text:
will yip
Circa Survive writing new album
Although details are scarce, the pieces of the puzzle seem to indicate that Circa Survive are currently at work writing and demoing for their fifth studio album. Circa guitarist Brendan Ekstrom took to Twitter over the weekend to vaguely discuss the band's current plans. @stupidfaqqot n ...
Tj Horansky
I Am The Avalanche announce new album 'Wolverines', stream new song "The Shape I'm In"
Brooklyn natives I Am The Avalanche have announced that their new album Wolverines will be out March 17 via I Surrender Records. The band are currently streaming the album's first single, "The Shape I'm In", over at esquire.com. The album was produced b ...
Polar Bear Club – Death Chorus
Polar Bear Club Death Chorus Polar Bear Club have had one bender of an album cycle. In the two-year space between records, they've redefined their lineup (two founding members remain, the core songwriting duo of singer Jimmy Stadt and guitarist Chris Browne), opened for their heroes in Bad Religion, signed up for marriage (congrats, Jimmy!) and ...
Brian Kraus
Title Fight – Spring Songs EP
Title Fight Spring Songs EP Don't let the name fool you: Spring Songs is definitely not a collection of cheery toe-tappers from the usually gloomy Kingston, Pennsylvania, four-piece. Nope, the plodding four-track EP carries on right where 2012's Floral Green left off, exploring more of the sludgy, ruminating neo-grunge and Jawbreaker-esque '90s punk that's become the band's hallmark. Like on Flora
Brendan Manley
Various Artists – Off The Board: A Studio 4 Family Compilation
Various Artists Off The Board: A Studio 4 Family Compilation Off The Board: A Studio 4 Compilation is essentially an unintentional follow-up to Run For Cover Records' 2011 collection, Mixed Signals. Like that compilation, it features new, unreleased songs from some of the best acts in contemporary punk and emo. Althoug ...
Brian Shultz
Daylight stream new song "Siblings" from the upcoming Will Yip compilation
Doylestown, PA natives Daylight are streaming "Siblings", their contribution to the Will Yip compilation, over at rollingstone.com. Listen to the track here! The upcoming compilation is titled Off The Boards: A Studio 4 Family and will be released October 8. It will featu ...
Anthony Green announces fall solo tour and new album details, streams new single "Breaker"
Circa Survive frontman and Energizer bunny Anthony Green recently revealed that he will be embarking on a solo tour this fall in support of his new record, Young Legs. Young Legs will be released November 12 off of Green's own newly launched imprint label, Moshtradamus Records. The album release and ...
Producer Will Yip to release compilation featuring Circa Survive, Title Fight, Man Overboard, others
Most fans of AP are probably familiar with the name Will Yip by this point. If you're not, well, he might be your favorite producer and you just don't know it. On October 8, Yip will be releasing Off The Board: A Studio 4 Family Compilation, a compilation featuring new and previously unreleased tracks from bands such as Circa Survive, Title Fight, Man Overboard, Balance And Composure, Tigers J
"There Is Always Darkness" : In The Studio with Anthony Green
Circa Survive frontman Anthony Green can be a difficult person to get a hold of these days. Between recording his new solo album, Young Legs, touring with his "day job," and taking his two young boys to the playground, it's easy to understand why the highly revered lead singer can seem so elusive. AP was lucky eno... Read More ...
Anthony Green recording new album 'Young Legs' with Will Yip, Good Old War
According to a series of recent tweets and Vine posts, Circa Survive frontman Anthony Green is currently in the studio recording Young Legs, his follow-up record to 2012's Beautiful Things. Producer Will Yip (Daylight, Man Overboard, Title Fight) will be rockin' the control boards for the new album. This is good news for fans of C ...
Daylight – Jar
Daylight Jar Considering that up until recent history, Doylestown, Pennsylvania's musical claim to fame was pop bad-girl Pink and Afro-sporting Stevie Wonder knockoff Justin Guarini (that guy who almost beat Kelly Clarkson on American Idol), it's pretty incredible that these days sonic innovators Circa Survive and Balance And Composure both call D-Town home. And now, w ...


HomeBlogUncategorizedRole of hospital owners while executing brand promise campaigns and brand delivery challenges of healthcare institutions, a healthcare consulting perspective.
These short set of words represent the vision and mission of the business to the customers; the first impression that conveys the promise an organization wants to make. It helps the organization to position their brand in the industry and tell people who they are and what they stand for. Any long-term looking organizations need strong brand positioning. Specialists of brand strategy and healthcare consulting confirms that, it is a must to have a clear brand strategy that will provide them uniqueness, competitiveness and that guarantees greater value in the healthcare landscape.
It is critical to differentiate your organization from competitors and position it within today's changing market. In healthcare too, an organization's image can be very influential. It has the potential to attract more patients and funding, which in turn could be the difference between success and failure. The identity and brand recognition can also direct the behavior of employees and help attract top talent.
As business models evolve, the way hospitals brand themselves must evolve as well. However, it is not enough to just have a branding strategy in place. The actual patient experience must fulfill on that promise. The management, staff, physicians and employees of the hospital should make sure to align brand strategy with business strategy; to balance investments in technology, people and infrastructure with an investment in brand.
Successful branding must encapsulate the entire healthcare organization, its people, actions and activities. For branding to play a pivotal role in the company, it has to have a strong support from the CEO and corporate management.
• Consistently invest in building a brand that will distinguish you. Branding should not be a one-off session but a truly integrated part of the boardroom strategy. A strong brand is instantly recognizable, is comprised of the messaging and visual elements, and connects with people.
• The top management also becomes highly visible representatives of the brand. It is imperative to invest in developing top leaders that not only understand the strategic charter of the brand but also enable the brands' further development and growth.
• As hospital owners, you have to inculcate a strong internal brand culture. For your brand identity to truly be effective, the brand values, mission, and expectations must be internally ingrained within your brand culture.
• Communicate healthcare branding strategy and values through every single touch-point of your organization. Make sure your brand is clearly understood, believed and delivered by owners and staff of the practice.
• An essential element of a successful brand strategy is the collaboration of your internal stakeholders. Your physicians, staff, and other team members are on the front line of healthcare delivery. Hospital owners should make sure that the staff understands how their behavior contributes to delivering on the brand promise.
Healthcare has changed over the past few years. Like other industries, it has become consumer-driven. What patients think of you before they know you is as crucial as their experience with the service you provide. Hence, the development of your healthcare brand and branding campaigns are highly important and dynamic exercises. Stay relevant and visible by doing it right, backed by consistent performance.
By following well defined branding strategies, companies can strategically navigate brand delivery challenges and drive successful business impact. As part of our healthcare consulting, India, Africa and GCC, team at Sarathy advisory have expertise in branding and positioning of healthcare organizations, services and products. The team helps top management in aligning brand strategy with business strategy, so that organizations discover opportunities for growth and competitive positioning.


text:
Q: How to populate a group in mongoose I have this in my mongoose schema...with some group...
'use strict';

var mongoose = require('mongoose')
, Schema = mongoose.Schema;

var clientSchema = new mongoose.Schema({

    name                                : { type: String },
    offerings                   : [{ type: String }],
    cscPersonnel                : {
        salesExec                   : { type: Schema.Types.ObjectId, ref: 'User' },
        accountGM                   : { type: Schema.Types.ObjectId, ref: 'User' },
},
    },
    netPromoterScore        : { type: Number }

});

module.exports = mongoose.model('clients', clientSchema);

I tried to populate reff dis way...I have also populated in ref (user as {path:'cscPersonnel'})
function getOneById(id){
    var deferred = Q.defer();
console.log("im in get by id" +id);
    model
        .findOne({ _id: id })
        .populate({path:'cscPersonnel'})//one way
           /* 'cscPersonnel salesExec',   //second way
            'cscPersonnel accountGM', */
        .exec(function (err, item) {
            if(err) {
                console.log(err);
                deferred.reject(err);
            }
            else
                console.log(item);
                deferred.resolve(item);
        });

    return deferred.promise;
} // gentOneById method ends

but unfortunatly ended up with this error!!!!
CastError: Cast to ObjectId failed for value "[object Object]" at path "_id"
{
  "message": "Cast to ObjectId failed for value \"[object Object]\" at path \"_id\"",
  "name": "CastError",
  "type": "ObjectId",
  "value": {
    "salesExec": "56cf5f09245f8a240b30693b",
    "accountGM": "56cf5f09245f8a240b30693b"
  },
  "path": "_id"
}

how to make it solve this issue.... do help , thanks in advance

A: Please try this one
model
    .findOne({ _id: id })
    .populate({path: 'cscPersonnel.salesExec'})
    .populate({path: 'cscPersonnel.accountGM'})
    .exec(function (err, item) {

redpajama_set_name: RedPajamaStackExchange


The CIC recently launched a national Industrial Hemp Strategy and Capacity Development Program to sustain and advance the Canadian industrial hemp industry. Celebrating its 10th year since gaining approval to grow industrial hemp, farmers have been steadily increasing acreage across Canada; specifically in the provinces of Manitoba, Saskatchewan, Alberta, Ontario and now Quebec. Originally, the industry relied heavily on the hemp seed and oil markets; however, fibre markets are being rapidly developed that create diverse opportunities and, potentially, a significantly better return on investment for the grower.
A recently completed collaborative project between Avcorp Industries, Profile Composites, National Research Council and the Composites Innovation Centre refined and evaluated a novel in-situ semi-impregnated material process for the manufacture of composite aerospace structures. The new process called In-Situ Semi-Preg (ISSP) has the potential to present similar processing and capital equipment cost reductions as semi-preg materials and the resin film infusion process.


text:
Q: Guava Return keys with value above some threshold I have this code to take a map and sort it by key
I then reverse the map to get them with the largest elements first.
Ordering<String> valueComparator =
       Ordering.natural().onResultOf(Functions.forMap(WordMap))
                         .compound(Ordering.natural());

WordMapSorted = ImmutableSortedMap.copyOf(WordMap,
                                  Collections.reverseOrder(valueComparator));

I'd like to know two things

*

*How can I get only the keys with a value above 10? I feel like given the sorting with guava there should be an easy way to specify a cutoff point (since once you reach a value below the threshold, you simply get all the items before it)

*How can I get the first 100 entries in the map (still in the form of a map). I know I can just get an array of keys and get the first 100, but I want the first 100 map entries. I know that normally a map has no order, but in this case it was sorted and made immutable so it does have order.

