice of $\chi=8$ is sufficient for the artificial effect of the outer boundary to be negligible in our simulations~\citep[see also][]{Chan:PEPI2007}.

\begin{figure}[h!]
\setfigurenum{S6}
\noindent\includegraphics[width=\linewidth]{S_Figure6}
\caption{Growth rate $\sigma$ of the magnetic energy as a function of the aspect ratio $\chi$ between the outer and the inner domains, for the case T4 in Table 1 of the main text. The black error bars represent one standard deviation and the gray bars represent maximum and minimum estimates.}
\label{fig:Conv_chi}
\end{figure}

\subsection{Convergence with $\lambda$}

Finally, let us consider the effect of the ratio of diffusivity between the outer and inner domains.
The cost of a simulation rapidly goes up with increasing $\lambda$ due to the larger number of iterations required to reach a given convergence threshold.
We nevertheless need to choose a large enough ratio $\lambda$ to accurately model the insulating outer domain.
In Figure~\ref{fig:Conv_lambda}, we show the variation of the growth rate $\sigma$, again for case $T4$, for different values of the ratio of diffusivity from $\lambda=50$ up to $\lambda=1000$.
Lower values of $\lambda$ are irrelevant and very demanding numerically since the magnetic field topology is more complex and would require an increase in the resolution used in the outer domain.
We observe that $\lambda=50$ overestimates the growth rate whereas $\lambda=10^2$ is very close to $\lambda=10^3$ with a relative error of less that $2\%$.
We therefore conclude that using $\lambda=10^2$ is enough to accurately model the outer insulating domain.

\begin{figure}[h!]
\setfigurenum{S7}
\noindent\includegraphics[width=\linewidth]{S_Figure7}
\caption{Growth rate $\sigma$ of the magnetic energy as a function of the diffusivity ratio $\lambda$ between the outer and the inner domains, for the case T4 in Table 1 of the main text. The black error bars represent one standard deviation and the gray bars represent maximum and minimum estimates.}
\label{fig:Conv_lambda}
\end{figure}

\end{article}

redpajama_set_name: RedPajamaArXiv


text:
I'M THINKING OF ENDING THINGS – Review by Diane Carson
September 8, 2020 September 13, 2020 Diane Carson 0 Comments charlie kaufman, david thewlis, i'm thinking of ending things, jesse plemons, netflix, Toni Collette
I'm Thinking of Ending Things is another Charlie Kaufman adventure
For anyone ready to abandon logical narratives, coherent dialogue, and the laws of physics, there's an alternative. Director Charlie Kaufman's I'm Thinking of Ending Things bears little resemblance to conventional cinema or reality as ordinarily presented. In fact, so convoluted are the film's flights of fancy in incongruous scenes that no one, including Kaufman, could answer star Jesse Plemons' question.
According to the September 6 New York Times feature on Plemons, as he and other actors puzzled over the story, Plemons asked, "Can you tell us what this is about?" Kaufman replied, "You know, I don't know." I can report only the basic elements. Adapted from Iain Reid's 2016 novel, a newly romantic couple, Lucy and Jake drive through a raging snowstorm to have dinner with Jake's parents on their isolated farm. The delightfully wacky dinner scene serves up supremely surreal humor that surpasses any definition of normality. Credit to, Toni Collette and David Thewlis who, as Jake's parents, give inspired performances to unhinged characters who shape shift through time warps.
Occasional interruptions to the dinner signal the illogical events to come as Lucy keeps insisting that she has to get back to her apartment that night. She and Jake do begin that return trip, the snowstorm continuing to rage. Along the way, topics range from Oscar Wilde to David Foster Wallace, a debate over the sexism or lack thereof of the song Baby It's Cold Outside, Lucy reciting perfectly a Pauline Kael film review of A Woman Under the Influence, without any attribution, plus a lovely ballet in a high school's hallways and songs from Oklahoma. If all this sounds disjointed, to push the dislocations further, Jake and Lucy stop for ice cream in the middle of nowhere. Jessie Buckley and Jesse Plemons embody their daft but serious characters, alternately stuck and unstuck in time, rather like Vonnegut's Billy Pilgrim.
Kaufman's previous films—Being John Malkovich, Eternal Sunshine of the Spotless Mind, and Anomalisa—prepare viewers for this dive down the rabbit hole of memory and joyful exploration of disconnected sequences. Figuring out how the pieces fit is a pointless endeavor. The only way to weave happily through this two and a quarter hour fantasy is to surrender to the tantalizing, playful, disjointed interactions and embrace the wildly unusual joy of letting go of reason and judgment.
I'm Thinking of Ending Things is available on Netflix.
← VIOLATION (TIFF20) – Review by Alexandra Heller-Nicholas
SHIVA BABY (TIFF20) – Review by Alexandra Heller-Nicholas →
Diane Carson
Diane Carson, Ph.D., Professor Emerita, has reviewed films for over 25 years and has covered the Cannes, Telluride, Toronto, Palm Springs, and Sundance festivals. She writes for KDHX, 88.1 FM. St. Louis' community radio. One of the founders of the St. Louis International Film Festival, she continues to serve on juries. A past president of the University Film and Video Association, she taught film studies and production at St. Louis Community College and at Webster University. Her new book, written with two colleagues, is "Appetites and Anxieties: Food, Film, and the Politics of Representation," Wayne State U. Press, 2014.


