Tim Reinhold of the Insurance Institute for Business & Home Safety wasn't satisfied that the way we measure hurricanes truly matches up to their power, or danger. So he teamed with Mark Powell of the National Oceanic and Atmospheric Administration to create a new hurricane rating scale, the IKE (integrated kinetic energy), which could prove to be quicker than current scales for warning people and planning evacuations. Reinhold, who now holds a patent for the scale, tells PM how it works.
Why replace the old Saffir-Simpson scale with an entirely new one?
A number of us have been watching the big storms that have come through in the past 10 or more years, looking at both the surge and the wind levels. Then [we looked] at... popular expectations based on the Saffir-Simpson scale, and realized there was a real disconnect [with the] expanded Saffir-Simpson scale (originally it was just wind speed; they added storm surge in there as well).
Look at an event like Ivanwhich would be one that hit in the Pensacola area and had a huge amount of surgeor even Opal before that. When those storms hit, the winds werent terribly high, but they had a tremendous amount of surge with them. Then you come to Katrina, Rita and Ike. When you look at what the storm was at least at landfall, Katrina was a Category 3 from a wind standpoint, but the surge was easily Category 5.
There was a lot of pressure coming on the hurricane center even back after Ivan to have categorized it as a Category 4 because of the surge. [But] the highest winds we could find anywhere, and we had instruments throughout the whole area measuring stuff as the storm came inwere a small area of Category 2 type winds, and most of the area around Pensacola actually saw Category 1 winds.
Tell us how your scale, the IKE, works. Its a little like the way seismologists measure the energy released in an earthquake, right?
The magnitude scale from [earthquakes] is based on energy, so this is sort of an analog to that. Were looking at the energy in the storm. Here, what Mark [Powell] has done is take a slice of the storm at 10 meters high and 1 meter deep and calculate the energy within that plane. So when people are running the numerical models, they could calculate that. Hes come up with some other ways, based on the radius of tropical storm force and radius of hurricane-force winds, that [these measurements] can also be calculated. There are several different ways to at least get some general estimates of what those numbers are.
Could you explain what the SDP [surge destructive potential] means for a storm?
For a storm like Katrina youd be seeing more in terms of surge. When it was sitting out in the middle of the Gulf as a Category 5 heading for the coast, it was both surge and wind, then the wind started falling apart. But the surge had pretty much been set in motion by that time and the total amount of energy in the storm didnt really drop, although it got spread out over a much broader area and the peak winds dropped down.
So the idea was to try to come up with a different scale that would do a better job of capturing the potential for surge damage [and] the potential for wind damage in a separate kind of way.
Elaborate on the 0-to-5.99 scale that you use to rate hurricanes with IKE.
Its trying to give a continuous scale, so hurricanes could be a high 3, or low 4. In the Saffir-Simpson youre either a 3 or a 4. But this scale is like "Youre a 4.9 so youre almost to a 5." [Were] trying to give a little bit more differentiation and smoothness to it so that people have a better sense.
What would the scale translate to a storm like Katrina? What would they have been on the IKE scale versus the S-S scale?
Katrina, when it was out as a Category 5 in the middle of the Gulf, was a 5 in both scales, I believe. Then as it came into land, the total kinetic energy above tropical storm force kept it (from a surge standpoint according to the IKE scale) as a 5, [even as] the wind part of it began to drop down.
This all boils down to planning, then?
In the end what people need to focus on is feet of water and knowing what their elevation is. Because by that time you know where [the storm is] going to go, and people can run the models on the setup of the waves and all thats going into creating that surge, so youre going to have a much better estimate of what that surge is going to beand hopefully the extent of it.
I think the one advantage of the IKE scale is that it gives a little bit earlier warning: "Guys, this is a really big storm and it's got a lot of energy and wherever it comes in, it's going to create a lot of surge because its such a big storm." Or, "It's a small-footprint storm but very high-intensity winds, so wind is going to be the biggest issue."
How could it affect safety and evacuations?
Its trying to give people an earlier warning. Right now there are so many areas of our coast... where the storm could be on you before theres enough time for the people that should be evacuating to evacuate. And so its trying to put things on peoples radar so they dont get caught waiting too long, and they cant get out.
Whats next for your research?
Theres more... that still needs to be done to help with peoples perception of how [our system would rate] a Katrina or a Camille or an Andrew, so that they get a better feel for what these numbers really mean. And theres still [unknown] physics between where the storm is right now, where youre looking at these numbers, and what it is going to mean when it actually hits land. So I see it as an early warning.


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text:
\section{Introduction}
It has been proposed that the onset of the sudden cooling at the Younger Dryas boundary (YDB) of 12,800$\pm$150 years ago was due to a celestial encounter. This is supported by the presence of high concentrations, at the boundary, of platinum-rich dust at thirty sites throughout the northern hemisphere (Petaev et al. 2013; Moore et al. 2017), along with a wide northern hemisphere distribution of claimed impact proxies such as glassy microspherules (Bunch et al. 2012), nanodiamonds (Bement et al. 2014) and an estimated ${\sim}10^7$ tons of magnetic spherules argued to be of impact origin (Wittke et al. 2013). These proxies are often found in combination with major changes in fauna and flora indicative of sudden climate cooling (Kletetschka et al. 2018).

Evidence has also been presented that the largest biomass-burning event of the last 120,000 years, with perhaps 5-10\%  of the Earth's biomass being consumed in wildfires over a few days or weeks, occurred at the YDB (Wolbach et al. 2018). Many large animal species became extinct in the same geological instant; in North America up to 35 large animal genera in North America were extinguished almost simultaneously (Faith \& Surovell 2009); in Australia, the extinctions amounted to about 80\% of large species. The cause of these megafaunal extinctions, and their precise timing, have been disputed (Scott et al. 2017), as has the interpretation of the ground evidence in terms of a cosmic encounter: these arguments and references are summarised by Pino et al (2019). The northern hemisphere cooling took hold within a few years or less, the temperature drop being comparable with a return to glacial conditions, and persisted for $\sim$1300~yr.

Pino et al (2019) have extended the investigation of the YDB to a southern hemisphere site in Chile, 40$^\circ$S, and again find a major peak in charcoal abundance, with evidence of megafaunal extinctions synchronous with those in the northern hemisphere, and similar elemental peaks such as platinum, gold and high-temperature iron spherules, taken to be cosmic input proxies. The cosmic input, if real, thus seems to extend over at least hemispheric dimensions.

With currently adopted impact rates, there is an expectation of one near-Earth asteroid impact of energy ${\sim}200$~megatons over the last 20,000~yr, quite inadequate to produce the observed global trauma  (Bland \& Artemieva 2006). The impact of a 4~km comet so recently in the past, as had originally been proposed for the event (Firestone et al 2007), is \textit{a fortiori} improbable. A subglacial impact crater ${\sim}30$~km in diameter in north-west Greenland has been attributed to the impact of a 1.5~km iron asteroid some time during the Pleistocene (Kjaer et al. 2018). Its precise age is, however, unknown and so its relation to the Younger Dryas geology is at present uncertain.

There are several lines of evidence to indicate that a large (${\sim}100$~km) progenitor comet in a low inclination, short period orbit was at that time giving rise to Comet 2P/Encke and the Taurid meteors through a cascade of disintegrations (Clube \& Napier  1984).  Backtracking the meteor orbits, Steel \& Asher (1996) estimate the initial disintegration to have begun ${\sim}20,000$ years BP  --  although an earlier epoch cannot be discounted --  and it has been suggested that the Younger Dryas boundary phenomena might have been triggered by an encounter with some of the fragmented material (Napier 2010). The object of this paper is to model the disintegration of the progenitor comet in more detail, to see whether a plausible match can be made between the astronomical environment of that time and the terrestrial record; and hence, more generally, to discuss the role of such comets in past climate variations.

\section{Comet disintegration modes}
Di Sisto et al. (2009) showed that there is a poor match between the distribution of Jupiter family orbital elements expected dynamically, and that observed, and attributed the difference to the disintegration of comets through sublimation and splitting. They derived formulae for both processes and gave four `good match' models (Table\,1) capable of reconciling the dynamics and the observations.  These are statistical models for an ensemble of Jupiter family comets, but are taken below to apply to the progenitor of the Taurid meteor complex and Comet Encke. The fraction of mass lost in a splitting event is, according to di Sisto et al., given by
        \begin{equation}
        s = s_0/R
        \end{equation}
        \noindent $R$ the comet radius in units of 10~km.
        \medskip

        The probability of splitting per revolution is
        \begin{equation}
        f = f_0 (q/q_0)^{-\beta}
        \end{equation}
        \noindent with $q_0 = 0.5$\,au.
        \medskip

\begin{table}

\begin{tabular}{rrrr}
${\rm model}$         & $\beta$   &  $f_0$  &  $s_0$   \\ \hline
1                               &  1             &   1/4     &  0.01      \\
2                               &  1             &   1/3     & 0.007     \\
3                               &   0.5         &   1/6     & 0.01       \\
4                   &   0.5         &     1       & 0.001      \\ \hline
\end{tabular}

\caption{\small Comet fragmentation models from Di Sisto et al (2009).  The observations can be fitted by frequent splitting events $f$ with small mass loss $s$ per event (model 4), or fewer events with larger mass loss (model 1).}
\end{table}