A: First observation: there's no need to use Collections.reverseOrder(valueComparator), when you can just use valueComparator.reverse().
1 requires some trickiness:
int index = Collections.binarySearch(WordMapSorted.values().asList(), 11);
index = (index >= 0) ? index : -index - 1;
// the elements at and after index have value strictly greater than 10
return WordMapSorted.keySet().asList().subList(index, WordMapSorted.size());

2 is doable like so:
WordMapSorted.headMap(WordMapSorted.keySet().asList().get(100));


text:
\section{Introduction}
  Non-thermal particle tails in particle energy spectra are evidence for a selective acceleration process that chooses to accelerate some particles but not most. The question to be asked of any acceleration model is which particles are selected and which are not. Shock acceleration, while it clearly selects only a minority of particles to be accelerated to very higher energies  [presumably the ones that already have a higher than average energy (Eichler, 1979c)], is remarkably equitable in regard to the different ion species. While there is modest enhancement of heavy elements, much of the differences in abundances from normal solar composition [e.g. correlation with first ionization potential (FIP)], can be attributed to "chemical" adjustment of the underlying composition of the thermal plasma.  (For example, any  electromagnetic separation of ions from neutrals could differentiate low and high FIP species from each other in partially ionized plasma. In the case of anomalous cosmic rays, the bias towards high FIP species is traced to the "pre-injection" they enjoy when the solar UV suddenly ionizes them after they have penetrated the solar wind in their neutral state. When this happens, they become the most energetic particle species in the solar wind plasma, and are more easily picked up by the shock acceleration mechanism.)

 In impulsive solar energetic particle (SEP) events, $^3$He  is often dramatically enriched relative to $^4$He nuclei. The $^3$He nuclei are believed to also receive an initial boost  - due to their resonance with ion-cyclotron waves (Fisk 1978) - but $^3$He-rich flares are not associated with shocks, and are generally smaller than shock-associated flares. Rather, it was proposed (Eichler 1979b, hereafter E79) that the $^3$He ions continue their acceleration by cyclotron damping turbulence as it cascades to smaller scales. Because the $^3$He nuclei have received a sufficient amount of pre-acceleration, they  have  larger gyroradii than protons,  (besides having a slightly smaller charge to mass ratio, which would be true of any heavy ion species). They need only a factor of $\sim 3$ increase in velocity to comfortably meet this criterion. At the scales where thermal or epithermal ions damp Alfven wave turbulence as it cascades to smaller spatial scales, the turbulence is a steeply decreasing function of wavenumber k, so that the $^3$He ions, which cyclotron resonate at the lower k, resonate with turbulence of  a much larger amplitude  and are preferentially accelerated. It was noted in E79 that extremely heavy elements would also experience highly preferential acceleration because they are not completely stripped. For example Fe$^{+10Q_{10}}$ has a gyroradius, at a given velocity, of $5.6Q_{10}$ times that of ions, and $2.8Q_{10}$  times that of $^4$He. An ultraheavy with $A\sim 200$ would have at most slightly more charge than iron, and would have a gyroradius that is more than 10 times that of protons of the same velocity. (Note that long wavelength magnetosonic waves tend to bring all ion species to the same velocity in a collisionless plasma [Eichler, 1979a], so the assumption of equal thermal velocities is reasonable.) The basic idea in E79 has since been confirmed in simulations (Miller, 1998). Observations (Mason et al., 2004) indicate that ultraheavies are indeed significantly enriched, even relative to iron, in $^3$He-rich flares. On the other hand, there are also energetic protons; apparently protons are not completely shut out of the acceleration process.

Formal expressions for the rates of particle diffusion in pitch angle and in momentum have been given by Kennel and Engelman (1966) and also by Lee and Volk,  (1975), Bogdan et al (1991) and Schlickeiser and  Achatz  (1993). The discussion below will be self-contained, however, with emphasis on particle diffusion in energy space. It will be assumed that particle velocities greatly exceed the Alfven velocity, so that the energy gain rate is slower than the pitch angle diffusion rate, and pitch angle distribution is therefore nearly isotropic.

The theory of cascading Alfven wave turbulence was revolutionized by Sridhar and Goldreich (1994), who noted that in the limit of sharp resonance the three wave process (symbolized by  ${\bf k_1 +k_2 \rightarrow k_3},\,  \omega_1 + \omega_2 \rightarrow \omega_3$)  invoked by Kraichnan (1966), the basis for the previously popular picture of cascading turbulence, does not  in fact take place. They further noted that, when interacting waves 1 and 2 are oppositely propagating, the four wave interaction $\bf{k_1 +k_2 \rightarrow k_3 +k_4},\,  \omega_1 + \omega_2 \rightarrow \omega_3 +\omega_4$ leaves  the parallel components of ${\bf k_1}$ and ${\bf k_2}$ unchanged, i.e. $k_{1,\parallel} = k_{3,\parallel},\, k_{2,\parallel} = k_{4,\parallel}$, and they conjectured on this basis that the turbulence would cascade more quickly in the perpendicular direction of $\bf k$-space, leading to tubular Alfven turbulence with $k_{\perp} \gg k_{\parallel}$.

In this paper, in sections 2 and 3  [see also Chandran (2000)],  it is noted that the tubular feature of  Alfven turbulence   would significantly affect the nature of the resonant cyclotron particle acceleration  because a particle whose parallel motion is in resonance with the wave motion would, for most pitch angles, pass through many perpendicular wavelengths, leading to a rapidly changing direction of the electric field that accelerates the particle. This causes the acceleration to be less efficient for low rigidity particles.  On the other hand, it is also  noted here that the acceleration becomes even more selective in favor of high rigidity particles and therefore favors  partially ionized heavy elements, and especially ultraheavy elements. It is shown that the acceleration time is constant in energy, leading to exponential growth in the energy content of superthermal particles, and with a faster growth time for partially ionized heavy ions.   In sections 4 and 5, comparison with observations is made, and it is argued that observations of impulsive solar flares is consistent both with dramatic enhancement of high rigidity ion species and with low overall efficiency, so that cascading turbulence remains an attractive  candidate for impulsive solar energetic particle events.

 \section{Basic Idea}

 The mathematical illustration of selective acceleration given in E79 was  simplified.  It was assumed that turbulent energy cascades monotonically to high k at a rate $dk/dt$ that is a given function U(k) of k, which would give a cascade time of $k/{dk\over dt} =  k/U$. In fact, the cascading is a non-linear process and its rate is more correctly expressed in proportion to the dimensionless amplitude of the turbulence ${\cal W}(k)k/(B^2/8\pi)$. However, Sridhar and Goldreich (1995) have argued that the level of turbulence adjusts itself so that the cascade time is $t_{cascade}\sim 1/v_A k_{\parallel}$, in which case  U(k) can indeed be expressed independently of  ${\cal W} (k) dk$.

 The condition for cyclotron resonance is that $k_{\parallel}v_{\parallel} -\omega - n\omega_c=0$. For non-relativistic particles, this is a condition on $v_{\parallel} \sim [E/m]^{1/2}$. Let us focus on the n=1  resonance, and for simplicity, on any single species of ions. Highly super-Alfvenic  particles, $v_{\parallel}\gg v_A= k_{\parallel}^{-1} \omega$  of velocity $v \sim k_{\parallel}^{-1} \omega_c$ satisfy the resonance condition so the spectral energy density can be expressed as a function of the parallel velocity of the particles that resonate with it, i.e.  ${\cal W} (k) dk \equiv W( v_{ \parallel})dv_{ \parallel}$. The cascade time at a given wavenumber is then naturally expressed in terms of the velocity of the resonant particles as $t_{cascade} = v_{\parallel}/v_{A}\omega_c$.

 The  average diffusion of particles in energy space due to mode k is given by \\${ D_{EE} = <[\Delta E]^2/\Delta t>\eta_{\parallel}\eta_{\perp}\sim \, <(dE/dt)^2>\eta_{\parallel}\eta_{\perp}\Delta t}$ where $\Delta E$ is the correlated energy change over a correlation time $\Delta t$, and where $ \eta_{\parallel}\eta_{\perp}$ is the fraction of particles that remain in phase with the wave over the correlation time. The energy change is due to electric fields in the observer frame acting along the particle velocity. For Alfven waves, the electric field  ${\bf \cal E}$  is perpendicular to the magnetic field, so  $dE/dt = ev_{\perp}\cdot {\cal E}$ and the phase correlation time,  $\tau_c$,  of the wave over which resonant particles are affected is, according to  Sridhar and Goldreich, $\tau_c \sim 1/k_{\parallel }v_{A}$. The electric field  ${\cal E}_k$ due to the {\bf k}th mode is given by ${\cal E}_k = {\bf u_k  \times  B} \simeq u_k B_o$. The fraction $\eta_{ \parallel}\sim(\Delta v/v)$ of particles at $v_{\parallel } \sim \omega_c/k_{ \parallel}$ that resonate with the wave is determined by the criterion that they gain or  lose a phase of less than $\pi/2$ over the correlation time $\tau_c$ (i.e. $\Delta v \tau_c = \pi/2k_{\parallel}$), and, assuming $\tau_{c} \sim \tau_{cascade}$, $\eta_{ \parallel}\sim v_A/v_{\parallel}$.  Of those that are within the parallel resonance,   the fraction  $\eta_{\perp} = 1- \cos\theta $ of particles whose pitch angle $\theta$ is small enough that their gyration does not carry them across a distance of more than $1/2\pi$ of a perpendicular wavelength $2\pi/k_{\perp}$, i.e. those obeying $k_{\perp} r_g \sim {k_{\perp} v_{\perp}\over \omega_c } \lesssim 1$, can be small when $k_{\perp} \gg k_{\parallel}$, which lends added importance to the modes $k_{\perp} \lesssim k_{\parallel}$.