text:
Don Jon: a conquest for Gordon-Levitt
Jon Martello is a man who knows his priorities: his body, his pad, his cars, his family, his church, his girls...and his porn. Especially the porn.
Martello, played by Joseph Gordon-Levitt in the new film, Don Jon, is a buffed-up Jersey bartender with slicked back hair and, as mentioned, a porn addiction. Despite a routine that consists of taking a different beautiful woman home from the club each weekend, Jon is never quite satisfied and prefers the glow of his computer screen to the company of real women.
He feels no need to pursue a real relationship until he encounters Barbara (Scarlett Johansson), the most beautiful woman he's ever seen--a clear "10," his friends concede. Unlike the girls Jon typically beds, Barbara is not so easily seduced, forcing him to pursue her. Inevitably, the two become a serious couple. Jon, however, finds that he is still not content and is unable to give up his addiction. To complicate matters further, Barbara is also nursing her own addiction: Hollywood romances that give her a concept of love that is equally chimerical as Jon's perception of sex.
Gordon-Levitt proves with Don Jon that he is not only a talented actor but an adept director and screenwriter with a broad future ahead of him. He manages to tackle the subject of porn, an area many writers shy away from, and its effects on people and their relationships in a light and humorous, yet raw and honest way. Leading the cast, he gives a strong, compelling, confident and funny performance as Jon, a character who in other hands may not have been likable.
Johansson is captivating as the self-serving Jersey babe stealing scenes with surprising depth. The film also stars Tony Danza and Glenne Headly, who are perfectly cast and share great chemistry as Jon's comical, nosy, but well-meaning parents. But perhaps the best performance of all comes from Oscar nominee Julianne Moore, who plays the vulnerable, damaged and authentic older woman, Esther, whom Jon meets at a night school class Barbara makes him join in order to further his career. Watching their unlikely friendship and connection grow gives the film its real emotional depth.
Ultimately though, this film isn't about porn. It's about connection and separating fantasy from reality, lust from love, and yes, porn from actual sex.
CultureJennifer Verzuh October 1, 2013 Don Jon, film, Joseph Gordon-Levitt, Julianne Moore, Scarlett Johansson1 Comment
King's students on why things are getting Syri-ous
OpinionJosh Craddock and Julia Scheder October 4, 2013 President Obama, Syria, Vladimir Putin
Pier 17 to be demolished, many businesses still closed after Hurricane Sandy
CityAlex Nykamp September 30, 2013 Hurricane Sandy, Pier 17, South Street Seaport


text:
Q: Xcode - Can I develop for iOS 11.1 in El Capitan? I'm a software development student and I'm building an iOS app for a class.
The thing is I have a MacBook Pro Mid 2009 with El Capitan 10.11.6 (15G17023)
and an iPhone 5s running iOS 11.1.2 (15B202).
The latest version of Xcode compatible with El Capitan (I think) is 8.2.1 and it is not compatible with my iOS version.
The app I'm trying to make does not require ARKit or anything that advanced and I would like to know if is there a way I can make this work with my actual devices?
I really don't have the money to upgrade my MacBook for a newer one nor for an older iPhone.
Thanks a lot for your help!

Edit: I no longer have this problem but obviously the question will stay open because we haven't found a solution nor a proper answer.
What I did was install This High Sierra Patcher and from there update Xcode and everything necessary to develop.
I do not recommend this: you are making modifications to your computer that can result in unexpected behavior and you know, all that anti-piracy speech... and also Xcode runs terribly slow (there is a reason why this computer model cannot be updated anymore.)

A: I hope you get a better answer, because this is not ideal but is all I have:
You could develop using the latest version of Xcode that will run on your Mac using the simulator for day-to-day testing. Then when you really need to test on a real device, upload a beta to the App Store, configure yourself as an Internal Tester and use TestFlight to download the app to your 'phone.
Edit: This may also require a full developer account!

redpajama_set_name: RedPajamaStackExchange


Today is Mother's Day, but as we all well know, everyday is a good day to show your mom how much she means to you.
We all show our appreciation in different ways.
For one, Ludacris just remodeled his mother's home. It was her Mother's Day gift as apart of VH1's Dear Mama special according to Hot New Hip Hop.
Additionally, the late, lyrically adept, Tupac honored his mother, the late Afeni Shakur, with the release of the classic "Dear Mama" in 1995.
If you're at a loss for words on this Mother's Day- play one of these loving tracks. Mothers, thank you- forever!