\medskip

\begin{table}

\begin{tabular}{rrrr}
${\rm model}$ & final radius &   $N_f$     & $T$ \\ \hline
1                       &  16  &   670  &    5900         \\
2                       &  19  &   830  &  10000         \\
3                       &  18  &   650  &  20000         \\
4           &  16  &       0  &    ---      \\ \hline
\end{tabular}

\caption{Simulations of comet destruction, with sublimation and random splittings. The comets are in an Encke-like orbit with initial diameter 100~km and mass $4.7e20$~gm. The number of splittings yielding fragments of total mass $1e17$~gm  is recorded ($N_f$),  along with the time taken to evolve to the state where the fragment swarms have mass $\le 1e 17$~gm.}
\end{table}

\medskip

\begin{figure}
\noindent
\begin{minipage}[b]{\linewidth}
\includegraphics[angle=270,width=\linewidth]{mass.eps}
\end{minipage}
\noindent
\begin{minipage}[b]{\linewidth}
\includegraphics[angle=270,width=\linewidth]{msubl.eps}
\end{minipage}
\caption{Mass evolution of a 100 km comet in an Encke-like orbit. Models 3,1,2 top to bottom. Evolution is followed for 10,000 years. Mass lost by sublimation (bottom graph) is four orders of magnitude less than that lost by splitting (top graph).}

\end{figure}

\begin{figure}
   \includegraphics[angle=270,width=\linewidth]{radius.eps}
\caption{Radius evolution for models 1--3.}
\end{figure}

\begin{figure}
   \includegraphics[angle=270,width=\linewidth]{mfrag.eps}
\caption{Mass of material ejected at each splitting event, following the evolution of the 100 km comet.}
\end{figure}

Figures 1 and  2 show, respectively, the evolution of mass and radius of a 100~km comet in an Encke-like orbit ($q=0.34$~au), simulated by way of the parameters given in models 1 to 3.  The splittings took place randomly, in accord with the probabilities given by eqn (2), over a period of 10,000 years.  Splittings with mass loss ${\ge}10^{17}$\,gm took place 779, 939 and 611 times for models one, two and three respectively. These occur anywhere along its orbit but may tend to concentrate around perihelion (Boehnhardt 2004). Splitting is seen to be the dominant process of comet disintegration, with mass loss by sublimation four orders of magnitude down (Fig.~1). As comet disintegration proceeds and its mass dwindles,  the mass of fragments split off likewise declines (Fig.~3). Model 4, with very frequent low mass splittings, produced no fragment swarms with mass $>10^{17}$\,gm.

\section{Ejection and spread of fragments}
\begin{table}
\centering

\begin{tabular}{rrrrr}
${\rm model}$ & $D_0$ & $L_{rev}$ &  $L_{yr}$ &   $N_f$     \\ \hline
1                       &    150  &  5560     &   18350     &    1474      \\
1                       &    100  &  3700     &   12230     &     776      \\
1                       &     50  &  1850      &    6090     &      84      \\
1                          &     20  &   700        &    2300     &       0       \\  \hline
2                       &    150  &  6050     &   20000     & 1924     \\
2                       &    100  &  4030     &   13285     &  943      \\
2                       &     50  &  2025      &    6675     &    0     \\
2                       &     20  &   740        &    2450     &    0     \\ \hline
3                       &    150  & 6050      &   20000     & 1257     \\
3                       &    100  & 6050      &   20000     &  734      \\
3                       &     50  & 6050       &   20000     &   83     \\
3                       &     20  & 1160       &    3830     &    0     \\ \hline
\end{tabular}
\caption{The physical evolution of a comet in an Encke-like orbit with initial diameter $D_0$ km. The number of splittings yielding fragment clusters of mass $>10^{17}$~gm  is recorded ($N_f$),  along with the lifetime of the progenitor. These are measured in revolutions $L_{rev}$ or years respectively $L_{yr}$ and are taken to last until the diameter of the comet declines to $<$1~km.}
\end{table}

\medskip

I carried out simulations in which comets of various sizes in an Encke-like orbit underwent sublimation and random splittings in accord with the di Sisto et al. models, following the evolution for 20,000 years. Table~2 shows the lifetimes and numbers of splittings with masses in excess of $10^{17}$~gm.  The lifetime of a comet was measured by the time taken to decline to a $<$1~km object. All the models, except 4, predict something like 750-1500 splitting events yielding fragment clusters each of mass $>10^{17}$~gm, over timescales of order 6000 - 20,000 years (Table~3).  At an encounter speed of  $\rm {\sim}30\,km\, s^{-1}$, 10$^{17}$~gm of debris carries $10^7$ megatons of impact energy.

\section{Encounters with fragment swarms}
For the sake of illustration assume that the orbital elements adopted for the Taurid progenitor are those for the current Comet Encke:
$a$ = 2.214 au, $e$ = 0.84834, $i$ = $11.783^\circ$. From
\begin{equation}
r = \frac{a(1-e^2)}{1+e\cos \phi}
\end{equation}

\noindent With $r=1$~au, encounters with the Earth are possible when the true anomaly $\phi = 116.56^\circ$ or $243.44^\circ$. These intersections occur $(42.3+ nP)$ and $(1160.9+nP)$ days after perihelion, on the outward and inbound legs of the orbit respectively, $n$ the number of complete revolutions and $P{\sim}$1203 days the orbital period. The encounter speed is $\rm {\sim}30~km\, s^{-1}$. The probability of an encounter, and the energetics, are functions of the time of splitting, the ejection speed of the fragments, their total mass, and the epoch of the encounter.

\begin{figure}
   \includegraphics[angle=0,width=\linewidth]{figlo.eps}
\caption{Evolution of trail length over ten orbital periods (33~yr), for a $\rm 2\,m\,s^{-1}$ maximum dispersion of fragments. The peak lengths occur at perihelion passages, superimposed on a secular increase in trail length. Passages at 1~au are marked by dots. Inbound and outbound adjacent trail lengths are approximately equal.}
\end{figure}

\begin{figure}
   \includegraphics[angle=0,width=\linewidth]{hits.eps}
\caption{Evolution of trail lengths over ten orbital periods (33~yr), for maximum dispersion speeds 10, 5 and 2 $\rm m\,s^{-1}$ (top to bottom). Passages at 1~au are again marked by dots.}
\end{figure}

\begin{figure}
   \includegraphics[angle=0,width=\linewidth]{megatons.eps}
\caption{Kinetic energy of encounters with a debris trail of mass $10^{17}$\,gm for 10 comet revolutions (${\sim}33$~yr). The trail disperses at 2, 5 and 10 $\rm \,m\,s^{-1}$ respectively, top to bottom.}
\end{figure}

Simulations were carried out in which the fragments from a breakup were dispersed isotropically with random dispersion speeds up to a maximum $\Delta v\rm \,m\,s^{-1}$.  Estimates of the ejection velocities of meteoroids from comets are generally in the range $\rm 0-50 \,m\,s^{-1}$, although IRAS observations of cometary dust trails yield values less than $\rm \pm 5 \,m\,s^{-1}$ (Sykes \& Walker 1992, Kres\'{a}k 1993). Boehnhardt (2004) finds that, for short period comets, a mean of 16 cometary fragments is generated during a spitting event, with separation velocities  $\rm 2.7\pm2.3\,m\,s^{-1}$. Fig.~4 illustrates the evolution of length of a debris trail over ten orbits. This was formed by a splitting at $\phi=135^\circ$, 80 days after perihelion passage t, with $\rm \Delta v =  2\,m\,s^{-1}$ debris. The trail stretches and shrinks as it passes through perihelion and aphelion respectively, but superimposed on this is a secular lengthening at a rate of $\rm {\sim} 43\,m\,s^{-1}$. The rate of lengthening of the trail is directly proportional to the initial breakup speed of the fragments, but was found to be not strongly dependent on the true anomaly at which fragmentation occurred, apart from those taking place within a few days of perihelion. Fig.~5 illustrates the evolution of trail lengths at 1~au for several dispersion speeds.  The trail is 1\,au from the Sun 42.3 days before or after its perihelion passages.