Finally we can write

 \begin{equation}
 D_{EE}
  = e^2 B_o^2  \sum_k u_k^2 v_{\perp}^2{\eta_{\perp}}/c^2k_{\parallel }v_{ \parallel}\simeq  \sum_k m  u_k^2 mv_{\perp}^2{\eta_{\perp}}\omega_c.
 \end{equation}
 Below we will be concerned with nearly isotropic particle distributions, but with anisotropic wave spectra, so we have assumed in the above that parallel and perpendicular velocities are typically of the same order for most of the particles, and, in equation (1), $v_{\perp}^2$ can be replaced in any pitch angle average by $2v^2/3 =  2v_{\parallel}^2$. The factor $\eta_{\perp}$ essentially selects out the modes $k_{\perp} \lesssim k_{\parallel}$ in the sum, as will be seen below.

The acceleration time $\tau_a = E^2/D_{EE}$  is typically  longer than the cascade time  $\tau_{cas}=v/v_A\omega_c$ by the factor $(v/v_{\perp})^2 (v/u)^2(v_A/v  \eta_{\perp})$. The power  per thermal proton mass absorbed by a resonant particle of velocity $v_{\parallel}$ and perpendicular velocity $v_{\perp}$, $v_{\perp}^2 u^2 n(v_{\parallel},v_{\perp})\omega_c/v^2 n_{th}$, exceeds the  cascade power per thermal proton  mass, $u^2v_A\omega_c/v_{\parallel}$  only if the ratio   $n(v_{\parallel}, v_{\perp})/n_{th}$ of the number density of resonant particles, $n((v_{\parallel},v_{\perp})$, to the total, $n_{th}$, exceeds
 $(v_A/v)(v/v_{\perp})^2 /\eta_{\perp}$. This condition cannot be met unless the fraction of resonant particles exceeds $v_A/v$.  Unless the plasma is weakly magnetized or the resonant particles are already highly superthermal, it does not appear that the cascading turbulence could be damped until it cascades down nearly to scales where it could damp on the tail of the distribution of typical thermal ions.

 Let us  then assume  the turbulence cascade proceeds as in Sridhar and Goldreich (1995) without  too much energy absorption   by resonant  particles.  The 3-dimensional energy spectrum, by their arguments, is given by ${\cal W}(k_{\perp},k_{\parallel})\propto k_{\perp}^{-10/3}g(k_{\perp}^{2/3}k_m^{1/3}/k_{\parallel})\equiv k_{\parallel}^{-5}f(k_{\perp}^{2/3}k_m^{1/3}/k_{\parallel})$ where $k_m$ is the maximum wavenumber at which the turbulence is reasonably isotropic, and g and f are functions  that decline sharply beyond an argument of order unity.  This means that the wave energy $\int \int{\cal W}(k_{\perp},k_{\parallel})2\pi k_{\perp} dk_{\perp} dk_{\parallel}\sim W k_{\parallel}^3$ that is resonant with particles of energy $E \sim mv^2/2$ increases as ${\cal W}k_{\parallel}^3 \propto k_{\parallel}^{-2} \propto v_{\parallel}^2 \propto E$. In deriving this result we have taken  the integral over $k_{\perp}$  from $k_{\perp}=0$ only out to to $k_{\perp} =  k_{\parallel}$. The reason for this is that waves with $k_{\perp}\gg k_{\parallel}$ do not effectively accelerate the particles because their characteristic gyroradius $v_{\parallel}/\omega_c$, as defined by the resonance condition, cuts across many perpendicular wavelengths for pitch angles of order unity. (Alternatively, we could have considered particles with very small pitch angle, $\theta \le k_{\parallel}/k_{\perp}\ll 1$, but they  comprise only a small fraction of the total number of particles at a given energy [i.e. $\eta_{\perp} \ll 1$], and also absorb  less energy because they have such a small $v_{\perp}$. So in the end, most of the energy is absorbed by particles with larger pitch angles [$\eta_{\perp} \sim 1$] from the more parallel propagating waves.)

 The energy diffusion rate $D_{EE}$ then, by equation (1), scales as $EW(k_{\parallel},0)k_{\parallel}^3 \omega_c \propto E k_{\parallel}^{-2} \omega_c $, where $ k_{\parallel} = \omega_c/v_{\parallel } \sim  \omega_c/v$.  The acceleration time $E^2/D_{EE}$ is then independent of energy within any given ion species.  This means that the typical particle energy grows exponentially with time in the absence of escape.

 Significantly, it also implies that the acceleration time for partially ionized heavy elements is {\it shorter} than for protons  because, although their cyclotron frequency is smaller by a factor Q/M (where Q and M are in units of protons charge and proton mass respectively), the factor $k_{\parallel}^{-2}$ is larger by $(M/Q)^2$.  Altogether, the acceleration rate of a partially ionized heavy atom is $M/Q$ times that of a proton. Because the energy grows exponentially in time, the enhancements of ultraheavy elements at high energies can be huge.

\section{A Formal Derivation of the Acceleration Rate}
 We now present a more formal calculation justifying the above arguments:  The energy diffusion rate is given by
 \begin{equation}
 D_{EE}({\bf v})=<\Delta E(t)>^2/t =  <\int_0^t q{\bf v\cdot {\cal E}}{(\bf x[t^{\prime}]},t^{\prime}) dt^{\prime}><\int_0^t q {\bf v \cdot {\cal E}(x[t^{\prime \prime}]},t^{\prime \prime}) dt^{\prime \prime}>/t
 \end{equation}
 where
 \begin{equation}
 {\bf x[t]} = {\bf x_o} + v_{\parallel} t {\bf \hat z} + r_g\sin(\omega_c t + \phi_o){\bf \hat x}+ r_g\cos(\omega_c t + \phi_o){\bf \hat y},
  \end{equation}
   \begin{equation}
 \bf v(x[t]) = v_{\parallel}  {\bf \hat z} + r_g\omega_c\cos(\omega_c t + \phi_o){\bf \hat x}- r_g \omega_c \sin(\omega_c t + \phi_o){\bf \hat y},
  \end{equation}
  \begin{eqnarray}
  {\cal E}(x,t)={\it Re}\int\int \int {\cal E}_{\bf k} e^{i({\bf k\cdot x -\omega t +\phi_k(t))} }d^3k \\
  ={\it Re}\int\int \int {\bf {-u({\bf k})}\over c} \times {\bf B_o} e^{i({\bf k\cdot x -\omega t +\phi_k(t))} }d^3k
 \end{eqnarray}
and

\begin{eqnarray}
{\bf v \cdot {\cal E}_k} = B_o ( u_x(\bf k) v_y -u_y({\bf k}) v_x)e^{i({\bf k\cdot x -\omega t +\phi_k(t))}}/c \\ = B_o r_g \omega_c [u_x (k) \cos(\omega_c t + \phi_o)+ u_y(k)\sin(\omega_c t + \phi_o)]e^{i({\bf k\cdot x -\omega t +\phi_k(t))}}
\end{eqnarray}

We assume  that the Alfven turbulence is axisymmetric around $\bf \hat z$  so that we can without loss of generality consider an Alfven mode with $\bf k$  in the zx plane. In the Alfven mode, $u\parallel {\bf \hat y}$, and
\begin{eqnarray}
{\bf v \cdot {\cal E}_k} = B_o [u_y({\bf k}) v_x)e^{i({\bf k\cdot x} -\omega t +\phi_k(t)]}/c \\= B_o r_g \omega_c [u_x ({\bf k}) \cos(\omega_c t + \phi_o)]e^{i({\bf k}\cdot{\bf x} -\omega t +\phi_k(t))}/c.
\end{eqnarray}
Using the identities
\begin{equation}
e^{iz\sin\phi} =  \sum_{n=-\infty}^{\infty}J_n(z)e^{in\phi},\end{equation}
and
  \begin{equation}{2n\over z}J_n(z)=J_{n-1}(z)+J_{n+1}(z),
\end{equation}
 we can write
\begin{eqnarray}
{\bf v \cdot {\cal E}_k} = B_o r_g \omega_c u({\bf k})
\cos(\omega_c t +\phi_o)]
e^{i({ k_{\parallel}v_{\parallel}}t+k_{\perp}r_g sin(\omega_ct+\phi_o) -\omega t +\phi_k(t))+i{\bf k\cdot x_o}}/c\\
{\bf v \cdot {\cal E}_k}
={1\over2} B_o r_g \omega_c u({\bf k})
[e^{i(\omega_c t +\phi_o)]} + e^{-i(\omega_c t +\phi_o)}]
e^{i({ k_{\parallel}v_{\parallel}}t+k_{\perp}r_g sin(\omega_ct+\phi_o) -\omega t +\phi_k(t))+i{\bf k\cdot x_o}}/c\\
= {1\over2} B_o r_g \omega_c u(k)\sum_{n=-\infty}^{\infty}[J_{n-1}(k_{\perp}r_g) + J_{n+1}(k_{\perp}r_g)]
e^{i[({\bf k_{\parallel}v_{\parallel}}
+n\omega_c -\omega )t +n\phi_o +\phi_k(t)]+i{\bf k\cdot x_o})
}/c\\
=  B_o  \omega_c u(k)k_{\perp}^{-1}\sum_{-\infty}^{\infty} n J_n(k_{\perp} r_g )
e^{i({\bf k_{\parallel}v_{\parallel}}
+n\omega_c -\omega )t +n\phi_o+\phi_k(t))+i{\bf k\cdot x_o})
}/c
\end{eqnarray}