A new video from Osram Opto Semiconductors illustrates how LED technology is used in modern applications and how it is affecting our daily lives. The video is highly interesting for everyone from tech fans to lighting experts as it gives a very comprehensive overview of LED applications and provides an outlook on how the technology will be used in the future.
Modern lighting offers significant advantages compared to common light bulbs. Why is this important? Well, an average person interacts with over 140,000 LEDs per day. Innovative illumination and LED applications can profit from the high-tech product portfolio offered by Osram Opto Semiconductors. For full design support, additional information and complementary products visit EBV's Lightspeed Website.


text:
III Asian Games
Ever Onward
Nations participating
Athletes participating
112 in 13 sports
Officially opened by
Hirohito
Emperor of Japan
Mikio Oda
Main venue
← Manila 1954
Jakarta 1962 →
The 1958 Asian Games, officially the Third Asian Games (Japanese: 第3回アジア競技大会) and commonly known as Tokyo 1958, was a multi-sport event held in Tokyo, Japan, from 24 May to 1 June 1958. It was governed by the Asian Games Federation. A total of 1,820 athletes representing 20 Asian National Olympic Committees (NOCs) participated in the Games. The program featured competitions in 13 different sports encompassing 97 events, including four non-Olympic sports, judo, table tennis, tennis and volleyball. Four of these competition sports – field hockey, table tennis, tennis and volleyball – were introduced for the first time in the Asian Games.
This is the first time that Japan hosted the Asian Games.
The Asian Games is a multi-sport event, much like the Summer Olympics (albeit on a much smaller scale), with participation exclusively for Asian countries. The first edition was held in the capital city of India, New Delhi, in 1951, attracting 489 competitors from 11 nations.
The programme for the Tokyo 1958 Games included 13 different sports divided into 97 events. Four of these sports – judo,[1] table tennis,[2] tennis[3] and volleyball[4] – were not on the official Olympic sports programme at that time. Badminton was added as a demonstration sport, which, from 1962 onwards, became a regular competitive sport in the Asian Games.[5] Judo was another demonstration sport.
Athletics (31) (details)
Basketball (1) (details)
Boxing (10) (details)
Cycling (6) (details)
Diving (4) (details)
Field hockey (1) (details)
Football (1) (details)
Shooting (6) (details)
Swimming (21) (details)
Table tennis (7) (details)
Tennis (5) (details)
Volleyball (2) (details)
Water polo (1) (details)
Weightlifting (8) (details)
Wrestling (8) (details)
The tradition of torch relay, inspired by the Olympic Games, was introduced for the first time in the Asian Games in 1958.[6] The relay officially began from the main venue of the Second Asian Games, Rizal Memorial Coliseum, in Manila, Philippines. In the host nation, Japan, it was relayed from Okinawa to Kyushu Island. Okinawa was under the United States administration at that time. At the opening ceremony, the Games cauldron was ignited by the first Japanese Olympic gold medallist and the first Asian Olympic champion in an individual event, Mikio Oda.[6][7]
Participating nations
A record total of 1,820 athletes representing 20 member nations of the Asian Games Federation participated in the Games. The number of participating countries was also greatest in comparison to the first two editions of the Games.
The Thai delegation held a meeting on 22 May 1958 in Tokyo, and invitations were sent to the representatives of Malaysia, Burma and Laos. The agenda of the meeting was to discuss the possibility of forming a regional multi-sport event on the lines of Asian Games for the countries of Southeast Asia. This way the Southeast Asian Peninsular Games (SEAP Games), which later became the Southeast Asian Games, were established and the first SEAP Games were held in Bangkok, Thailand, in 1959.[8]
Participating National Olympic Committees
Ceylon (11)
Malaya (80)
North Borneo (8)
Republic of China (136)
South Vietnam (32)
The opening ceremony of the Tokyo 1958 Games was organised on 24 May 1958 at the National Olympic Stadium. The ceremony, among other dignitaries and guests, included the Emperor of Japan Hirohito, crown prince Akihito and Shah of Iran Mohammad Reza Pahlavi. Around 70,000 people attended the opening ceremony.[9]