 Table~3 reveals that the number of trails created is in the hundreds over the physical lifetime of the comet. As material in a trail disperses along the comet orbit, the probability of a terrestrial encounter with it increases but its incident kinetic energy, in the event of an encounter, declines. This is illustrated in Table~4, which gives encounter frequencies and energies for a swarm of fragments with mass $10^{17}$~g and maximum dispersion velocity $\rm \Delta v = 2 \,m\,s^{-1}$ as it spreads along the orbit. $L$ is the length of the swarm, which travels through the node at 1~au at a speed $\rm V{\sim}23~ km\,s^{-1}$. For the dispersions considered, the vertical dispersion of the material is less than $R_\oplus$ and the mass $M_{enc}$ intercepted by the Earth is $2R_\oplus/L/\cos\chi$, $\chi{\sim}64.4^\circ$ the angle at which the Earth intercepts the swarm.  The first 15 passages at 1~au would yield, in the event of an encounter with Earth, a mass influx with kinetic energy in excess of 3000 megatons (1~Mt${\sim} 4.2 \times 10^{22}$~ergs). Fig.~6 illustrates the impact energies for the first ten potential encounters following splitting events in which the fragments initially disperse at  2, 5 and 10~$\rm m\,s^{-1}$.
\begin{table}
\centering
\begin{tabular}{rrrrrr}
    yr &   $L$   & $D$ &  $\nu$ & $M_e$ &   $E$   \\ \hline
   3.3 &   732   & 2.4  & 0.002  & 40.3   & 42.8  \\
    6.6 &   1372 & 4.4  & 0.004 & 21.5   & 22.8  \\
   9.9 &   2012 & 6.5  &  0.005 & 14.7   & 15.6  \\
   13.2 &   2652 & 8.5  & 0.007 & 11.1   & 11.9  \\
   16.5 &   3292 &10.6 & 0.009 & 9.0   & 9.1  \\
   19.8 &   3932 &12.7 & 0.011 & 7.5   & 8.0  \\
   23.1 &   4572 &14.7 &  0.012 & 6.5   & 6.9  \\
    26.4 &   5212 &16.8 & 0.014 & 5.7   & 6.0  \\
   29.6 &   5852 &18.8 &  0.016 & 5.0  & 5.8  \\
  32.9 &   6492 &20.9 &  0.017 & 4.5   &  4.8  \\
  36.2 &   7132 &23.0 &  0.019 & 4.1   &  4.4  \\
  39.5 &   7772 &25.0 &  0.021 & 3.8   &  4.0  \\
  42.8 &   8412 &27.1 &  0.023 & 3.5   &   3.9 \\
  46.1 &   9052 &29.1 &  0.024 & 3.3   &  3.5  \\
  49.4 &   9692 &31.2 &  0.026 & 3.0   &  3.3 \\ \hline
\end{tabular}
\caption{Encounters with a single debris swarm  of mass $10^{17}$~g created at true anomaly $135^\circ$, 80 days after perihelion passage. The fragments have initial random speeds and directions relative to the comet nucleus, uniformly distributed with maximum initial dispersion speed of $\rm 2 \,m\,s^{-1}$. The trail length $L$ is in units of $R_\oplus$, the duration $D$ of crossing the Earth's orbit is in days, and the encounter probability is $\nu$. The cumulative probability of an encounter with this swarm is ${\sim}0.2$. The mass $M_e$ intercepted is in units of $10^{13}$~g, and the kinetic energy $E$ of the incident material is in units of $10^3$ megatons.}
\label{tab:enc}
\end{table}

When the orbits of comet and Earth intersect, a fragment swarm of length $L$ will cross the Earth's orbit with duration of passage $D = L/V_o$ days, being a fraction $D/P$ of its orbital period.  The probability $\nu$ of a terrestrial encounter during such a passage is
\begin{equation}
\nu = L/(V_oP) {\sim}2.68\times 10^{-6} L
\end{equation}
\noindent where $\rm V_o{\sim}23~ km\,s^{-1}{\sim}310.5\,R_\oplus/day$. Table~4 illustrates the encounter probabilities per passage of a $10^{17}$\,g swarm of fragments with initial random dispersion speeds of up to $\rm 2 \,m\,s^{-1}$. The weighted mean length of the swarm over 50~yr is ${\sim}6680\,R_\oplus$ and the cumulative probability that the Earth will encounter it while $E>6000$\,Mt is $p{\sim}$0.2.

The mean mass $M_e$ intercepted by the Earth during passage through this swarm was determined by following the evolution of 50,000 particles representing it, and counting the numbers intercepted by the Earth during each of 100 random passages through it. The encounter energy lay in the range 6000-50,000 megatons over a 50~yr period following the splitting. During this time another 8-16 or so splittings may take place ($f_0$ of Table~1), adding to the density of the expanding trail and hence the encounter energy. If nodal crossings occur 10 times in the course of a 15,000~yr disintegration history, consistently with the precession period of Comet Encke, then there is only a 10\% chance, $(1-p)^{10}$, of avoiding an encounter with mean impact energy $<E>\sim 6000$\,Mt.

The probability of a damaging encounter can also be roughly estimated by scaling up from the single-body collision probability (e.g. Kessler 1981, Rickman et al. 2014). Taking the interval between collisions with a body like Comet Encke as $5\times 10^8$~yr,
then the interval $\Delta t$ in years between encounters with a fragment swarm is of order
\begin{equation}
\Delta t = \frac{5\times 10^8}{A} \times \frac{l_c}{l_f} \times \frac{1}{N}
\end{equation}
\noindent where $A$ is the face-on area of the swarm in units of the cross-section of the Earth, $l_c$ is the active lifetime of the comet, $l_f$ is the effective lifetime of the swarm as a significant hazard, and $N$ is the number of such fragments generated over the active lifetime of the comet. We have $A = L \cos\chi\times 2\delta z$. Here $\delta z$ is either the out-of-plane dispersion of the fragments, determined by a least-squares fit to the computed trail, or the radius of the Earth, whichever is larger (generally the latter for modest dispersion speeds). Taking, from Table~4, a characteristic $L=6700\,R_\oplus$,  $l_c = 10^4$\,yr, $l_f = 50$\,yr and $N = 10^3$,  eqn (5) yields an interval  $\Delta t {\sim} 17,000$~yr between encounters of at least 6500 Mt energy, and 3,800~yr between encounters of at least 5000\,Mt energy.  There is thus good agreement between the encounter rates obtained from eqns (4) and (5). Orbital precession is significant over the millennia during which the comet is fragmenting, and second or third generation comets may themselves form individual branches, but this does not affect the overall encounter probabilities as estimated above.

Both planetary perturbations and solar radiation pressure will act to disperse a meteor stream. The simulations here apply to fragments larger than the micron-sized dust particles associated with tails. Spitzer observations of the fragments associated with the breakup of Comet 73P/Schwassmann-Wachmann 3 appear to show that their mass is dominated by particles 0.1~mm size upwards (Vaubillon \& Reach 2010), which are less subject to Poynting-Robertson drag over the timescales considered here (Williams 2002). Comet Encke lies outside the Jovian sphere of influence, and Jupiter's differential influence on a fragment swarm over say a dozen revolutions may also be neglected for the present purpose.

\section{Multiple impacts and climate transitions}
The disintegration history of comets is varied and has been extensively discussed (e.g. Boehnhardt 2004; Fernandez 2009). Comets may split into a few fragments, or produce many small pieces, or disintegrate altogether, but cascading fragmentation is probably the prime disintegration process, and the existence of many meteoroid substreams within the Taurid complex indicates that the progenitor comet took this route. Unseen remnants (dormant comets) may be a major source of meteor showers (Jenniskens 2008). At least 19 of the brightest high-eccentricity near-Earth asteroids have been statistically linked to the Taurid complex (Napier 2010), along with others (Spurny et al. 2017; Porub\u{c}an et al. 2004). Swarm material will be in the form of dust, boulders and probably larger bodies, and the duration of encounters will range from a few hours to a day or two. As the cluster decays from a handful of bodies to a meteor stream, intermediate stages are likely to involve increasing numbers of smaller bolides. The spectra and breakup heights of Taurid meteors show a variety of compositions and strengths, consistent with a heterogeneous composition of the primary body (Matlovi\u{c} et al. 2017; Tubiana et al. 2015), and it is likely that larger fragments will yield Tunguska-like airbursts. If we consider that a wildfire could be initiated by a one megaton bolide impacting on suitable material, and half the mass of say a 10000 megaton encounter (Table~\ref{tab:enc}) was in the form of such bolides, then a global wildfire would likely be initiated.

Studies of Earth history of the last 150,000 years have revealed that the climate is subject to sudden temperature changes, with transitions often taking place within decades or even a few years (Flohn 1979; Adams et al 1999; Steffensen et al 2008), and persisting for a few centuries up to a millennium or so. These changes are superimposed on the longer climatic cycles probably caused by orbital and polar precessions (Rial 1999). The onset of the Younger Dryas cooling was one such event. It was abrupt in onset and intense, amounting to 2 to 6$^\circ$ in the Northern hemisphere, and was accompanied by a sudden transition in European vegetation from temperate to Scandinavian. In modern times, a sudden global cooling of this amplitude would have a calamitous effect on agriculture (Engvild 2003).

The abrupt collapse of the Akkadian and other civilisations around 4170 BP has been attributed to a shift to more arid conditions, drought driving subsequent societal and political collapse (Cullen et al. 2000). The onset of the aridity has been attributed to a cooling of the North Atlantic. Several hypotheses have been proposed to explain such abrupt coolings and there are likely to be multiple causes given the complexity of internal mechanisms. Courty et al. (2007), on the basis of paleosoil evidence, have proposed that the Akkadian collapse was due to a cosmic disturbance (cf Coqueueniot \& Courty 2012). We discuss here the possibility that the sudden and extreme coolings recorded over the Quaternary may have arisen from comet dust sprinkling the upper atmosphere and reducing sunlight incident on the Earth's surface (Clube \& Napier 1984; Asher et al. 1994; Clube et al. 1996; Napier 2001).