We invoke axisymmetry of $u({\bf k})$ around the z direction and  write

\begin{equation}
\int \int \int { u^2}({\bf k}) e^{i({\bf k\cdot x }-\omega t +\phi_k(t)) }d^3k = \int \int u^2(k_{\perp},k_z) e^{i({\bf k\cdot x }-\omega t +\phi_k(t)) }2\pi k_{\perp} dk_{\perp}dk_{\parallel}
\end{equation}
whence

\begin{eqnarray}
 D_{EE}({\bf v})t &=& \int dk_{\parallel}\int 2\pi k_{\perp}dk_{\perp} \nonumber <\int_0^t d( t^{\prime}+ t^{\prime \prime})/2 \int_0^t d( t^{\prime}- t^{\prime \prime})q^2  \omega_{c}^2  {u^2({ k}) B_o^2\over k_{\perp}^2 c^2 } e^{i[({\bf k_{\parallel}v_{\parallel}}
 -\omega )(t^{\prime}- t^{\prime \prime} ) + \phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})] }\nonumber \\
&&  \big(\sum_{-\infty}^{\infty} n^2 J_n^2(k_{\perp} r_g )  + \sum_{-\infty}^{\infty} \sum_{m\neq n} nm J_n( k_{\perp} r_g )J_m (k_{\perp}r_g)
e^{i n\omega_ct^{\prime\prime}-i m \omega_ct^{\prime} }\big)>
 \end{eqnarray}

 Note that  $ nt^{\prime\prime}-mt^{\prime}=(n-m)t^{\prime\prime} + m(t^{\prime\prime}-t^{\prime})$ which means that for $n\neq m$, the integrand oscillates over $ t^{\prime\prime}$, and does not contribute significantly to $D_{EE}$. So we henceforth ignore the terms proportional to $J_n( k_{\perp}r_g)J_m(k_{\perp}r_g )$ for $n\neq m$.

 Assuming that  the correlation time of $\phi_{\bf k} (t)$ is small compared to t, the limits of the $ (t^{\prime}- t^{\prime \prime})$  integral can be taken to be $[-\infty, +\infty]$. We can view the term

 \noindent
 $\int_{-\infty}^{+\infty}  d(t^{\prime}- t^{\prime \prime}) e^{i( k_{\parallel} v_{\parallel}+n\omega_c -\omega)(t^{\prime}-t^{\prime \prime}) +i[\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})] } $
  as a Fourier component of $e^{i[\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})]}$, and the ensemble average,  $<\int_{-\infty}^{+\infty}  d( t^{\prime}- t^{\prime \prime})e^{i( k_{\parallel} v_{\parallel}+n\omega_c -\omega)(t^{\prime}-t^{\prime \prime}) +i[\phi(t^{\prime})-\phi(t^{\prime\prime})] } >$, as a Fourier component of  $ <e^{i\phi[(t^{\prime})-\phi(t^{\prime\prime})]}>$.

 If the randomization of phases proceeds as diffusion in $\phi_k$ space, then the probability distribution of $[\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})]$
is given by
\begin{equation}
p[\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})]=(2\pi)^{-1/2} exp  \left([\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})]^2/D_{\phi(k), \phi(k)}[t^{\prime}-t^{\prime\prime}] \right),
\end{equation}
then
 \begin{equation}
  <e^{i[\phi(t^{\prime})-\phi(t^{\prime\prime})]}> = \int p[\phi_{\bf k}(t^{\prime})-\phi_{\bf k}(t^{\prime\prime})]e^{i[\phi(t^{\prime})-\phi(t^{\prime\prime})]}d[\phi(t^{\prime})-\phi(t^{\prime\prime})]  = exp[-|\Gamma  (t^{\prime}-t^{\prime\prime})|],
 \end{equation}
 where $\Gamma = D_{\phi(k), \phi(k)}/4$, and
 \begin{equation}
< \int_{-\infty}^{+\infty}  d( t^{\prime}- t^{\prime \prime})
 e^{i(k_{\parallel}v_{\parallel}+n\omega_c -\omega )( t^{\prime}- t^{\prime\prime})+i[\phi(t^{\prime})-\phi(t^{\prime\prime})]}>
 = {2\Gamma\over[(k_{\parallel}v_{\parallel}
+n\omega_c -\omega )^2 + \Gamma^2 ]}
 \end{equation}

 If $\Gamma \sim k_{\parallel}v_{\parallel}$, as posited by Goldreich and Sidhar, then we can make the approximation
 \begin{equation} {\Gamma\over(k_{\parallel}v_{\parallel}
+n\omega_c -\omega )^2   + \Gamma^2 }\simeq \pi \delta( k_{\parallel}v_{\parallel}
+n\omega_c -\omega ). \end{equation}

Using the above, we now write
\begin{equation}
D_{EE}({\bf v}) = 2\pi \int dk_{\parallel}\int 2\pi k_{\perp}dk_{\perp} q^2  \omega_c^2  {u^2({k_{\parallel}, k_{\perp}}) B_o^2\over k_{\perp}^2 c^2 }\\
 \sum_{-\infty}^{\infty} n^2 [J_n^2(k_{\perp} r_g )  \delta({ k_{\parallel}v_{\parallel}}
+n\omega_c -\omega )
\end{equation}

We now simplify further by assuming that $v\gg v_A$, so that $ \omega = k_{\parallel}v_A$  is negligible compared to $ k_{\parallel}v$. Then

\begin{eqnarray}
D_{EE}({\bf v}) \simeq 2\pi v_{\parallel}^{-1}\int 2\pi k_{\perp}dk_{\perp} q^2  \omega_c^2  {B_o^2\over k_{\perp}^2 c^2 }
 \sum_{-\infty}^{\infty} n^2 u^2(n\omega_c/v_{\parallel}, k_{\perp})J_n^2(k_{\perp} v_{\perp}/\omega_c )
\end{eqnarray}

In the theory of  Sidhar and  Goldreich, $u^2(k_{\parallel},k_{\perp})$, which is proportional to the wave energy,  declines steeply for $k_{\perp}\gg k_* \equiv k_{\parallel}^{3/2}l^{1/2}$ where $l$ is the scale at which $u_{\perp}\sim v_A$, i.e. where $\rho u^2(k_{\parallel},k_{\perp} )k_{\parallel}k_{\perp}^2 \sim B_o^2/8\pi$. For $k_{\perp}\le k_{\parallel}^{3/2}l^{1/2}$, the quantity  $u^2$ should be roughly  constant in $k_{\perp}$, as it is established by mode coupling which should equalize the energy among modes, and it should scale as $k_{\parallel}^{-5}$.\footnote{or equivalently $k_{\perp}^{-10/3}$, given  that  the wavenumbers for a given eddy scale as  $k_{\perp}\propto k_{\parallel}^{3/2}$.} The factor $J_n^2(k_{\perp} v_{\perp}/\omega_c ) $, $n\neq 0$, peaks when its argument is of order unity, and declines asymptotically at larger arguments as $k_{\perp}^{-1}$,  so the integrand declines at  large $k_{\perp}$  at least as fast as $k_{\perp}^{-2}$. For resonant ions obeying $v_{\perp}\lesssim v_{\parallel}\sim \omega_c/k_{\parallel}$, the decline in $J_n$ begins at smaller $k_{\perp}$ than the decline in $u^2$, so we can take $u^2(k_{\parallel}, k_{\perp})$ to be approximately constant in $k_{\perp}$ over the significant range of the integral.

So
\begin{eqnarray}
u^2(l^{-1}, l^{-1})l^{-3}
\simeq v_A^2
\end{eqnarray}
and, for $k_{\perp}\lesssim k_{\parallel}^{3/2}l^{1/2}$,
\begin{eqnarray}
u^2(k_{\parallel}, k_{\perp})
\simeq v_A^2l^{3} |k_{\parallel}l|^{-5}
\label{usquared}
\end{eqnarray}
whence

\begin{eqnarray}
D_{EE}({\bf v}) \simeq 4\pi v_{\parallel}^{-1} q^2  \omega_c^2  {B_o^2\over   c^2 }
 \sum_{1}^{\infty}n^2 \psi_n u^2(n\omega_c/v_{\parallel}, \omega_c/v_{\perp}) \nonumber \\
\simeq  4\pi v_{\parallel}^{-1} q^2  \omega_c^2  {B_o^2\over   c^2 }
 \sum_{1}^{\infty}n^2\psi_n v_A^2 l^3 (v_{\parallel}/n\omega_c l )^5 \nonumber \\
 =  4\pi mv_A^2 mv_{\parallel}^2 [v_{\parallel}/l\omega_c]^2 \omega_c \sum_1^{\infty}n^{-3}\psi_n
 \simeq  4\pi  (mv_{\parallel}^2)^2 [v_A/l\omega_c]^2 \omega_c
 \label{deeb}
\end{eqnarray}
 where $\psi_n \equiv 2\pi \int_0^{\infty}J_n^2(x) d\ln x$.\footnote{ Although this integral would diverge logarithmically for n=0, the n=0 mode is erased by the $n^2$ coefficient.  The integral  is well defined for $n\ge 1$. }
[In contrast to the above, equation (9) of Chandran (2000) assumes that $u^2(k_{\parallel}, k_{\perp}) = 0$ for  $k_{\perp}\lesssim k_{\parallel}^{3/2}l^{1/2}$. This would seem to neglect the most important modes, which obey  $k_{\perp} \sim k_{\parallel}$, and hence  $k_{\perp}\ll k_{\parallel}^{3/2}l^{1/2}$.]