In the following calendar for the 1958 Asian Games, each blue box represents an event competition, such as a qualification round, on that day. The yellow boxes represent days during which medal-awarding finals for a sport were held. The numeral indicates the number of event finals for each sport held that day. On the left, the calendar lists each sport with events held during the Games, and at the right, how many gold medals were won in that sport. There is a key at the top of the calendar to aid the reader.
OC Opening ceremony ● Event competitions 1 Event finals CC Closing ceremony
May / June 1958
Ceremonies OC CC
Athletics 5 6 6 5 9 31
Basketball ● ● ● ● ● ● ● 1 1
Boxing ● ● ● 10 10
Cycling – Road 2 2
Cycling – Track ● 1 ● 2 1 4
Diving 1 1 1 1 4
Field hockey ● ● ● ● 1 1
Football ● ● ● ● ● ● 1 1
Shooting 1 2 1 ● 1 1 6
Swimming 6 5 5 5 21
Table tennis ● ● 2 ● ● ● 5 7
Tennis ● ● ● ● 2 3 5
Volleyball ● ● ● ● ● ● 2 2
Water polo ● ● ● 1 1
Weightlifting 2 2 2 2 8
Wrestling ● ● 8 8
Total gold medals
Main article: 1958 Asian Games medal table
Athletes from 16 countries won medals, leaving four countries without a medal, and 11 of them won at least one gold medal. Afghanistan, Cambodia, Nepal and North Borneo did not win any medal. The Japanese 4 × 100 metres medley relay team of Keiji Hase (backstroke), Masaru Furukawa (breaststroke), Manabu Koga (freestyle) and Takashi Ishimoto (butterfly) won the gold medal with a time of 4:17.2 and broke the world record.[10]
The ranking in this table is consistent with International Olympic Committee convention in its published medal tables. By default, the table is ordered by the number of gold medals the athletes from a nation have won (in this context, a nation is an entity represented by a NOC). The number of silver medals is taken into consideration next, followed by the number of bronze medals. If nations are still tied, equal ranking is given; they are listed alphabetically by IOC country code.
The top ten ranked NOCs at these Games are listed below. The host nation, Japan, is highlighted.
* Host nation (Japan)
Japan (JPN)*
Philippines (PHI)
South Korea (KOR)
Iran (IRN)
Pakistan (PAK)
India (IND)
South Vietnam (VNM)
Burma (BIR)
11–16 Remaining 1 2 16 19
Totals (16 nations)
^ "Judo at the 1964 Tokyo Summer Games – Overview". Sports Reference. Archived from the original on 17 April 2020. Retrieved 4 January 2014.
^ "Table tennis at the 1988 Seoul Summer Games – Overview". Sports Reference. Archived from the original on 17 April 2020. Retrieved 4 January 2014.
^ "2 More Olympic Games". The New York Times. October 2, 1981. Retrieved 4 January 2014.
^ "Volleyball at the 1964 Tokyo Summer Games – Overview". Sports Reference. Archived from the original on 17 April 2020. Retrieved 4 January 2014.
^ "Badminton – History". Doha-2006.com (via Wayback Machine). Archived from the original on 4 January 2007. Retrieved 4 January 2014.
^ a b "III Asian Games". Pakistan Sports Board. Retrieved 8 January 2014.
^ Nakamura, Ken (26 April 2010). "Interview with Mikio Oda, first Japanese Olympic gold medallist". International Association of Athletics Federations. Retrieved 8 January 2014.
^ Rahman, Mansoor (5 August 1989). "Lofty ideals that shaped SEA Games – Member countries". New Straits Times. Kuala Lumpur. p. 6. Retrieved 3 January 2014.
^ "Events & Discoveries – Asian Games". Sports Illustrated. 8 (22). 2 June 1958. Retrieved 3 January 2014.
^ "A worldwide roundup of the sports information of the week". Sports Illustrated. 8 (23). 9 June 1958. Retrieved 3 January 2014.
Japanese Olympic Committee
Preceded byManila Asian Games Tokyo III Asiad (1958) Succeeded byJakarta
Medal table (summer
winter)
1951 New Delhi
1958 Tokyo
1962 Jakarta
1974 Tehran
1986 Seoul
1990 Beijing
1994 Hiroshima
2002 Busan
2010 Guangzhou
2014 Incheon
2018 Jakarta & Palembang
2022 Hangzhou
2026 Aichi & Nagoya
1986 Sapporo
1996 Harbin
1999 Kangwon
2003 Aomori
2007 Changchun
2011 Astana & Almaty
Far Eastern Championship Games
Afro-Asian Games
Asian Youth Games
Asian Para Games
Nations at the 1958 Asian Games in Tokyo, Japan
North Borneo
Republic of China
Events at the 1958 Asian Games (Tokyo)
1958 in Asian sport
1958 in Japanese sport
International sports competitions hosted by Japan
Asian Games by year
Sports competitions in Tokyo
Multi-sport events in Japan
1958 in multi-sport events
1950s in Tokyo
May 1958 sports events
June 1958 sports events