The hypothesis that cosmic dusting might be responsible for ice ages has a long history. Passage through molecular clouds has been proposed as the cause of ice epochs or snowball glaciations (McCrea 1975, 1981; Begelman \& Rees 1977; Yabushita \& Allen 1985, 1989; Pavlov et al 2005; Kataoka et al. 2014). Hoyle \& Wickramasinghe (1978) raised the possibility that ecological catastrophes such as ice ages and the Cretaceous-Tertiary extinctions may have been caused by passages close to the nucleus of a comet. The proposed timescales for these events are geological. However, with the finding that large Centaurs leak into the near-Earth environment at a geologically rapid rate (Galiazzo et al. 2019, Napier 2015, Horner et al. 2014), it now appears that such bodies are likely to be suppliers of cosmic dust on much shorter timescales, extending into the Quaternary and even historical times.

A 100~km comet with density $\rm 0.4~g\,cm^{-3}$, comprising 50\% dust, releases $10^{14}$~tons of dust over the course of its disintegration, largely through the intermediary of hierarchic fragmentation. The debris encountered during these passages will generally be a mixture of dust and larger fragments. From Table~4 and the associated discussion it appears that the Earth may intercept $10^{7}$~tons of dust and boulders over a few hours during such an encounter, as against 30-50 tons of normal daily background flux. Much of this meteoric input will ablate to smoke in the mesophere, i.e. micron-sized particles (Klekociuk et al. 2005). Particles with mass $\ltsimeq 10^{-12}$g will not become hot enough to ablate. An organic grain of diameter $1 \mu$ and density $2 \rm g\,cm^{-3}$ has a mass $10^{-14}$~g yielding, for a uniform distribution of dust over the Earth's atmosphere, a square centimetre column of $2\times 10^8$ particles. For spherical particles, the intensity of sunlight reaching the ground is then reduced by a factor $\exp (-\tau)$ with  optical depth $\tau{\sim}1.6Q_{ext}$ for vertical incidence of sunlight. $Q_{ext}\sim$2 for particles $\gtsimeq 1~\mu$ in diameter leading to a diminution of sunlight at ground level by factor of $\sim$25.  The carbon content of cometary dust has been measured in Comets 1P/Halley and 67P/Churyumov-Gerasimenko, and has been found to be high (e.g. Jessberger et al. 1988 for 1P and Bardyn et al. 2017 for 67P). Thus the dust particles of Comet 67P are made of 50 percent organic carbon by mass, presumably reflecting the composition of pristine solar system material. Organic carbon spheres have a high scattering efficiency, ${\sim}1.5$, and low absorption efficiency, ${\sim}0.05$, diminishing sunlight by a factor of 10. The creation of such meteoric smoke in the mesosphere at the concentrations considered here would effectively turn the Earth white in visible light, while allowing infrared radiation to escape from the surface (Hoyle \& Wickramasinghe 1978), during the months or years of settling. Coagulation of aerosols would, however, change the shape and size of the particles, and introduce porosity, all of which would alter their absorption and scattering properties. The extent to which charged aerosols would coalesce is uncertain: in noctilucent cloud conditions, in situ rocket observations have revealed both larger and smaller particle radii (L\"{u}bken \& Rapp 1981). The settling time of spherical micron-sized particles is about 3 to 5 years, depending on factors such as latitude and season. The overall climatic effects are likely to be complex (Renssen et al 2015) and to involve an altered atmospheric circulation, and the blocking of sunlight by the soot generated from the intense wildfire activity at the YDB, which yields an essentially infinite optical depth during its residence time of days to weeks in the lower atmosphere (Wolbach et al. 2018).

The injection of ${\sim}10$ million tons of carbon-rich aerosols and water vapour into the mesosphere over a few hours (Table 4), as against the current background flux of ${\sim}50$ tons/day, is likely to lead to noctilucent clouds, an increased planetary albedo, and significant cooling. One would expect the climate (but not necessarily the biosphere) to recover within a decade (Robock et al. 2009) unless the cooling triggers a climate instability such as that proposed by Hoyle (1982).

\section{Conclusions}
I have modelled the disintegration of a large comet in a short-period orbit, using Comet Encke as an archetype, and find that there is a reasonable expectation of one or more brief meteor `hurricanes', with intensities far beyond modern experience, in the course of disintegration of the progenitor. Enough meteoric smoke may be created during such encounters to generate sudden coolings of some years' duration, along with widespread wildfires. The terrestrial upsets at the onset of the Younger Dryas boundary of 12,900 BP, and  the simultaneous collapse of early civilisations around 2350 BC, may have been triggered by events of this character.

\section{Acknowledgements}
I thank David Asher for discussions on this topic.

redpajama_set_name: RedPajamaArXiv


text:
Five Indonesian fishermen kidnapped by Philippine militants
Gulf Times - al-Kaabi
Al-Kaabi meets with Japanese trade minister
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi met in Doha on Wednesday with Hideki Makihara, Japan's State Minister of Economy, Trade and Industry.
12/17/2019 7:47:33 PM20
Al-Kaabi urges QP employees to apply 'newly learnt knowledge and skills' in workplace
Qatar Petroleum honoured more than 450 "frontline leaders" who have completed an 18-month specialised leadership programme, the second of which it has organised for its senior employees.
Al-Kaabi meets Salvador president
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi on Thursday met with Nayib Armando Bukele Ortz, the President of El Salvador, who is currently on a visit to Qatar.
Al-Kaabi calls upon GECF nations to develop natural gas resources, expand trade routes
HE the Minister of State for Energy Affairs welcomes the GECF Heads of State to 6th Gas Summit in Doha in 2021
Al-Kaabi meets with Equatorial Guinea minister of mines and hydrocarbons
HE Minister of State for Energy Affairs Saad bin Sherida al-Kaabi on Thursday met with Gabriel Mbaga Obiang Lima, the Minister of Mines and Hydrocarbons of Equatorial Guinea.
Al-Kaabi meets with senior Chinese energy official
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi met with Zhang Jianhua, director of China's National Energy Administration in Beijing on Tuesday.
Al-Kaabi meets with South Korean energy minister, top executives
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi held talks in Seoul on Monday with Sung Yun-Mo, South Korea's Minister of Trade, Industry and Energy.
Al-Kaabi meets with Philippines Secretary of Energy
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi met in Doha with the visiting Philippines Secretary of Energy Alfonso Gaba Cusi and the accompanying delegation ...
Al-Kaabi meets Pakistan minister for power and petroleum
HE the Minister of State for Energy Affairs Saad bin Sherida al-Kaabi met in Doha on Monday with Omar Ayub Khan, Pakistan's Federal Minister for Power and Petroleum.
Muntajat plays 'prominent' role in Qatar's energy sector development: al-Kaabi
HE the Minister of State for Energy Affairs, Saad bin Sherida al-Kaabi, also the President and CEO of Qatar Petroleum, has acknowledged the prominent role Muntajat plays in the development of Qatar's energy sector.
Al-Kaabi discusses energy ties with Hungarian Minister
HE Saad bin Sherida al-Kaabi, Minister of State for Energy Affairs, met in Doha with Peter Szijjarto, Minister of Foreign Affairs and Trade of Hungary, who is currently on an official visit to Qatar.
Qatar to host sixth Gas Summit of GECF in 2021, says al-Kaabi
Qatar will host the sixth Gas Summit of the Gas Exporting Countries Forum (GECF) in 2021, offering an opportunity for dialogue at the highest levels on the latest developments and trends ...

redpajama_set_name: RedPajamaCommonCrawl


African Safaris Adventures offers you with fantastic luxury beach gateways both in Kenya and Zanzibar. East Africa boasts of long coastline with unspoiled pristine white sandy beaches where you will enjoy your holidays sun bathing and swimming in warm Indian Ocean waters.
Stay in the beach hotels, lodges or cottages while enjoying the pristine sandy beaches lined with magnificent palms and wonderful ocean life. Kenya's coast is famed as one of the best in the world. You can stay in Kenya's South coast home to Diani Beach, Chale Island and Shimoni. Great water sports here include fishing expeditions, deep sea diving, sport fishing, snorkeling, scuba diving and swimming with dolphins.
Visitors to Kenya's coast have the opportunity to visit or stay in Mombasa Island. A haven for traditional Arabic and Portuguese history. Visit the fort Jesus fortress and the old town rich with antique Arabic architecture and vibrant with Afro-Arabic Swahili culture. Feel the nostalgia of walking the narrow paths and passages. While there, our visitors can visit Tudor creek, Have dinner under the stars, visit the old harbor and the port.
Kenya's North Coast is the longest stretch of beach and is vibrant. Lined with world class lodges and resorts as well as hotels, open beaches, water sports, international class nightclubs abd discotheques for all the fun. The north coast features Mtwapa Creek and Mtwapa town a few minutes from Mombasa Island, Kikambala, Kilifi, Watamu, Malindi and Lamu to the North most end.
At the northern tip of the island is Nungwi, approached by a road lined by banana palms, mangroves and coconut trees. This is the dhow building capital of Zanzibar island, so it is a good place to see traditional craftsmen at work. Zanzibar also boasts several small offshore islands which are ideal for a day-trip.
Prison (or Changu) island is the most popular with tourists because it is only a short trip from Stone Town. Originally, it was used by Arabs to detain recalcitrant slaves, and then a jail was built by the British, but it was never actually used. Visitors to Zanzibar will notice a large population of ancient Aldabra tortoises. Other islets near to Stone Town are Chapwani, Chumbe and Bawe.