 Equation (\ref{deeb}), valid for $k_{\parallel} \gtrsim 1/l$, implies,  as argued qualitatively in the previous section,  that the acceleration time $t_{acc}$, over which $D_{EE}t_{acc}= E^2$, is constant, so particles subjected to this acceleration gain energy exponentially  in time. As argued qualitatively in the previous section, the acceleration rate at a given velocity is {\it inversely} proportional to the cyclotron frequency $\omega_c$, so that partially ionized heavy ion species are preferentially accelerated.  For the larger spatial scales,  $k_{\parallel} \lesssim 1/l$, on the other hand,  strong, isotropic Kolmogoroff turbulence is probably be the more appropriate description, and  2nd order Fermi acceleration by cyclotron damping would proceed at a rate  $u(r_g)^2/v^2\tau(r_g)$ where $ u(r_g)$ is the turbulent velocity at the scale of $r_g$, and $1/\tau(r_g)$ is the coherent interaction time with an "eddy" and is equal to $\omega_c$.\footnote{We assume that the strong turbulence randomizes the ion's motion on the timescae of $\omega_c^{-1}$.  If the particle's velocity exceeds that of the turbulence, as we may assume for superthermal particles in subsonic turbulence, then this timescale is shorter than that of the fluid motion.}  For a given $\omega_c$, and for the Kolmogoroff spectrum $u(r_g)\propto r_g^{1/3}$, the acceleration rate varies as $r_g^{2/3}\omega_c/v^2  \propto v^{-4/3} \omega_c^{1/3}$. This does {\it not} favor species with velocity or large M/Q. The cascade  model of Goldreich and Sidhar, on the other hand,  gives  an acceleration rate for  test  particles that is {\it inversely} proportional to  $\omega_c$, thus favoring partially ionized ultraheavies among particles over lower Ze/M ions species at a given velocity, in contrast  to isotropic turbulence, in which the acceleration rate of  a test  particle at  a given velocity is proportional to $\omega_c^{1/3}$.

We have not yet taken into account the backreaction of  the cyclotron damping on the turbulence,  which would surely result in the presence of particles that gain energy exponentially with time. This is  considered in the next section.

\section{Backreaction of Particles on the Alfvenic Turbulence}

Alfvenic turbulence without damping  is difficult to solve formally,  and even more difficult when damping is included.  We  may identify several timescales in the problem  associated with   wave-wave and wave-particle interactions on a given spatial scale:  the cascade times $t_{cascade,\perp}$ and $t_{cascade,\parallel}$ in the $k_{\perp}$ and $k_{\parallel}$  directions, respectively,    and the wave damping timescale due to particle acceleration. Goldreich and Sridhar  argued that, at all spatial scales smaller than $l$ but larger than the dissipative range, the strengh of the turbulence reached a level where $t_{cascade,\perp}\sim t_{cascade,\parallel} \sim  1/k_{\parallel} v_{\parallel}$.  They called this approximate equality between parallel and perpendicular cascade times "critical balance".  Their argument is that resonant three-wave coupling  among Alfven waves is forbidden and the cascade in $k_{\parallel}$  can come about only if there is sufficiently strong mode coupling to broaden mode coupling resonance. Cascade  in the parallel direction,  according to this argument,  must "wait"   for perpendicular cascade.  A similar argument could be made  in the reverse  direction -  that  perpendicular cascade  cannot proceed  more rapidly than the time $1/k_{\parallel}v_A$ required  for the waves to feel  the parallel dimension,   because two dimensional turbulence,  having too many conserved quantities of motion,  does not cascade   to high   wavenumbers.

In E79, where the distinction   between perpendicular and parallel cascade was not made, it was argued  that in steady state, (what would be later called) critical balance should exist between the  turbulent cascade time and the damping time, so that just enough turbulence could trickle down to small spatial scales  to resonantly accelerate low energy ions,  just enough to supply the energetic  population that damps the turbulence.  The simplified mathematical  derivation of this is  based on a simple cascade  model in which there is an ordered flow of energy from low k to high k,   according to the spectral  evolution equation
 \begin{equation}
\frac{{\partial\cal W}(k)}{\partial t}
= -\frac{\partial}{\partial k}
\left({{\cal W}(k)}U(k)\right) -{\cal D}(k).
 \end{equation}
 Here  ${\cal W} (k) dk$ is the energy density in turbulence in waves between  the wavenumbers k and k+dk,  $U(k)\sim k/t(k)$  is the k-velocity with which turbulent energy cascades through scale $k$ ( from $\sim k$ to $\sim 2k$ over time t($k$), say).
 $ {\cal D }(k)$ is the rate at which wave energy is damped by the particles. Let us  assume for the purposes of analysis, as is E79,
that there is a dominant ion species.  Defining
  $W(E)dE \equiv {\cal W}(k)dk$, where E is the ion energy that cyclotron damps waves at wavenumber k; i.e. $k^{-1}=r_g\equiv mcv/eB=(2E/m)^{1/2}$,  we can write

\begin{equation}
\frac{\partial  W(E)}{\partial t}
=  \frac{\partial}{\partial E}
\left[ W(E)U(E)\right] - \left[ \frac{d W(E)}{dt}\right]_{damping}.
\label{dwdt}
\end{equation}
where $E/U(E) \sim  t_{cascade}$,
and the spectral  evolution of the particles obeys
\begin{equation}
{\partial  f(E) \over \partial t} = \frac{\partial}{\partial E} \left[ \frac{dW(E)}{dt}\right]_{damping}
\label{dfdt}
\end{equation}
Now suppose \newline
$ \left[\frac{dW(E)}{dt}\right]_{damping}=W(E)\rm d(E){\partial  f \over \partial E}$,
 where the energy diffusion coefficient, $W(E)\rm d(E)\equiv D_{EE}$,  is written in a form that is manifestly proportional to the wave energy density $W(E)$.  The steady state solution  to equations (\ref{dwdt}) and (\ref{dfdt}) is then

\begin{equation}
W(E) = U^{-1} P(E_{max})exp\left(-\int_E^{E_{max}} {\rm d}(E^{\prime}){\partial  f \over \partial E^{\prime}}U^{-1}  dE^{\prime}\right)
\label{wofe}
\end{equation}
where $P(E_{max})$ is the turbulent power per unit volume flowing in from  the largest scale that can accommodate the particles before they escape.
and
\begin{equation}
f(E) = \int_E^{E_{max}} {U(E)\over \rm d(E)E} dE
\end{equation}

This solution is time independent and describes  a constant upward flux  $\cal F$ of particles in energy space. Because the exponent in the right hand side of equation (\ref{wofe}) is $\ln E$, the solution describes a depletion of cascade power, $P(E)= W(E)U(E)$, as the wave energy cascades to smaller spatial scales  (where it is resonant with particles of smaller E), that is a fixed fraction of the total; i.e.
\begin{equation}
dlnP(E)/d lnE = 1
\end{equation}
and
\begin{equation}
P(E)=E {\cal F}.
\label{pofe}
\end{equation}

The time-dependent analogue of this solution is, to a fair approximation, the same as in the above, but with $ E_{max}$ replaced by $E_m(t)$,s  where $E_m(t)$ is defined by the condition that the total energy in the particles $\int_0^{E_m(t)}f(E)EdE$ and in the turbulence $\int_{0}^{E_{max}}W(E)dE$ equals the total amount of accumulated energy $P(E_{max})t$ that has been introduced into the system over time t.

 Equation (\ref{pofe}) implies that the damping rate of wave energy by the particles is equal to the cascade rate, i.e. that the damping and cascading are in "critical balance". This follows from the fact that the flux removed from the turbulence at a given spatial scale by the resonant particles of corresponding energy E is proportional to E, so $P(\alpha E) = \alpha P(E)$.  The resonant particle absorb much of the energy at any given scale but they allow just enough to cascade through to smaller scales so that the acceleration of less energetic particles is, in turn,  just enough to replace them as the acceleration moves them to higher energy bins.

 Do we then conclude that, in a 3D description of wave energy cascade, parallel cascade, perpendicular cascade,  and wave damping all proceed at the same rate? Unfortunately there is one complication:  that only waves  with $k_{\perp} \lesssim k_{\parallel}$  are efficiently damped by the  particles,  whereas most of the wave energy, according to Goldreich and Sridhar,  cascades perpendicularly to $k_{\perp} \gtrsim k_{\parallel}$. The possibility must be considered that wave energy can then make an "end run" at $k_{\perp}\gg k_{\parallel}$ around the resonant particles  and penetrate to high wavenumber without losing much energy to the particles.

 There  are, {\it a priori}, at least two possible resolutions of this:

 1) Enough wave energy is backscattered to lower $k_{\perp}$, because of the energy sink there, so that most of it is absorbed by the particles before cascading to high k.   In this case the one dimensional approximation  may retain validity, and the above analysis would apply with $\int W(E)dE =  \int \rho u^2(k_{\perp},k_{\parallel}) dk_{\perp}dk_{\parallel}$, and $U(E) = E k_{\parallel}v_A $. Using equation (\ref{usquared}), we can write
 \begin{equation}
\int W(E)dE = \int \rho u^2(k_{\perp},k_{\parallel}) d^2k_{\perp} dk_{\parallel} \sim u^2(k_{\perp},k_{\parallel}) k_{\parallel} k_{*\perp}^2 \sim   \rho v_A^2/k_{\parallel} l
 \end{equation}
where $k_{*\perp}\equiv (k_{\parallel}l)^{1/2}/l$ is the maximum perpendicular wavenumber of the energy-rich modes at a given $k_{\parallel}$.

 2) At $k_{\parallel} \gg 1/l$, most of the energy cascades as it would in the absence of damping by particles. In this case, the question is how such turbulence eventually damps  when its energy is to be found in the high $k_{\perp}$,  $k_{\perp} \gg  k_{\parallel}$. Does it damp on thermal particles or on non-thermal ones? Electrons or ions?