-Contact your local fire department, health department, or forestry office for information on fire laws.
-Make sure that fire vehicles can get to your home. Clearly mark all driveway entrances and display your name and address.
-Report hazardous conditions that could cause a wildfire.
-Teach children about fire safety. Keep matches out of their reach.
-Post fire emergency telephone numbers.
-Ensure adequate accessibility by large fire vehicles to your property.
-Plan several escape routes away from your home – by car and by foot.
-Talk to your neighbors about wildfire safety. Plan how the neighborhood could work together after a wildfire. Make a list of your neighbors' skills such as medical or technical. Consider how you could help neighbors who have special needs such as elderly or disabled persons. Make plans to take care of children who may be on their own if parents can't get home.
Design and landscape your home with wildfire safety in mind. Select materials and plants that can help contain fire rather than fuel it. Use fire-resistant or noncombustible materials on the roof and exterior structure of the dwelling, or treat wood or combustible material used in roofs, siding, decking, or trim with UL-approved fire-retardant chemicals. Plant fire-resistant shrubs and trees. For example, hardwood trees are less flammable than pine, evergreen, eucalyptus or fir trees.
-Rake leaves, dead limbs and twigs. Clear all flammable vegetation.
-Remove leaves and rubbish from under structures.
-Thin a 15-foot space between tree crowns, and remove limbs within 15 feet of the ground.
-Remove dead branches that extend over the roof.
-Prune tree branches and shrubs within 15 feet of a stovepipe or chimney outlet.
-Ask the power company to clear branches from powerlines.
-Remove vines from the walls of the home.
-Clear a 10-foot area around propane tanks and the barbecue. Place a screen over the grill – use nonflammable material with mesh no coarser than one-quarter inch.
-Regularly dispose of newspapers and rubbish at an approved site. Follow local burning regulations.
-Place stove, fireplace and grill ashes in a metal bucket, soak in water for 2 days; then bury the cold ashes in mineral soil.
-Store gasoline, oily rags and other flammable materials in approved safety cans. Place cans in a safe location away from the base of buildings.
-Stack firewood at least 100 feet away and uphill from your home. Clear combustible material within 20 feet. Use only UL-approved wood-burning devices.
-Review your homeowner's insurance policy and also prepare/update a list of your home's contents.
-Regularly clean roof and gutters.
-Use 1/8-inch mesh screen beneath porches, decks, floor areas, and the home itself. Also, screen openings to floors, roof and attic.
-Install a dual-sensor smoke alarm on each level of your home, especially near bedrooms; test monthly and change the batteries at least once each year.
-Teach each family member how to use a fire extinguisher (ABC type) and show them where it's kept.
-Keep handy household items that can be used as fire tools: a rake, axe, handsaw or chain saw, bucket and shovel.
-Keep a ladder that will reach the roof.
-Consider installing protective shutters or heavy fire-resistant drapes.
-Identify and maintain an adequate outside water source such as a small pond, cistern, well, swimming pool, or hydrant.
-Have a garden hose that is long enough to reach any area of the home and other structures on the property.
-Install freeze-proof exterior water outlets on at least two sides of the home and near other structures on the property. Install additional outlets at least 50 feet from the home.
-Consider obtaining a portable gasoline powered pump in case electrical power is cut off.
-Back your car into the garage or park it in an open space facing the direction of escape. Shut doors and roll up windows. Leave the key in the ignition. Close garage windows and doors, but leave them unlocked. Disconnect automatic garage door openers.
-Confine pets to one room. Make plans to care for your pets in case you must evacuate.
-Arrange temporary housing at a friend or relative's home outside the threatened area.
-Wear protective clothing – sturdy shoes, cotton or woolen clothing, long pants, a long-sleeved shirt, gloves, and a handkerchief to protect your face.
-Take your Disaster Supplies Kit.
-Tell someone when you left and where you are going.
-Choose a route away from fire hazards. Watch for changes in the speed and direction of fire and smoke.
-Close windows, vents, doors, blinds, or noncombustible window coverings and heavy drapes. Remove lightweight curtains.
-Shut off all utilities if possible, including bottled gas.
-Open fireplace damper. Close fireplace screens.
-Move flammable furniture into the center of the home away from windows and sliding glass doors.
-Turn on a light in each room to increase the visibility of your home in heavy smoke.
-Seal attic and ground vents with precut noncombustible coverings.
-Place combustible patio furniture inside.
-Set up a portable gasoline-powered pump.
-Place lawn sprinklers on the roof and near aboveground fuel tanks. Wetting the roof may help if it is shake-shingled.
-Wet or remove shrubs within 15 feet of the home.
-A three-day supply of water (one gallon per person per day) and food that won't spoil.
-One change of clothing and footwear per person and one blanket or sleeping bag per person.
-A first aid kit that includes your family's prescription medications.
-Emergency tools including a battery-powered radio, flashlight, and plenty of extra batteries.
-An extra set of car keys and a credit card, cash, or traveler's checks.
-Special items for infant, elderly, or disabled family members.
-An extra pair of eye-glasses.
-Keep important family documents in a waterproof container. Assemble a smaller version of your kit to keep in the trunk of your car.
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-Find out about the hazards in your community.
-Ask how you would be warned.
-Find out how to prepare for each type of disaster.
-Discuss the types of disasters that could occur.
-Explain how to prepare and respond to each type of disaster.
-Discuss where to go and what to bring if advised to evacuate.
-Practice what you have discussed.
1. A place a safe distance from your home in case of a home fire.
-Choose an out-of-state friend as a "check-in contact" for everyone to call.
-Post emergency telephone numbers by every phone.
-Show responsible family members how and when to shut off water, gas, and electricity at main switches.
-Contact your local fire department to learn about home fire hazards.
-Learn first aid and CPR. Contact your local American Red Cross chapter for information and training.