text:
Gigantic Fountain Of Cold Molecular Gas Pumped By A Black Hole – Observed By ALMA
MessageToEagle.com | November 12, 2018 | Astronomy | No Comments
MessageToEagle.com – Using the Atacama Large Millimetre/submillimetre Array (ALMA) of telescopes, the team, which includes researchers from Cardiff University, has observed a supermassive black hole acting like a 'monumental fountain' in the middle of a galaxy over a billion light-years from Earth.
"Galaxy evolution can be pretty chaotic, and big galaxies like this tend to live hard and die young. For the first time we have been able to observe the full cycle of a supermassive black hole fountain, that acts to regulate this process, prolonging the life of galaxies,"Dr Timothy Davis, from the School of Physics and Astronomy at Cardiff University, said in a press release.
NRAO/AUI/NSF; D. Berry
At the center of the galaxy, named Abell 2597, the black hole is drawing in vast stores of cold molecular gas and then spraying them back out again in an ongoing cycle.
The giant elliptical galaxy Abell 2597 lies at the heart of one of the universe's most massive structures and has a sprawling cluster of other galaxies surrounding it.
According to the researchers, this entire system operates via a self-regulating feedback loop. The incoming material provides power for the fountain as it "drains" toward the central black hole, like water entering the pump of a fountain. This gas then causes the black hole to ignite with activity, launching high-velocity jets of super-heated material that shoot out of the galaxy.
As it travels, this material pushes out clumps and streamers of gas into the galaxy's expansive halo, where it eventually rains back in on the black hole, triggering the entire process anew.
By studying the location and motion of molecules of carbon monoxide (CO) with ALMA, which shine brightly in millimetre-wavelength light, the researchers were able to measure the motion of the gas as it falls in toward the black hole.
It is from these plumes of gas that new stars are formed in galaxies, and the researchers believe that the process they have observed could be common across the Universe and, more importantly, could be crucial to the development of massive galaxies like this one.
MessageToEagle.com
Tags:ALMA, galaxy Abell 2597
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Good quality data enables the utility to understand network and asset behavior, operating conditions, and their impact on customer service. Electric networks change routinely, and operations reflect a dynamic condition. Therefore, quality data must be regularly assessed based on its context of use. The utility network must enable accurate measurements of network behavior to assure accurate observations and the ability to optimize measures in response to current and accurate data. The ability to assure correct inputs from system and operations data enables the utility to substantially improve the quality and cost efficiency of its operations.
Furthermore, the outlook of network operators to data sharing must shift from "need to know" basis to a presumption of disclosure. There should be more of data-sharing between gas and electricity networks.
Cyient's Intelligent Data Management Solution (iDMS) has been customized to seamlessly monitor, identify, and rectify input data quality through configurable machine learning validation routines with no impact on CAPEX. For further information, visit Cyient.


If you've been searching for the best wireless laser printer to fulfill your specific requirements, you've found what you've been looking for. In this review, you will find listed the best wireless color laserjet printers that can be utilized without the need to make connections with wires to your gadgets. This makes these type of printers excellent choices if you have the need to print from your tablets or smartphones.
Furthermore, the best color wireless printers are deeply versatile, as they can easily be installed just about anywhere in your office or home. You also won't need to worry about trailing cables and wires across the building. Basically, all you'd really require for proper functioning is just a robust wireless network and a power outlet or socket. The best contemporary wireless laser printers are also capable of printing directly from various mobile gadgets such as smartphones, tablets, and laptops. Which means they are certainly better suited to contemporary needs, as a lot of people make use of these mobile gadgets for daily tasks. So, read on and find out the best wireless printers for your specific needs.
The HP LaserJet Pro CE914A CP1025nw printer offers you the ability to print wirelessly from anywhere and easily share the resources through its built-in Ethernet. This wireless laser printer is manufactured with a 4 ppm (print per minute) print speed in color. Asides from this it also offers you the ability to print in black and white at a print speed of 17 ppm.
This is an amazing printer that possesses various multi-functionalities allowing you to print with USB, PC, Mac, 802.11b/g/n Wireless and Ethernet. It allows paper sizes that start from 3 in by 5 into 8,5 in by 14 in. The LaserJet HP Pro Color CE914A also comes with a paper tray with a 250 sheet capacity, hence you can expect approximately 15,000 copies monthly.
Its print per minute speed is quite low if you require a lot of prints per hour or daily.
This printer features a 28 print per minute.
This is one of the best wireless laser printers due to its fast speed. With amazing print speeds getting up to 28 prints per minutes and the initial page being outputted in approximately 8.9 seconds, you can comfortably expect to have a page monthly volume ranging from 750 to 3500 pages.
The LaserJet Color HP Pro M477fdw also offers a powerful scan resolution of 1200 dpi as well as featuring a multi-purpose 50 and 250 sheet Automatic Document Feeder, ADF trays.
Wireless connectivity range isn't so broad.
HLL8350CDW Brother Color Laser Wireless Printer is known for its mix of reliability, efficiency, and speed. It utilizes a print resolution of 600 by 2400 dpi as well as speeds getting up to 32 page per minute. Its automatic duplex provides for double-sided printing.
You can install the printer easily through the Internet or USB and comes with tray capable of holding 250 sheets. However, it does not have a preset mode for photo printing on certain sizes of paper.
This printer does not offer a preset mode for photo printing on certain paper sizes.
This printer the HP LaserJet Pro M252dw is an amazing wireless color LaserJet printer due to its 800 MHz processor and 150 sheet paper capacity. It is very compatible with multiple printing languages such as PDF, HP PCL, 5th, HP PCL 6, PCLm, Native Office, URF, level 3 HP postscript emulation.
It has the ability to print up to 19 pages per minute offering you a monthly page volume of 2500 pages or less. The printer is also compatible with different page sizes and uses up to 375 power watts when in active printing, with 1.7 watts in sleep mode, standby watts up to 8.7 and auto off or off watts of 0.1.
Its page per minute capability is quite low at 19 ppm.
Comes with a standard sheet tray capacity of 150 sheets.
With a ppm of 19, the HP LaserJet Pro M277dw wireless color printer can be utilized via the wireless connection by 5 people or less simultaneously. It spends about 13 seconds in order for the initial color page to be outputted as well as a monthly page volume ranging from 250 – 2500 pages.
Possessing a scan resolution of 1200 dpi, it supports most sizes of paper and is produced with a regular paper tray of 150 sheet capacity as well as an ADF of 50 sheets. It, unfortunately, isn't available with duplex printing and you'd need to copy 2 sides manually.
Doesn't come with duplex printing and double-sided printing must be done manually.
The Canon image class LBP612Cdw is one of the best wireless printers on the market. It connects via wifi, Ethernet, USB, and wifi direct. Although it's speed isn't one of its positives at 19 pages per minute it offers users a good mix of great features and print quality.
This wireless laser printer also has a paper capacity of 150 which is ok for office or home use. So if you are looking for a wireless printer that offers great graphics this is an excellent choice.
Possesses a resolution of 600 by 600 dpi.
HP, 200 M251nw LaserJet Pro Wireless Color Printer offers a print resolution of 600 by 600 dpi. It as well creates images which are extremely crystal clear and can handle a great number of sheets on its sheet tray.
It can easily be connected via 1 Ethernet TX network 10/100 Base, USB 2.0 high-speed port or 802.11b Wireless networking to the network.
This printer is regarded as one of the best wireless laser printers available in the market. Brother Compact MFCL2700DW Laser all in one printer utilizes an optical resolution scan of 600 by 2400 dpi as well as a print speed maximum of 27 ppm.
It is compatible with Windows and Mac operating system. This all in one printer supports duplex printing as well. Its sheet tray can easily hold up to 250 sheets at once and does amazingly for heavy printing.
The Brother, Wireless Compact DCPL2540DW Laser Printer takes the number one spot as one of the best wireless color laserjet printers. This is because it has proved itself as one of the fastest laser color printers available in the market. It is manufactured with a powerful 2400 by 600 dpi maximum resolution, which ensures you of topmost quality and high Def copies.
This professional printer is available with a sheet capacity of 250 sheets and is compatible with a variety of paper sizes. It can easily be connected wirelessly through USB 2.0 interface or network and supports auto duplex printing as well.
Sheet capacity may be considered average depending on users needs.
Due to the printers wireless nature, it means you will not have to bother about wires or cords creating an obstruction when working. Nevertheless, the sensitivity of the connection will differ greatly from one form to another. Always pick an item that has coverage over a wide area.
The resolution of the printer you opt for is the major determinant of the clarity of the image it produces for you. A machine with a 600 dpi, for example, is the lowest resolution quality you can get for laserjet printers. On the other hand, a printer with 2400 dpi would possess amazing image clarity. The higher the dpi gets the better the image results you get.
The best printer that you can go for should be capable of supporting various functionalities as well as being compatible with a lot of operating systems. It should also be able to connect simultaneously to laptops, smartphones, computers, tablets, and other tech gadgets.
This is how quickly the machine prints and is usually referred too in terms of prints per minute or ppm. Which means how many documents it can print out in a minute for you. This is a vital aspect to consider if you require a lot of documents to be printed daily and need it done fast.
Most of the printers in this review of the top best wireless laserjet printers are multifunctional models that scab, print, and copy, which is great for usage in a work environment. It's also good to opt to purchase a printer that can easily be connected to your mobile gadgets via Google cloud print or Apple AirPrint. This makes it very easy for you to print documents stored on your mobile device, cloud or tablet.
A model with color functionality is an excellent choice for you if you require a printer to print out presentation materials or creative projects. This helps to elaborate prints that look very professional.
Asides from the resolution of a printer which is measured in dpi and determines image quality. You must also keep your eye on the accuracy of the printer. This is because most times fast printers may tend to output less accurate prints, hence, you need to find that awesome balance between quality and speed.
One of the hardest aspects of choosing a wireless color laserjet printer is knowing just which one is the best for your specific requirements. This is why this review is important you can now easily purchase the most efficient choice for your needs once you know what to look out for.


text:
Q: flatpak define dependency in manifest How to add another flatpak packages as a dependency to my app?
I want my app to be able to call mpv, so it would be nice to install io.mpv.Mpv along with my app.