 For Alfvenic turbulence, it is easy to show that for $k \lesssim \omega_c/c$, most of the current, as measured in the lab frame, is borne by ions.  This means that by the time the turbulence cascades down to the scale of the ion gyroradius, strong magnetic turbulence is essentially heat, as the effective collision time of a typical current-bearing ion is of the order of the gyroperiod. This may be considered the damping scale of the Alfvenic turbulence, unless a population of ions with larger gyroradii coherently cyclotron damps the turbulence at larger  spatial scales.

 We may compare the  rates of cascade $\tau_{cas}^{-1} = k_{\parallel} v_A$ and of cyclotron damping. The analysis above indicates that the  inverse acceleration time for individual ions participating in cyclotron damping is $\tau_{acc}^{-1} \sim (v_A/l\omega_c)^2 \omega_c$, so the particles absorb energy at a rate of  $f(E)E^2\tau_{acc}^{-1} $, and the  wave energy damps on a  timescale of $\tau_{damp}=\tau_{acc} W(E)/f(E)E \simeq {(v_A/l\omega_c)^{-2} \omega_c}^{-1} [\rho v_A^2/f(E) E^2 ][k_{\parallel}l]^{-1} $.  Here we have used equation (\ref{usquared}) to substitute for $W(E)=u^2(k_{\parallel, k\perp})k_{\perp}^2k_{\parallel}$.  The ratio of cascade timescale $\tau_{cas}$ to  damping  time scale is then given by

 \begin{equation}
 {\tau_{cas}\over \tau_{damp}}=[v_A/l\omega_c][f(E) E^2/\rho v_A^2 ].
 \end{equation}

 In situations where the turbulence is powered by a stirring mechanism on spatial scales much larger than a thermal ion gyroradius, the quantity $ (v_A/l\omega_c) $ is much less than unity,  so if  $[f(E) E^2/\rho v_A^2 ]\lesssim 1$, then the turbulence,  even if well mixed by mode coupling into the regime $k_{\parallel}\gtrsim k_{\perp}$, cascades to scales of thermal gyroradius before  being damped by the tail of the thermal distribution.

  On the other hand, the ions at the thermal tail are accelerated exponentially in time, which means their energy content $ f(E) E^2$ grows significantly over a timescale of $(l/v_A)^2 \omega_c$. If the duration  of  the event responsible for the stirring and the collisional timescale are both much longer than this,  and if the particles do not escape before reaching significantly larger energies, then the particle distribution can  evolve to the point where $ {\tau_{cas}\over \tau_{damp}}\gg 1 $, and the turbulence is absorbed before it reaches scales of thermal gyroradii. Physically,  the requirement for this is that the mixing is such than it introduces more turbulent energy density over time than the {\it local} magnetic energy density, so that $[f(E) E^2/\rho v_A^2 ] \gg  l\omega_c/v_A \gg 1$.
  In a solar flare,  which is powered by magnetic energy, this is a significant constraint,  because one expects that the magnetic field energy would be released  and fully dissipated within several Alfven crossing times, and that enough magnetic energy would remain such that the final Alfven velocity would be within an order of magnitude of the original one.

  On the other hand, it is possible that a  region of strong magnetic field annihilation stirs ups the less magnetized neighboring  regions.  Consider, for example, a magnetic arch on the solar surface with a length scale L of $10^8$ cm,  an equipartition scale $l=10^7$ cm, a field strength of 300 G, and an Alfven velocity of $10^8$ cm s$^{-1}$. Then $\omega_c = 10^{6.5}$  and  the acceleration  time is
  $\tau_{acc} \sim [(v_A/l\omega_c)^2 \omega_c ]^{-1} \sim  10^{4.5}$s,  which is too long for a solar flare.
  For a neighboring region, however,
  take the parameters to be $L=10^8 \rm cm$, $B= 3$G, $v_A = 10^6$ cm s$^{-1}$, but let us still assume that the kinetic energy density $U_K$ is comparable to what it is within the strongly magnetized loop, i.e. $10^4$ times the magnetic energy $U_B$ in the less magnetized, surrounding region at scale L.  Assuming the kinetic energy at scale $l$ is, as in the Kolmogoroff spectrum,  $(l/L)^{2/3}$  of what it is at scale L, then  $l =  (U_B/U_K)^{3/2}L = 10^{-6}L = 10^2$ cm. The dimensionless parameter $ (v_A/l\omega_c)^2 \sim 10^{-1}$, and the acceleration timescale is only about 10 gyroperiods, $\lesssim 10^{-3}$ s. This equipartition length $l$, for a thermal velocity of $10^{7.5} v_{7.5}$ cm/s, $ v_{7.5}\lesssim 1$,  is not much greater than a thermal  ion gyroradius, and in fact,  less than the gyroradius of  a partially ionized ultraheavy. So it would then be reasonable to assume that the turbulence at larger scales is quasi-isotropic with $u \gtrsim v_A$, and that the particle acceleration and wave damping for resonant particles at these scales is described by equations (\ref{dwdt}) and (\ref{dfdt}), and that the  anisotropy  predicted by Sridhar and Goldreich does not set in significantly above a thermal ion gyroradius. Given that the  accelerated particles $E\lesssim 1$ MeV/nucleon, have energies only about $10^3$ above thermal energies $\sim 1 $ KeV/nucleon, there are not enough ultraheavies to significantly damp the turbulence, so that we need not consider their back reaction on the turbulence.  The fact that rare ultraheavies are enhanced even relative to iron in impulsive SEP events, despite the likely conclusion that they do not monopolize the energy budget, suggests that the turbulence is a steeper function of $k_{\parallel}$ than a simple Kolmogoroff spectrum. Yet it is possible that {\it all} of the ultraheavies are accelerated well beyond thermal energies. So perhaps a typical impulsive SEP event is properly parametrized somewhere between each of the two extreme examples  given just above. It is also possible that a large fraction of iron-like nuclei and preaccelerated species such as $^3$He are also picked up by the cyclotron damping mechanism and accelerated well beyond thermal energies. There are enough of them to possibly weaken the turbulence enough that it goes into the Sridhar-Goldreich regime, and at this point the situation would be sufficiently complex as to be beyond the scope of this paper.

In clusters of galaxies, the virial motion of galaxies can power Alfvenic turbulence. Considering the parameters $n= 10^{-2}\rm cm^{-3}$,  $B= 10^{-7}$ G,  $kT \sim 10$ keV. Then $v_A \sim 30$ km/s, the ion gyrofrequency is $ \omega_c \sim 10^{-3}\rm s^{-1}$, and the gyroradius is $r_g \sim 10^{11}$ cm.  Let us choose  $u^2 = 10^{-2} kT/m_p = [10^7$ cm s$^{-1}]^2$ $ \sim 10 v_A^2$.  The collisional mean free path is of  order $10^{22}$ cm, and the collision time of order $10^{14}$s. If turbulence can be excited on scale L much smaller than this, then the acceleration time is

\begin{equation}
\tau_{acc}= (l/r_g)^2 \omega_c^{-1} \sim 10^3 (L/10^{11}\rm cm)^2 s
\label{ratio}
\end{equation}
If the winds from individual stars of galaxies "rake" the intracluster medium and excite small scale turbulence at scale L,  then ions can be accelerated until their  gyroradii are comparable to L. For $L\sim 10^{16}$ cm,  this would imply that relativistic energies are attained -  enough for them to generate energetic electrons in nuclear collisions.

\section{Summary and Discussion}
We have gone back to an earlier work  (Eichler, 1979b) and reexamined it in light of the prediction of Sridhar and Goldreich (1995) that Alfven wave turbulence becomes tubular as it cascades to higher wavenumber. Tubular eddies aligned with the magnetic field (i.e. wavenumber nearly perpendicular to the field) are less efficient at accelerating particles via cyclotron resonance because resonant particles, having $v=\omega_c/k_{\parallel}$, cut across many tubes breadth-wise (i..e. many perpendicular wavelengths) during a single gyration. On the other hand, because the spectrum is a much steeper function of parallel wavenumber than in older theories (e.g. Kraichnan, 1965), the partially ionized heavy elements, having large gyroradii,  enjoy a stronger advantage (i.e. a shorter acceleration time) relative to lighter species with smaller gyroradii.  { We found the acceleration rate in Alfven turbulence with Sridhar-Goldreich geometry to be constant with energy in any one ion species, but with an acceleration rate that is proportional to the mass-to charge ratio.  This means that particles gain energy exponentially with time, and that, in the initial phases, the abundance enhancement of ultraheavies can be exponentially larger relative to lighter species.  It aslo suggests flat energy spectra until escape limits further acceleration so that the energy resides mostly in particles that have undergone many e-folds in energy.  It remains an open question whether the non-thermal tail of the spectrum reaches steady state, but, as the observed spectra are somewhat steeper  than we have calculated, maybe it doesn't. Rather, it is quite possible that the spectra we observe represent the superposition of particles from many acceleration sites, each with its own time-limited maximum energy, and this would lead to dramatic enhancement of partially ionized ultraheavies at the higher energies.}

We have shown that if strongly super-Alfvenic turbulence is stirred up by solar flares, then the Sridhar-Goldreich mode of cascade may set in at scales $l$ that are actually smaller than the thermal gyroradii of heavy ions, under the assumption that they move at the same "thermal" velocity at the lighter species (Eichler 1979a) due to other collisionless dissipative processes. In this case, the left hand side of equation (\ref{ratio}) can be large and some heavy ion species (e.g. oxygen, iron, which are sufficiently abundant that acceleration out to $\sim 1$ MeV/nucleon could in principle consume most of the energy budget) can damp the turbulence before it cascades to small enough scales to cyclotron resonate with protons, as discussed in E79. If such a situation were to obtain, it would further enhance the preferential acceleration of ultraheavies relative to lighter species.

 Observations suggest that impulsive SEP events do not coincide with coronal mass ejection, but rather originate at the interfaces between active regions and coronal holes (Wang et al., 2006). This is consistent with the picture that turbulent energy is exported from the strongly magnetized active region to the less magnetized coronal hole, where it is more super-Alfvenic, and thus less tubular.