It's been raining constantly, back here in Ireland and right now I just want summer! At times, I never dress for the weather because I think If did in Ireland, I'll be wearing all black everyday and friends be worried lol!
Update: This week flew! Sadly, I have a confession... I couldn't go to the gym! But it's hard work this weekend! I wish I could just go to the gym in the mornings but if i was to do that, I'll be late for work and college! I've had so much opportunities to expand this blog but because I will be writing my thesis basically dissertation , well a 8000 word book. I have no time! sadly it will have to wait!


Brutal Energy High-Stim pre-workout is formulated with ingredients that provide mental and physical energy for any type of workout (aerobic or anaerobic). The Energy & Focus complex ingredients boost mental alertness and elevate mood to make pushing through a mentally tough session easy. Supporting this with Strength & Performance ingredients like creatine, beta alanine and betaine means you don't beat your body up into a state of over-training and allows progressive results from the hard work put in during the training session. B vitamins and BCAA's support metabolic energy producing functions in the body and provide the energy substrate for working muscles.
The focus is on using natural, safe ingredients, no narcotics in disguise.
CAFFEINE from natural green coffee extract, – reduces the perception of effort so your workout feels easier.
TeaCrine® – similar to caffeine but is slower to build a tolerance. Improves mental and physical energy while reducing the perception of fatigue. Acts to improve mood and motivation and provides some pain reduction during exercise. Delivers energy, mental clarity and improved motivation and mood, without increasing heart rate or blood pressure. Delivers energy and focus without the crash, jitters or habituation associated with caffeine.
TeaCrine® and caffeine are perfect compliments. Caffeine alone = 2 hours. Caffeine + TeaCrine = 4-6 hours. Together with caffeine, TeaCrine extends the feeling of energy. It provides a 'cleaner' energy without the crash or jitters, and improves focus and concentration for real results.
TeaCrine® is not habit forming nor does the body get used to it. The strength of the effect remains the same, even after 60 days of use.
N-acetyl-l-carnitine – Stimulates the mind and increases neural communication, providing better cognitive processes. Also associated with cell growth and recovery and muscle building.
L-dopa from Mucana Pruriens – promotes feeling good, enhances mood and improves motivation. Also associated with increased HGH levels and has antioxidant properties.
Beta Alanaine – improves the body's ability to resist physical fatigue. Delays fatigue and improves muscular strength and power through stabilising muscle pH. Improves both aerobic and anaerobic performance.
Betaine – aids endurance, boosts muscle mass and strength and may also improve body composition by lowering bodyfat. Also plays a role in relieving aches and pains which also helps improve ongoing physical performance.
Arginine – increase Nitric Oxide levels to improve blood flow to working muscles.
Krealkalyn – all the benefits of Krealkalyn – improve strength & muscular endurance through metabolic pH buffering.
B VITAMINS – folic acid, biotin, B1, B2, B3, B6, B12 – support the action of betaine as well as play a critical role in energy production including the metabolism of carbs, support the health of nerves and blood cells for optimal workout performance.
BCAA's – 2:1:1 – branched chain amino acids are used by muscles for energy during workouts – help support action of key ingredients by providing an energy substrate so as not to utilise the body's own muscle. Essentially providing 'muscle food' for the workout.


Investment Property Of The Week….
This property will be ideal for couples or families alike due to the fantastic location for town centre, both train stations and it's just 5 minutes walk from the OFSTED outstanding and oversubscribed Barnby Road Academy School. A great thing to bare in mind is that families with young children will aim to enroll their little ones at Barnby Road School meaning that they are likely to stay at the property until they leave when they're 11 years old.
In the last 3 years, 4 properties have been sold on this street ranging from £120,000 to £226,000 but only one was a terrace which sold for £120,00 in a similar condition to this property in December 2016.
The house has good sized rooms throughout with an upstairs bathroom and an additional shower room downstairs, the kitchen appears to require nothing but a good clean and the bathroom ceiling just needs a repaint along with a replacement shower as the tiles and suite don't appear to be that old. As for the rest of the house, certainly all the carpets need to be replaced and those rooms with wood flooring either need carpet laying or painting/varnishing as they all look tatty and worn. The bedrooms definitely need a lick of paint or a wallpapered feature wall or two for a bit of colour and the peeling ceiling in Bedroom 3 needs some TLC!
This week we are talking about this 2 bedroom terraced house on Lime Grove, Newark.
It is not very often a great renovation project like this is available in the centre of Newark.
Look at the house to the right and you can visualise what it could become.
The green paint must go.
The photos are quite fascinating, this house is seemingly preserved in a bygone era and you can imagine that is how the house has looked for many decades. A very basic kitchen with hob & sink, the furniture and simplicity of living.
Looking past that to bring it up to modern day living you could certainly put your own stamp on it.
The good news is that the bathroom is upstairs which can sometimes be a pitfall with these terraced properties. That will certainly save some money.
There is the potential to extend & possibly a few walls to knock through so there is definitely scope to add value which makes this property an ideal investment as a buy to let or to flip.
To say the garden (which is apparently planted with shrubs) looks overgrown is an understatement but I am sure that somewhere under there is a patio crying out for a table & chairs.
A 2 bed on the same street recently sold for £120,000 giving an indication of prices once renovated.
Once renovated you could expect this property to rent out for £500 per month giving a yield of 6%.