A: I think it is not possible. The classical way is to write the mpv compilation rule in your application manifest so that it can then be used by your application. You can find the mpv manifest here, so that you can include/adapt this code for your application manifest.

redpajama_set_name: RedPajamaStackExchange


Get "Behind the Scenes" on January 19th and 20th, 2019 at the Orange Empire Railway Museum in Perris, where volunteers operate, maintain and restore the West's largest collection of vintage rail cars.
At this annual all-day event, visitors get special access and tours of locomotives, passenger and freight cars, streetcars, interurban electric cars and artifacts dating back to 1870.
Bring the family for a fun and fascinating day! Activities at Behind the Scenes will feature tours and special equipment operations. Visit Ruffulo Carhouse 7, a restoration shed filled with trains and trolleys that is not usually open to the public. Get special access to the pit where you can go underneath a street car and see how it works. For an additional fee, get behind the throttle (under supervision) and run a real locomotive. Enjoy other special equipment.
Admission includes unlimited rides on other classic passenger trains and streetcars of Southern California's railroad past. This gated event supports museum operations and the continued restoration of historic rail cars and rail line.
Admission is free to members! Non-member Admission is $12 for ages 12 and up, $8 for children ages 5 to 11, and children ages 4 and under are free. Tickets available at the Box Office on the day of the event.
The address is 2201 S. "A" St., Perris, CA.Visit www.oerm.org or call (951) 943-3020.
© 2018 Southern California Railway Museum, dba Orange Empire Railway Museum. All Rights Reserved.


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Lei Muk Shue Estate () is a public housing estate in Sheung Kwai Chung, Tsuen Wan, New Territories, Hong Kong, near the exit of Shing Mun Tunnels. It is the largest public housing estate in the Tsuen Wan District, with the population of 28,100 in December 2021. Although it is geographically located in Sheung Kwai Chung (literally means "Upper Kwai Chung"), administratively it belongs to the Tsuen Wan District instead of the Kwai Tsing District because it is at the west of Wo Yi Hop Road, the boundary between the two districts.

History
Lei Muk Shue Estate was initially constructed in the 1970s when 17 buildings were erected. It started redevelopment in the 1990s, at which time eight old buildings were demolished. Ten new buildings and a shopping centre built between 1998 and 2005.

Houses

References

Tsuen Wan
Tsuen Wan District
Residential buildings completed in 1975
Residential buildings completed in 1980
Residential buildings completed in 1998
Residential buildings completed in 2000
Residential buildings completed in 2005
Public housing estates in Hong Kong

redpajama_set_name: RedPajamaWikipedia


text:
Q: Angular MyCtrl as instead of scope not working for me I've got a form with hundred of fields.
As part of a secondary controller I'm trying to avoid the $scope to bind the data to my view. The way I go is:
angular
    .module('app')
    .controller('SequencesController', SequencesController) // main controller for the view
    .controller('AccordionCtrl', AccordionCtrl); // the one I'm targetting

AccordionCtrl.$inject = ['$scope','$http'];
function AccordionCtrl($scope,$http) {
    this.foo = "bar";
}

I'm using this on my view but it's not working.
<div ng-controller="AccordionCtrl as acc">
           Acc : {{ acc.foo }}
</div>

Using $scope does work though. Any ideas?

Extra information:
The view is binded to a main controller that's called like that in app.js
.when('/sequences', {
            controller: 'SequencesController',
            templateUrl: 'app/Sequences/sequences.view.html',
            controllerAs: 'vm'
        })

A: When you are trying to access to the object(controller) property: {{ acc.foo }}, which angular is doing behind is: $scope.acc.foo, because this is how angular works, you must define your variables inside the scope.
If you dont want to interfer in the showing variables, create two diferent objects inside the scope: $scope.viewVars and $scope.backVars and add them all properties you need separately.


Such intense concentration! Happy WW.
WHat a cute little girl. Happy ww.
she's so adorable–you must be so proud!!
Look at those cute little painted toesies!
My niece is around the same age. She loves the camera too. It must be something about cameras but my niece knows exactly when someone is about to take a photo. She sort of likes start posing and stuff. All our family laugh when she does it. Is that the same with your kids?
Man your blog is loaded with little extras. It crashed my browser twice and I had to open it in Firefox to get it to finish loading. Looks like your blog is as busy as your life sounds. I hope you get some rest soon!


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text:
Callan Gray
2 Reporters Leaving Wednesday, Slawson Stays at WKBW-TV
At the end of the May book, 2 reporters are moving onto their next stops. May 23 will be the last day for WGRZ-TV's Danny Spewak and WIVB-TV's Ali Ingersoll.
Gray Moves To Top 20 Market, 2 New Hires Join WIVB-TV
Callan Gray, from WIVB-TV, bid farewell to viewers in Western New York earlier this month. You can see her goodbye in the tweet below.
https://twitter.com/CallanGray4/status/983215827171332096
The former weekend anchor/reporter has moved to KSTP-TV in Minneapolis, Minnesota, which is Market 15 in the country. She will be a reporter for the ABC affiliate. Gray's three-year stint in Buffalo came after she worked at WCYB-TV/WEMT-TV in Tri-Cities, Tennessee as a reporter and anchor. while at Syracuse University, she was also the local host at WAER-FM of All Things Considered, NPR's flagship program.
She is a graduate of Syracuse University where she earned degrees in Journalism and Earth Science.
Two Ithaca College graduates have started at WIVB-TV within the past few weeks.
Kelsey Anderson joined the station in March 2018 as a multi-media journalist. The Western New York native spent over four years in Boise, Idaho, at KBOI-TV as an anchor and reporter. Before leaving the station, Anderson was the station's morning anchor alongside Bryan Levin. While out west, she earned awards from the Idaho State Broadcasters Association and the Idaho Press Club for her reporting. Anderson previously interned at WKBW-TV and WENY-TV in Elmira, New York.
WIVB-TV wasted no time in finding a replacement for Shannon Shepherd, who left the station to join Fox Sports San Diego. Jenna Harner joins the CBS affiliate as a sports reporter/anchor from WENY-TV in Elmira, New York, where she most recently served as Sports Director. She made her on-air debut this past weekend, just in time for the NFL Draft, baseball in Western New York, and the Bandits season. She is originally from Connecticut and interned at WFSB-TV and Fox CT before her stint in Elmira.
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text:
Q: ORMlite Android foreign key support I am not clever from ORMlite documentation. Is is possible to declare in class, that this parameter is foreign key?
e.g. I have table Customer:
@DatabaseTable(tableName = "customer")
public class Customer {
    @DatabaseField(id = true)
    private String customerName;

    @DatabaseField
    private String customerSurname;

    @DatabaseField(foreign = true)
    private String accountNameHolder;

    @DatabaseField
    private int age;

    public Customer() {
    }
}

AccountNameHolder should aim towards DatabaseField name from table Accounts. How to do that? I have found only parameter foreign = true, but there is nothing about, which parameter and from which table it represents.
Thanks

A:
AccountNameHolder should aim towards DatabaseField name from table Accounts. How to do that?

I'm not exactly sure what you want but possibly you should change your foreign field to be the actual type instead of a name:
@DatabaseField(foreign = true)
private Account account;

Internally, ORMLite will store a account_id field (maybe the string name) in the Customer table but you don't have to worry about that.  Remember that when you query for a Customer, the Account that is set on the account field will just have the id field set.  To have ORMLite also lookup the account you will need to set the foreignAutoRefresh=true.
As @Lalit pointed out, here is some documentation on this subject.  We've spent a long time on the documentation so it should be helpful.

*

*Foreign objects

*Foreign auto refresh
Also, there is some example code about foreign fields.
Hope this helps.