It is still an  open question whether the heavier ion species are merely preferentially accelerated, as in a mostly  perpendicular cascade of turbulent energy, or whether they actually monopolize the energy budget of the cascading turbulence, which is more likely to be true for isotropic  than for tubular Alfven turbulence. Either way, the acceleration rate is a strongly increasing function of gyroradius, and ultraheavies can thus be  strongly enhanced relative to protons and other lighter species at high energies. However, the fact that rare ultraheavies ($Z\gg 26$) are enhanced even relative to iron  suggests that  monopolization of the energy budget, which is not likely in the case of rare ultraheavies,  is not the only mechanism for the enhancement. This woul disfavor simple isotropic Kolmogoroff or Kraichnan pictures of turbulence.

A key observational quantity that might distinguish between these two distinct scenarios for the damping of a turbulent cascade is the fraction of flare energy that goes into energetic particles, as opposed to heat and/or mass ejection. Monopolization of the energy budget by superthermal heavy ions would predict that most of the cascading turbulence went into the superthermal particles, rather than heat.  However, other loss mechanisms, such as acoustic losses and non-linear Landau damping need to be considered before this matter can be fully settled. It is clear that any dissipation mechanism steepens the turbulence spectrum as it cascades to higher wavenumber, making the acceleration less efficient but increasing preference for high rigidity ion species.

It is therefore significant that observations of $^3$He-rich flares are consistent with a {\it low acceleration efficiency}. We may estimate that a coronal mass ejection (CME) requires at least $10^{11}$ g (Wang et al, 2006), hence at least $10^{26}$ ergs, to be detected, and CMEs that have been reported are typically more energetic than this by several orders of magnitude (Shimojo and  Shibata, 2000). By contrast, the fluence of SEPs, at energies of order 1 MeV,  is of order $10^3$ $^4$He nuclei per $cm^2$, which at 1 A.U. corresponds to an isotropic-equivalent energy of $\ll 10^{25}$ erg. The impulsive SEPs are apparently observed only when the field lines associated with the {\it boundaries} of active regions intersect the ecliptic - there is no indication that they are convected out of the corona, along with ejected mass, over a broad solid angle -  indicating that the particles escape only on isolated field lines, and that the true energy in escaping SEPs for these events is many orders of magnitude less than the isotropic-equivalent energy.

The presence of some protons and $^4$He nuclei in the impulsive SEP population, is not unexpected. The enhancement is typically a sensitive but  smooth  function of mass to charge for all elements from He to ultraheavies, given reasonable assumptions about the charge states in a hot corona (Mason et al 2004). The enhancement  can be fitted as being proportional to $(M/Q)^{3.26}$. It may be that protons, which are not plotted in Mason (2004), are somewhat more abundant than simple extrapolation of  their formula (Reames, 1999). On the other hand, it could be that there is additional heating due to other mechanisms which competes with cyclotron damping when the rate of the latter is sufficiently small.

We have suggested here that SEP populations might shed light on how Alfven turbulence cascades and damps. At present, the picutre of
 relatively small energy content in SEPs, together with a systematic enhancement of ion species as a strong function of their charge to mass ratio,  is consistent with the Sridhar-Goldreich picture of tubular cascading of Alfven turbulence. More observational details are  needed to strengthen  this conclusion.

\acknowledgements
I thank  G. Mason for very helpful conversations and for encouraging a return to this work. I also thank Y. Lyubarsky and U. Keshet for helpful theoretical conversations. I gratefully acknowledge support from the Israel-U.S. Binational Science Foundation, the Israeli Science Foundation, and the Joan and Robert Arnow Chair of Theoretical Astrophysics.

\bigskip
\bigskip

\centerline{References}

 \noindent Bogdan, T.J., Lee, M.A. Schneider, P. 1991, JGR, 96, 161

  \noindent Chandran, B.D.G., 2000, ApJ, 529, 513

  \noindent Eichler,  D. 1979a, ApJ, 229, 409

 \noindent Eichler, D., 1979b, ApJ, 229, 413

 \noindent  Eichler, D., 1979c, ApJ, 229, 419

  \noindent Fisk, L.A. 1978, ApJ 224, 1048

 \noindent  Kennel, C.F. \& Engelman, F. 1966, Phys. Fluids, 9, 2377

  \noindent Kraichnan, R.H. 1965, Phys. of Fluids, 8, 1385

  \noindent Lee, M.A. \& Volk, H. J., 1975, ApJ, 198, 485
\bigskip

  \noindent Mason, G., Mazur, J.E., Dwyer, J.R., Jokipii, J.R., Gold, R.E., \&  Krimigis, S.M., (2004)   ApJ, 606, 555,

 \noindent  Miller, J.A. 1998, Space Science Reviews 86, 79,

\noindent Reames, D.V. 1999, Space Science Reviews, 90, 413

  \noindent Reames, D.V., 2000, ApJ, 540, L111

  \noindent Schlickeiser, R. \& Achatz, U. , 1993, J. Plasma Phys. 49,  63

  \noindent Shimojo, M. \& Shibata, K., 2000, ApJ 542, 1100 doi:10.1086/317024

 \noindent Sridhar, S. \& Goldreich, P., 1995, ApJ, 438, 753

 \noindent Wang, Y.M., Pick, M. \&  Mason, G.M. (2006) ApJ, 639, 495

\begin{comment}

redpajama_set_name: RedPajamaArXiv


Gain insights into image-processing methodologies and algorithms, using machine learning and neural networks in Python. This book begins with the environment setup, understanding basic image-processing terminology, and exploring Python concepts that will be useful for implementing the algorithms discussed in the book. You will then cover all the core image processing algorithms in detail before moving onto the biggest computer vision library: OpenCV. You'll see the OpenCV algorithms and how to use them for image processing.
The next section looks at advanced machine learning and deep learning methods for image processing and classification. You'll work with concepts such as pulse coupled neural networks, AdaBoost, XG boost, and convolutional neural networks for image-specific applications. Later you'll explore how models are made in real time and then deployed using various DevOps tools.
All the concepts in Practical Machine Learning and Image Processing are explained using real-life scenarios. After reading this book you will be able to apply image processing techniques and make machine learning models for customized application.
Data scientists and software developers interested in image processing and computer vision.
This book has been written by Himanshu Singh, who has written books like Practical Machine Learning and Image Processing: For Facial Recognition, Object Detection, and Pattern Recognition Using Python. The books are written in Computer Science category. This book is read by people who are interested in reading books in category : Computer Science. So, if you want to explore books similar to This book, you must read and buy this book.
So if you are a Reader belonging in the Good category, and you read it daily for 1 hour, it will take you 11 days.


For parents, the task of telling children about your intentions is painful and difficult.
Whilst as adults you have already worked your way through to the decision to separate or to divorce your children are only just starting on a journey that you may already have more or less completed. It will come to them as a great shock even if they have already suspected that it may happen.
There are no hard and fast rules. Every child is different and you will need to judge the best way of telling your child based on what you think their frame of mind is.
The most important thing to remember is their need for security (you are both still their parents and always will be), and they should have the opportunity to express themselves and their feelings in whatever way they feel able. This may vary greatly from extreme anger to complete silence. If you have more than one child you will need to weigh up whether you tell them individually, or all together, or a combination of this.
If you are to do this without getting into further conflict it is a good idea to tell the children together. If you feel you can then try to think through together the sort of questions your children will be likely to ask and how will you answer them. Decide which questions you may not be able to answer and how you will deal with those – questions such as "where will we live?" for examnple. Will you be able to give them the same "story"? It is important that you do avoiding blame.
Being at home will feel safer for children – if they are upset they can show their emotions and have access to you both. Allow plenty of time so that you are going to be able to cope with the possible immediate reactions and remember to be readily available at all times for delayed reactions.
Telling daughter about divorceBe honest with your children and don't retract if they cry. It is likely to cause more pain later on because you set up false expectations that cannot be realised and it only prolongs the hurt. It is important to be reassuring without making unrealistic promises – this is a very difficult task for parents, we never want to feel that we have deliberately upset our children. Think about what your child or children are able to understand at this stage too. They are not adults and their perceptions and understanding are at a different stage from your own. Your children do not need to hear from either of you the faults of the other – remember, you are the people they love and are closest to in their whole world – that won't change for them even if it has for you.
There could be tears, anger, pleading, promises of good behaviour, fear, bravado and denial. Do not argue or negotiate but tell the child you understand and you know that it does hurt but you will try to help them so that it hurts less. Be clear that what has happened has not been because of them or anything that they have done, but a decision made between their two parents.
If future arrangements have been determined let them know what they are. Probable timing of events can be helpful for older children, but do not overwhelm them with too much information at first, only what you judge they can take in initially. Think about the age of each child and your own close knowledge of their level of understanding and be guided by that. Tell them if you wish that you are coming to see people to work out what is best for all of you and you will tell them as soon as you know anything if this is appropriate. Be specific but don't over explain. Try not to involve them in the solution or decision making unless they are old enough – and even then be aware that many children still prefer for their parents to be the people who decide what is best for them.
If one of you is going to move out it often helps to involve the children in the move. Show them where you are going to be moving to, where their future bedroom will be when they visit you, show them the kitchen and your future bedroom. Children worry about the wellbeing of the non-resident parent, will s/he have enough to eat, where will s/he sleep, will they be alright? By involving them they can feel reassured and also feel they are actively participating – the fantasies are minimised. Sometimes this is not possible because the parent is moving away. If this is the case, and you know what the visiting arrangements will be, tell them jointly so that they feel reassured that they will be seeing you regularly.
Mother and child moving houseDo not be surprised if they talk to their friends about it. This sometimes proves helpful as friends may well have parents who are apart and they are sometimes reassuring or quite matter of fact about it all. Equally, watch out if your child tells no-one and be prepared to continue reassuring them that what is happening in their family often happens in other families too. Ask if they can think of anyone they know in a similar situation and tell them you understand that sometimes it is difficult to talk about. Do not be surprised if they tell you each quite different things about the same situation – their love and loyalties to you both will leave them wanting to make clear how much they love each of you. Sometimes they will need to show how cross they are or how distressed. If you can manage to keep your adult communication going during this time it will assist the children to understand that you remain, as their parents, together in your concern for them.
MOST IMPORTANT OF ALL – reassure children that you will both go on being their parents. You will always be their mother and father and the fact that you and your spouse are unable to get on well together anymore does not in any way alter your feelings for them. They are your children forever and your love for them will always remain the same.