I want to get historic data of finished processes.
I am working with MS-SQL database (set db.properties).
I created the model via activiti-explorer, so the variables are defined as Form-properties.
I also dont get variables.
Have you tried it with the below request ?
Hi, The rest api command you wrote will not work when process has finished/Completed.
Thanks alot for trying to help !!


text:
Annual and quarterly reports of YMCA international work in China
Identifier: Y.USA.9-1-1
Kautz Family YMCA Archives
SCOPE AND CONTENTS OF THE COLLECTION
Annual and quarterly reports of North American YMCA foreign secretaries working in various cities in China between 1895 and 1949. This set of reports was collated from the set of bound Reports of Foreign Secretaries (for all countries) and from the records of YMCA International Work in China. In addition to documenting the successes and challenges of establishing the Young Men's Christian Association in China, the reports provide unique observations on Chinese society during the late Qing and Republican periods. The reports also document the YMCA movement's role in introducing and spreading Western philosophies of education, public health, and physical fitness.
Majority of material found within ( 1896-1925)
International Committee of YMCAs. World Service. (Organization)
Use of Materials:
This collection is protected by the Copyright Law of the United States (Title 17, U.S. Code). It is the user's responsibility to verify copyright, ownership, and to obtain all the necessary permissions prior to the reproduction, publication, or other use of any portion of these materials.
HISTORY OF YMCA INTERNATIONAL WORK IN CHINA
Although the YMCA movement had been active in China as early as the 1870s, the first North American work YMCA work in China dates from 1889, when Luther Wishard travelled there as part of his efforts to lay the groundwork for a major expansion of YMCA foreign work. He found four student YMCAs in existence and organized three more. Associations, chiefly for foreigners living in those cities, had also been organized in Shanghai and Hankou (Hankow). In 1895, the International Committee of the YMCA in North America sent the first American YMCA secretary, D. Willard Lyon, to China as a response to appeals from missionaries in Beijing (Peking), Shanghai, and Yantai (Chefoo). This was the beginning of fifty-five years of North American YMCA involvement in China. Over the years approximately 150 secretaries served in about forty associations throughout the country.
Lyon launched his work in Tianjin (Tientsin), rather than Beijing, as he had first intended, for there, so he said, was "the only city in China with a well-organized system of educational institutions for the teaching of Western subjects." As the future leaders of China, students were the focus of much the International Committee's attention. Following a tour of institutions of higher learning by Lyon and John R. Mott, then general secretary of the newly organized World's Student Christian Federation, twenty-two new student YMCAs were organized in China in 1896.
Part of the appeal of the YMCA was the International Committee's policy of stressing indigenous leadership, support, and control, which appealed to the burgeoning nationalism of the Chinese. However, the rapid growth of the YMCA in China initially required additional staff from the North American Association. Among the other early YMCA secretaries sent were Robert Ellsworth Lewis, Robert Reed Gailey, and Fletcher Sims Brockman. The Boxer Rebellion briefly halted the YMCA's activities in China, but recovery and advance followed rapidly. The General Committee of China, Korea, and Hong Kong was founded in 1901. The following year, headquarters were established in Shanghai. In 1912 the General Committee became the National Committee of the Young Men's Christian Association of China, with Brockman as the first national secretary (1901-1915). The peak of the International Committee's involvement came in the early 1920s, with 89 secretaries serving in China. By that time, there were 30 city associations with a membership of over 32,000, plus 170 student associations counting 14,200 members. Local boards of directors and the National Committee soon became predominantly and then exclusively Chinese. More and more, the responsible positions, both local and national, were filled by Chinese. In the position of National Secretary, Brockman was followed by C. T. Wang (1915-1916), David Yui (1916-1936), S. C. Leung (1926-1949), and Y. C. Tu.
While the YMCA's foreign work was rooted in the missionary movement and Bible classes were among the first activities offered by the fledgling association, the program included a variety of other educational programs, including English classes, lectures, and vocational training. Physical training, public health education (a national health campaign organized by the YMCA in 1920s virtually ended typhus in China), and other fields of work were soon added as the YMCA responded to local needs. The YMCA introduced many Western sports and Western-style sports competitions, and can also take credit for the early organization of the Olympic movement in China. Under the leadership of Max Exner, who became the first national physical director in 1908, as well as C. H. Robertson and educator Zhang Boling (Chang Poling), the YMCA organized the Far Eastern Games, the first international competitions in the far east.
After the revolution in 1949, the American YMCA continued to support Chinese YMCAs in Hong Kong and Taipei, Taiwan. Involvement by North Americans (or acknowledgement of the Y's Western connections) proved impossible under Communist rule. Nevertheless, a number of YMCAs on mainland China persisted. As of 1955, twenty-six continued to operate, the only Christian institution with a social program which had not been taken over by the government, but the YMCA in the United States had little direct contact with the YMCA in China during the middle decades of the century. In 1979, relations between the Chinese and American YMCA movements were renewed when Li Shao Pao, K. H. Ting, and Wen Han Zhou attended the World Council on Religion and Peace Conference in Princeton, New Jersey. Following friendly negotiations, funds held by the U. S. National Council of YMCAs for the YMCAs of China during World War II and following were returned in 1983. Subsequently, there have been continued delegations and visits by groups and individuals.
[Historical information adapted in part from Kenneth Scott Latourette, World Service: A History of the Foreign Work and World Service of The Young Men's Christian Associations of the United States and Canada, New York: Association Press, 1957. ]
Collected reports, primarily quarterly and annual, of North American YMCA foreign secretaries working in various cities in China.
ORGANIZATION/ARRANGEMENT OF THE RECORDS
Each report is listed along with the name of its author (the reporting foreign secretary), the title of the report, and the year it was issued. The locale (usually a city) reported on is also provided in both the older form used in the original reports and, in parentheses, the more modern Pinyin form of romanization. Lists of the reports with links to the digitized versions are provided in three arrangements:
Alphabetical by Author
Alphabetical by Location
These reports are also available in print in the form of a set of 19 published volumes: The Archives of the Young Men's Christian Assoication in China at the University of MInnesota Libraries: the Annual Reports, 1896-1949(Guangxi Normal University Press, 2011). In addition to facsimiles of the reports themselves, these volumes also include biographical sketches of the reporting secretaries, a brief history of Chinese YMCA city association buildings and conference centers, and various useful indexes.
Extensive additional reports, correspondence, and other related records can be found in Records of YMCA International Work in China (Y.USA.9-2-4), separately cataloged in the Kautz Family YMCA Archives
Collated from Reports of Foreign Secretaries (for all countries) and from the Records of YMCA International Work in China (Y.USA.9-2-4) and digitized by the University of Minnesota Libraries in 2007.
China Subject Source: Lcnaf
Church work -- China. Subject Source: Library of Congress Subject Headings
Education -- China. Subject Source: Library of Congress Subject Headings
Public health -- China. Subject Source: Library of Congress Subject Headings
Sports -- China. Subject Source: Library of Congress Subject Headings
Students -- China. Subject Source: Library of Congress Subject Headings
Young Men's Christian Associations of North America. International Committee
Young Men's Christian associations -- Administration Subject Source: Library of Congress Subject Headings
Young Men's Christian associations -- China Subject Source: Library of Congress Subject Headings
YMCA INTERNATIONAL WORK:
An Inventory of Annual and Quarterly Reports of Work in China
Finding aid prepared by Lara Friedman-Shedlov.
Contact The Kautz Family YMCA Archives Collecting Area
http://www.lib.umn.edu/ymca
ymcaarch@umn.edu
[Indicate the cited item and/or series here]. Annual and Quarterly Reports of YMCA International Work in China. Kautz Family YMCA Archives. University of Minnesota. See the Chicago Manual of Style for additional examples.
[Indicate the cited item and/or series here]. Annual and Quarterly Reports of YMCA International Work in China. Kautz Family YMCA Archives. University of Minnesota. See the Chicago Manual of Style for additional examples. https://archives.lib.umn.edu/repositories/7/resources/927 Accessed February 09, 2023.