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text:
November 19, 2019 Guidelines
Which device converts digital signals to analog signals?
1 Which device converts digital signals to analog signals?
2 Which converts digital signal into analog signal and analog signal to digital signal?
3 In which method the digital signal is converted to analog signal using modulation?
4 Can you convert digital to analog?
5 How can we convert analog signal to digital?
6 Why is analog better than digital?
7 What is digital signal example?
8 What are the main steps to convert an analogue signal to digital signal?
9 What are three kinds of digital to analog conversions?
10 How do you convert analog signal to digital?
11 How do digital to analog converters work?
12 What are some examples of analog and digital signals?
13 What are some things that use analog signals?
14 What is a digital signal?
A modem is a device that translates digital signals from a computer into analog form so that they can be transmitted over analog telephone lines.
Which converts digital signal into analog signal and analog signal to digital signal?
In electronics, a digital-to-analog converter (DAC, D/A, D2A, or D-to-A) is a system that converts a digital signal into an analog signal. An analog-to-digital converter (ADC) performs the reverse function.
In which method the digital signal is converted to analog signal using modulation?
The following techniques can be used for Digital to Analog Conversion: 1. Amplitude Shift keying – Amplitude Shift Keying is a technique in which carrier signal is analog and data to be modulated is digital. The amplitude of analog carrier signal is modified to reflect binary data.
Can you convert digital to analog?
Digital to analog conversions can be performed using resistor networks and the conversion to an analog signal is usually in the order of nanoseconds. Since the digital information is a step approximation of the input signal, the resulting output from a D to A converter reflects this step nature of the signal.
How can we convert analog signal to digital?
ADCs follow a sequence when converting analog signals to digital. They first sample the signal, then quantify it to determine the resolution of the signal, and finally set binary values and send it to the system to read the digital signal. Two important aspects of the ADC are its sampling rate and resolution.
Why is analog better than digital?
Analog signals are much higher density, and can present more refined information. Analog signals use less bandwidth than digital signals. Analog signals provide a more accurate representation of changes in physical phenomena, such as sound, light, temperature, position, or pressure.
What is digital signal example?
Difference between the Analog signals and Digital signals
Analog signals
Digital signals
Analog signals produce too much noise. Digital signals do not produce noise.
Examples of analog signals are Human voice, Thermometer, Analog phones etc. Examples of digital signals are Computers, Digital Phones, Digital pens, etc.
What are the main steps to convert an analogue signal to digital signal?
What are three kinds of digital to analog conversions?
Types of DACs
Weighted Resistor DAC.
R-2R Ladder DAC.
How do you convert analog signal to digital?
How do digital to analog converters work?
DACs take a binary number of the digital form of audio and turns it into an analog voltage or current that, when done entirely over the course of a song, can create a wave of audio that represents the digital signal. It creates the analog version of the digital audio in "steps" of each digital reading.
What are some examples of analog and digital signals?
Temperature sensors, FM radio signals, Photocells, Light sensor, Resistive touch screen are examples of Analog signals. Computers, CDs, DVDs are some examples of Digital signal. The digital signal bandwidth is high. Analog signals are deteriorated by noise throughout transmission as well as write/read cycle.
What are some things that use analog signals?
Uses of Analog. Analog signals have a number of uses. AM and FM radio, for instance, are signals that are transmitted in analog. Telephones (at least simple, older telephones) use analog signals to transmit voice data to the phone central office.
What is a digital signal?
A digital signal is a way of transmitting data that converts the data to discrete values, usually based on the binary code that computer systems work upon, which consists of packets of information coded as strings of ones and zeros. Using digital signaling allows for an accurate and nearly identical copying…
Does bevel go up or down?
How do you send G codes to 3D printers?


text:
Q: Why Redefine Function Namespace? Compiling and executing the following files works without any issues. When I remove the aos:: from in front of the euler function in Ode.cpp the compiler throws the following error.
Ode.cpp:13: undefined reference to `aos::euler(std::vector<double, std::allocator<double> >* (*)(std::vector<double, std::allocator<double> >*, unsigned int, unsigned int), std::vector<double, std::allocator<double> >*, unsigned int, unsigned int)'
collect2: error: ld returned 1 exit status

Why does it do that? I already defined the namespace in both the definition and the implementation files of Ode.
Cheers,
MrMcKizzle
Ode.hpp
#include <SDL2/SDL.h>
#include <vector>
#include <iostream>
#include <string>

#ifndef ODE_HPP
#define ODE_HPP

namespace aos
{
    std::vector< double > * euler(
        std::vector< double > * (*)(std::vector< double > *, Uint32, Uint32),
        std::vector< double > * x, Uint32 dt, Uint32 t
    );

    class Integrator {
        public:
            Integrator();
            //~Integrator();
            std::vector< double > * (*integrator)(
                std::vector< double > * (*)(std::vector< double > *, Uint32, Uint32),
                std::vector< double > * x, Uint32 dt, Uint32 t) = euler;  ///< Stores a pointer to the default ODE integrator function (defaults to euler)
            std::vector< double > * integrate(
                std::vector< double > * (*)(std::vector< double > *, Uint32, Uint32),
                std::vector< double > * x, Uint32 dt, Uint32 t
            );
    };
}
#endif

Ode.cpp
using namespace aos;

std::vector< double > * aos::euler(
    std::vector< double > * (*f)(std::vector< double > *, Uint32, Uint32),
    std::vector< double > * x, Uint32 dt, Uint32 t)
{
    std::cout << "aos::euler" << std::endl;
    return f(x, dt, t);
}

Integrator::Integrator(){}

std::vector< double > * Integrator::integrate(
    std::vector< double > * (*f)(std::vector< double > *, Uint32, Uint32),
    std::vector< double > * x, Uint32 dt, Uint32 t)
{
    std::cout << "Integrator::integrate" << std::endl;
    return this->integrator(f, x, dt, t);
}

main.cpp
#include "Ode.hpp"

#include <SDL2/SDL.h>
#include <vector>
#include <iostream>
#include <string>

std::vector< double > * dummysys(std::vector< double > * x, Uint32 dt, Uint32 t)
{
    cout << "main.cpp::dummysys" << endl;

    return new vector< double >();
}

int main(int argc, char **argv)
{
    aos::Integrator * intgr = new aos::Integrator();

    vector< double > x;
    //integrate(dummysys, &x, 16, 123);
    intgr->integrate(dummysys, & x, 16, 123);

    return 0;
}

A: In your cpp enclose your implementation in the namespace aos just like you did in the hpp.
namespace aos
{
std::vector< double > * euler(
    std::vector< double > * (*f)(std::vector< double > *, Uint32, Uint32),
    std::vector< double > * x, Uint32 dt, Uint32 t)
{
    std::cout << "aos::euler" << std::endl;
    return f(x, dt, t);
}

Integrator::Integrator(){}

std::vector< double > * Integrator::integrate(
    std::vector< double > * (*f)(std::vector< double > *, Uint32, Uint32),
    std::vector< double > * x, Uint32 dt, Uint32 t)
{
    std::cout << "Integrator::integrate" << std::endl;
    return this->integrator(f, x, dt, t);
}
}

And you can use the using namespace aos in the main.cpp


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text:
Q: TOC in DITA - Count nodes in different documents How is it possible to acces and count nodes in linked xml documents with the xsl:number function?
I´m trying to aim something like <xsl:number level="multiple" format="1.1." count="someNode | document(@href)/someOtherNode"> but within the 'count' function it´s not possible to use the 'document()' function. Therefore there must be another way to access elements stored in other '.xml' - documents.
EDIT
For what I understood is that I have to create a temporary copy of my whole node-structure for 1st performance and 2nd readability (and 3rd of course - accessability).
My Idea: I want to store the whole nested node tree in a readable variable. Therefore I have to create a variable and copy all nodes plus their content into it.
This is my desired file structure:

*

*Root Document .XML contains all language specific documents as ditamaps
<map>
<navref mapref="de-DE/A.2+X000263.ditamap"/>
<navref mapref="en-US/A.2+X000263.ditamap"/>
<navref mapref="es-ES/A.2+X000263.ditamap"/>
</map>

*Language specific manuals (.ditamap) - multiple documents possible
<bookmap id="X000263" xml:lang="de-DE">
<chapter href="A.2+X000264.ditamap"/>
</bookmap>

*Chapters for each manual
<map id="X000264" xml:lang="de-DE">
<topicref href="A.2+X000265.ditamap"/>
</map>

*Contents (.dita) or SUB-Chapters (.ditamap)
<map id="X000265" xml:lang="de-DE">
<topicref href="A.2+X000266.dita"/>
<topicref href="A.2+X000269.dita"/>
<topicref href="A.2+X000267.ditamap"/>
</map>
All these documents contain several nodes that I want to count and easily access (e.g. to prevent over-using the document(@...) function.
I started to create a temporary copy of all contents like so:
<xsl:variable name="spine">
    <xsl:for-each select="collection('../../?select=*.xml;recursive=yes')">
        <xsl:for-each select="//*">
            <xsl:copy-of select="current()"/>
        </xsl:for-each>
    </xsl:for-each>
</xsl:variable>
I´m aiming for a solution that just reads through all the .xml / .ditamap /.dita documents in their correct order and that gets me a 1:1 copy of all nodes and contents. Then I could easily read the stored variable node tree and would not have to manually traverse through all documents. And of course I could easily count then all nodes of a specific type.
Thanks in advance.

A: In XSLT 3.0 you can use the doc function in a pattern (count attribute is a pattern), but I doubt that would help you here.
But since you are omitting the select attribute, I assuming you are counting the context node. Unless the context node is in the document you are referring to, there is no way to count it, because the pattern must match the current node. If the context node is already in the document you are referring to, you can omit the document function in the pattern (leave the rest of the pattern in) and it will "just work".
If you are trying to count something that cannot be captured by a pattern, but requires a select expression, then you should manually create the numbers by using a combination of count expressions. Since I don't know your input document, I can't really give an example.
Edit (after your edit)

<xsl:for-each select="//*">
   <xsl:copy-of select="current()"/>
</xsl:for-each>

Don't do this (sorry for the bold ;). This has the effect that you create a copy of each descendant element. I.e.:
Input:
<root>
   <child>
      <deeper>
   </child>
</root>

will result in output like this (note how each descendant is copied again):
<root>
   <child>
      <deeper/>
   </child>
</root>
<child>
   <deeper/>
</child>
<deeper/>

In fact, something along those lines should suffice (I added the originating URI, may help with debugging):
<xsl:variable name="spine">
    <xsl:for-each select="collection('../../?select=*.xml;recursive=yes')">
        <doc original-href="{base-uri()}">
            <!-- assuming you do not need any comments in the root of the document -->
            <xsl:copy-of select="/*"/>
        </doc>
    </xsl:for-each>
</xsl:variable>

If you do not make a copy, I think you can still get what you want, but as said above, you may need to do some counting yourself.
Something I didn't mention: if you want to count nodes from several sources, and they differ in element name only, it may be enough to just write count="someNode | someOtherNode". However, if someOtherNode is from a different document, then you must make sure that the current matching selection is in the correct order. By default, selecting multiple documents has implementation defined order.
In short, I think your suggested approach is good. I doubt it has performance benefits (because you are creating a copy of everything), but just time your solution to find out.

A: After some research and yet another request on Stackoverflow, I got a working solution for my needs. The following describes the way I´m handling the situation right now:

*

*Create a composed document (see here) stored in a variable

*Now I can apply the templates according to the variable like so
<xsl:apply-templates select="$myVar/document/*"/>

*With this I can easily access and count each node that exists in this single source document (as far as I understood it´s not possible to easily count nodes that are not composed in a single document)

A: Use DITA-OT (http://www.dita-ot.org/) to make the compound middle file from root document (map). DITA-OT's "preprocess" and "TopicMerge" processing will generate following structured merged middle file:

*

*Expanded map structure portion composed of only topicref elements (in your case).

*Topic body portion referenced from map portion.

Usually TOC is generated by the stylesheet from map structure portion by counting the topicref elements hierarchy.
From your example, I have noticed that the root map is composed of navref elements. The navref reference will not be resolved from its DITA definition. Using mapref element instead of navref will resolve the reference and the referenced contents will be included into the merged middle file.
This is the most convenient way to accomplish your requirement.


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text:
Q: How to format fields read from pdf with iText java I want to read every editable field from a pdf file, and given their origin format, save the flattened pdf
This is what I tried to do to save the flattened pdf with every field
    FileInputStream existingFileStream = new FileInputStream (src);

    PdfReader pdfReader = new PdfReader (existingFileStream);
    PdfStamper stamper = new PdfStamper (pdfReader, new FileOutputStream(dest));

    AcroFields form = stamper.getAcroFields();
    HashMap map = (HashMap) form.getFields();
    Set s = map.keySet();
    int i = 0;
    for (Iterator it = s.iterator(); it.hasNext();) {
         String key = (String) it.next();
         i++;
         //Grabamos en el campo el valor de un contador

         form.setField(key,form.getField(key));
    }

    stamper.setFormFlattening(true);
    stamper.setFreeTextFlattening(true);
    stamper.close ();
    pdfReader.close ();

With this code I've achieved to flatten the pdf but I dont know how to format all the fields.
An example of the problem is that if the origin PDF has 2 empty editable fields, the result PDF does not save the value of those fields.


text:
Indonesian rock is rock music from Indonesia, a product of the culture and globalizing outlook of the country, similar to this genre's music globally. Indonesian-specific ideas about individualism, interdependency, modernism, and the supernatural have also been observed in the rock videos and music of the nation.

One of the largest rock festivals in Indonesia is the Jakarta Rock Parade, a 3-day festival recently hosting over 100 bands.

History

1940s - 1960s

Rock music began to enter Indonesia around the 1950s during the western rock fever. However, the heyday of rock music in Indonesia was preceded by the band The Rolles (1967) with the genre of jazz rock music. They brought music with different concepts so that they were able to play with the tastes of music lovers at that time. The band was also able to survive and was still popular until the 1980s.

In that era, Indonesian-Dutch rock bands were also very popular, such as The Tielman Brothers, which was founded in 1947 by several youths from Kupang (Reggy, Ponthon, Andy and Loulou Tielman). The band is generally seen as the founder of Indorock, although other Indorock bands have existed before them. Being ethnically Indonesian and playing Western music for white audiences in the Netherlands and Germany.

1970s - 1990s

The development of rock music in Indonesia grew rapidly when rock bands such as God Bless, Gang Pegangsaan, Giant Step and Rawa Rontek moved quickly to strengthen the rock music genre in Indonesia. Along with the development of rock music in Indonesia, the term "Underground" emerged to group bands with the concept of loud, wild and extreme music.

The 1980s can be said to be the golden era of rock music in Indonesia because early 1988 became the first history in which rock music was performed directly in front of the public.

Then when slow rock music from Malaysia started to boom thanks to the appearance of the band Search through the hit song "Isabela". So in Indonesia the slow rock genre began to gain wide popularity. An Indonesian musician who is famous for playing the slow rock genre is Deddy Dores.

In addition, there are also many works of Deddy Dores performed by Nike Ardilla, Cony Dio, Poppy Mercury, Mayank Sari. The pattern of Indonesian slow rock has also plagued other musicians or singers in Indonesia such as Oppie Andaresta, Minel, Inka Christy, Lady Avisha, Cut Irna, and others. The popularity of Indonesian slow rock occurred during the 1980s to 1990s. In that era, Indonesian Rock mostly had a mellow and sad music style

List of bands
This is a list of Indonesian rock bands:
 ADA Band
 The Changcuters
 Cokelat
 Dewa 19
 Drive
 Edane
 God Bless
 Guruh Gipsy
 Gigi
 Jamrud
 J-Rocks
 Kekal
 Koes Plus
 Koil
 Kotak
 Padi
 Pee Wee Gaskins
 Killing Me Inside
 Navicula
 Netral
 Nidji
 Noah (band)
 Nymphea
 /rif
 Sajama Cut
 Shorthand Phonetics
 Slank
 Sore
 Sucker Head
 Superman Is Dead
 The S.I.G.I.T.
 Tielman Brothers
 Voice of Baceprot
 Zeke and the Popo

See also
Indo pop
Alternative
Turbo-folk, presenting similarities with 90's Indonesian rock music.
Music of Indonesia
List of Indonesian musicians

References

Rock bands

Indonesian styles of music
Lists of musicians by nationality
Rock


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Q: how to import __future__ for keyword-only argument of python 3.0? The following code in python2.6 throws syntax error
>>> def f(a,*args,c):
  File "<stdin>", line 1
    def f(a,*args,c):
                  ^
SyntaxError: invalid syntax

but this syntax is valid in python3.0. I would like to know what should I import in my interpreter to make it work.
ie. from import __future__ ????
for importing print function of 3.0, I would do from __future__ import print_function
similarly this defination is invalid in 2.6
def f(a,*b,c=5,**kwargs):

while it is legal in 3.0

A: The new syntax is discussed in PEP 3102 and it's indeed not valid in Python 2.x.
However you can obtain the keyword arguments from **kwargs manually:
def f(a, *b, **kwargs):
    if 'c' in kwargs:
        pass

The other alternative is to upgrade to Python 3.x.

A: This feature of the Python 3 compiler has not been backported to Python 2.x.
There is no magic from __future__ import switch to enable it, your only option is to upgrade to Python 3.x.
Your second function could instead be defined as:
def (a, *b, **kwargs):
   c = kwargs.pop('c', 5)

to be Python 2 compatible.

A: Another way to emulate keyword-only-arguments is:
def f(a, *args, **kwds):
    b = kwds.get('b', 42) # 42 being the default for b

if you wan't to make sure that no unsolicited arguments are passed you can use pop instead:
def f(a, *args, **kwds):
    b = kwds.pop('b', 42)

    assert not kwds # after we've popped all keywords arguments kwds should be empty


text:
using System;

namespace Tuple
{
    public class StartUp
    {
        public static void Main()
        {
            var inputTokens = Console.ReadLine().Split(' ');
            var names = $"{inputTokens[0]} {inputTokens[1]}";
            var address = inputTokens[2];
            var namesAdress = new Tuple<string, string>(names, address);
            Console.WriteLine(namesAdress);

            inputTokens = Console.ReadLine().Split(' ');
            var name = inputTokens[0];
            var liters = int.Parse(inputTokens[1]);
            var nameLiters = new Tuple<string, int>(name, liters);
            Console.WriteLine(nameLiters);

            inputTokens = Console.ReadLine().Split(' ');
            var intParam = int.Parse(inputTokens[0]);
            var doubleParam = double.Parse(inputTokens[1]);
            var intDouble = new Tuple<int, double>(intParam, doubleParam);
            Console.WriteLine(intDouble);
        }
    }
}

redpajama_set_name: RedPajamaGithub