text:
Ospreys v Viadana Verdict
By Paul Morgan, Rugby World Magazine
The vast majority of the 7,000 crowd expected to come along and see the Ospreys score four tries, win and take their tenth Heineken Cup point in seven days to go top of Pool 3…and the Ospreys didn't disappointed, delivering on all levels.]
It is true they were lacklustre at times, without intensity by the bonus-point try arrived in the 42nd minute, from Gareth Owen, so it was job done and over the business end of the competition, next month; away to Clermont Auvergne and home to Leicester.
Ospreys coach Scott Johnson said their objective after four rounds was to have their destiny in their own hands. And they have achieved that, heading Pool 3 by four points. Clermont and Leicester will beat Viadana in January, so realistically they need to win both games to win the pool.
A number of things stood out for me.
Tommy Bowe: The Ospreys should move hell and high water to make the Irishman sign a new contract, and not take up the offer from Leinster. He running and finishing against Viadana was exceptional, as was his strength with ball in hand. He could be the Ospreys' Ronaldo in January. Do what you need to, to keep him!
Dan Biggar: Two years ago former Ospreys coach Lyn Jones told me Biggar would one day play for Wales, and now at only 20 he seems to get better with every day. His goalkicking is Dan Carter-like, we knew that. But he is learning how to run a game, and one of the reasons Bowe is able to make his runs off his wing is the way Biggar reads the game. Bowe pinched man of the match from him today, but Biggar got my vote.
Andrew Bishop: Another exceptional talent – Wales, with Jonathan Davies of the Scarlets also a 12, look like they have an impressive reservoir of talent to take over from Gavin Henson.
Adam Jones: Wonderful to see the tighthead back on the field. I was in Pretoria to see his horrific injury on the Lions tour. Had he and Gethin Jenkins stayed on the field in that second Test I am sure they would have won.
But were you at the game. Who was your man of the match.
Do you think the Ospreys will come through their make-or-break January and qualify for the quarter-finals?