text:
Effects of municipal sewage sludge doses...
Effects of municipal sewage sludge doses on the yield, some yield components and heavy metal concentration of dry bean (Phaseolus vulgaris L.)
Togay N., Togay Y., Dogan Y.
AFRICAN JOURNAL OF BIOTECHNOLOGY, vol.7, no.17, pp.3026-3030, 2008 (Journal Indexed in SCI)
Title of Journal : AFRICAN JOURNAL OF BIOTECHNOLOGY
Page Numbers: pp.3026-3030
Significant grain yield increase to applied municipal sewage sludge was obtained. This study was carried out in order to investigate the effects of the different doses municipal sewage sludge application on the heavy metal concentrations, yield and quality of dry bean in the 2006 and 2007 years. The trial was conducted in randomized complete block design with three replications. Four municipal sewage sludge doses (0, 20 000, 40 000 and 60 000 kg ha(-1)) were applied. Significantly higher pod and seed number per plant in municipal sewage sludge treatments had increasing effects on grain yield. Whereas grain yield, which was the highest component was obtained from 60 000 kg ha(-1) municipal sewage sludge with 1766.3 kg ha(-1) in the first year and with 1881.6 kg ha(-1) in the second year. The lowest grain yield were obtained from 0 kg ha(-1) municipal sewage sludge in both years. 60 000 kg ha(-1) municipal sewage sludge application was optimal with respect to increasing yield and yield characteristics. Concentrations of heavy metals in grain and shoot were similar to those in the fertilizer treatments. Cu, Zn, Cr, Pb and Ni in grain and shoot were well below their toxic thresholds.

redpajama_set_name: RedPajamaCommonCrawl


What trouble are you having? Check out Heads Up Poker Videos and Instruction at HUSNG.com | The ultimate resource for professional heads up poker strategy and training videos.
Last edited by ruimdg; 08-02-2014 at 09:31 AM.


* * Whole Sale Price*** you pay what dealers pay at the auction.
Great condition 2009 Infiniti G37 with very low miles. Clean title! Ice cold ac, new tires, sunroof, xenon hid lights, fresh service and oil change. Runs and drives great. Full Extended warranty available.
This auction is for cash buyers but we do offer SUB PRIME credit (no score needed) financing starting at $1500 down , low monthly payments we work several banks that finance all levels of credit and no minimum score is required. We can approve anyone with a social and income. Rates start at 12.99% with low monthly payments and flexible terms up to 72 months.
Vehicle is listed locally and may be sold at anytime.


Situated on a rocky peak halfway between Aix-en-Provence and Marseille, you will come across the Edgar Mélik Museum along the small alleys dating from the 12th century.
This former stronghold, where the Counts of Provence once lived, was again ennobled in 1934, thanks to the powerful palette of the painter Edgar Mélik, who had purchased the northern part of the fortified castle.
Upon his death, the municipality of Cabriès acquired in part this feudal dwelling, which opened to the public in 1980.
With his murals on nearly all the walls, including those of the 17th century chapel, Mélik's works can today be admired by everyone.
Temporary exhibitions devoted to the great names in art history, such as Dali, Picasso, Chagall, Miro, Giacometti, without forgetting the Provençal schools of painting, also take place since the museum's opening.


One heart-shaped box filled with berries and one filled with chocolates checks those sweet boxes! A decadent Valentine's gift for her, she'll enjoy strawberries hand-dipped and hand-decorated in Belgian dark and milk chocolate. The fruit flavors continue with a dark chocolate raspberry gem and milk chocolate orange cream--perfect for the chocolate lover in your life. Rich dark chocolate ganaches, salted caramel, and almond clusters set off this elegant Valentine's Day duo.
Chocolates Net Weight 7.1 oz.


Using A/B, new ideas can be essentially focus-group tested in real time: Without being told, a****fraction of users are diverted to a slightly different version of a given web page and their behavior compared against the mass of users on the standard site. If the new version proves superior—gaining more clicks, longer visits, more purchases—it will displace the original; if the new version is inferior, it's quietly phased out without most users ever seeing it.
**Creating a solution internally will take a significant amount of time and company resources. Typically larger companies invest the time, because they have very specific use-cases. The good news is that if you have the resources, you can customize this as you see fit.
**Open source can be a great option. Many packages like waffle (for Django) and split for Rails do a fantastic job at a very low cost. The downside is that the project may become stagnant. There's a bit of ambiguity, but I highly recommend using an open source package. Don't reinvent the wheel.
**I'm a big fan of third-party tools like Optimizely & Visual Website Optimizer (if you couldn't tell already.) The reason why I suggest it is because it breaks down the barriers to setting up and running tests. That's probably the biggest challenge companies face. The other two options will require more engineering resources.
I recommend that you do further segmentation, whether that's by new/returning visitors, countries, or traffic source. Don't be afraid to dig deeper.
Fortunately there's some great integrations software companies have to make this really easy. I personally use Optimizely + Mixpanel, but you could use KISSMetrics or Google analytics too.


text:
Woke Diversity and Equity Programs Have Failed; We Don't Need More of Them in Our Schools
Jonathan Butcher / @JM_Butcher / January 20, 2023
School districts across the country established diversity, equity, and inclusion offices to reduce discrimination, but hundreds of studies show "anti-bias" training doesn't reduce bias or increase diversity. (Photo: Klaus Vedfelt/Getty Images)
Jonathan Butcher / @JM_Butcher
Jonathan Butcher is the Will Skillman fellow in education at The Heritage Foundation and the author of "Splintered: Critical Race Theory and the Progressive War on Truth" (Post Hill Press/Bombardier Books, 2022).
School districts across the country have established diversity, equity, and inclusion, or DEI, offices to reduce discrimination, and the federal Department of Education regularly touts the value of DEI programs to quell bias. Yet nationwide, school officials reported a "record number" of discrimination complaints last year.
In truth, studies show that DEI offices accomplish little more than producing a lot of bureaucratic sound and fury on the taxpayers' dime.
Some of the complaints came from parents of children with special needs who reported that schools neglected their children during the pandemic. But that didn't keep The New York Times from blaming conservative lawmakers who, the newspaper's report asserted, "rolled back civil rights protections" by rejecting the bias and discrimination inherent in DEI programs inspired by critical race theory.
The number of complaints logged in 2022 (approximately 19,000) is some 19% higher than the then-record number reported in 2016—the year before former President Donald Trump took office. Yet DEI efforts were already well underway back then.
In 2015, the Education Department had released reports on how to "advance equity" and how to create more "equity" in preschools. In 2016, it reported on "promising practices" to advance diversity and inclusion in higher education and racial diversity among teachers.
The drive continues. Last year, the agency launched a new "equity action plan" that, among other things, celebrates the billions of dollars in taxpayer money being sent to schools as part of COVID-19 relief packages.
Yet despite the reports and new money, the racial problems in schools remain "astronomical," according to federal officials. So why do they think we need more of the same DEI?
"Anti-racist" literature and equity projects want us to see racism in everything, making it harder to decide what actions are biased and deserve a response. If we accept the "astronomical" numbers are authentic, then—given the prevalence of DEI programs for many years—we have to question these programs' value.
Research has already shown that diversity training programs have failed to improve attitudes and behaviors for years and attempts to reduce bias through measuring just how much of it each of us has stored away in the recesses of our minds have been a spectacular bust. Anthropology Now reports that "hundreds of studies dating back to the 1930s suggest that anti-bias training doesn't reduce bias."
More recent studies reviewing hundreds of surveys of bias-training participants finds "weak immediate effects on unconscious bias and weaker effects on implicit bias." Consultants Rik Kirkland and Iris Bohnet at McKinsey & Co. wrote that after reviewing diversity research from all over the world, they "did not find a single study that found that diversity training in fact leads to more diversity."
Still, school districts across the country are conducting DEI training and instruction—often mandatory—and implementing the programs emanating from Washington. And the Biden administration remains committed to digging and then refilling holes created by its DEI efforts.
State lawmakers should consider proposals that give parents veto power over these initiatives. Parents should be able to review school curriculum and student assignments. Only a few states offer parents a way to see what their children are being taught with the ability to create change when necessary, short of choosing another school.
State officials should also prohibit school leaders from forcing teachers or students to accept the idea that they are guilty of prejudice just because of their skin color. Nor should they be made to profess ideas such as "America is systemically racist" (a practice that is already prohibited by the Civil Rights Act of 1964).
Evidence on DEI programs' effectiveness is not missing. The research demonstrates failure.
Teachers, parents, and students do not need lawmakers to reinforce these efforts. Rather, they should opt for something different—say, lessons on the shared American values of equality under the law, freedom, and opportunity.
This article originally appeared in The Washington Times
Have an opinion about this article? To sound off, please email letters@DailySignal.com, and we'll consider publishing your edited remarks in our regular "We Hear You" feature. Remember to include the URL or headline of the article plus your name and town and/or state.


Joseph Plunkett Tower is the last of the seven Ballymun flats standing and today work began on its demolition.
DEMOLITION WORK ON the last remaining Ballymun tower began today, signalling the end of an era for many Dublin people.
Whether you once lived in the flats or you just remember them in the city skyline, the Ballymun flats are iconic in Dublin.
TheJournal.ie paid a visit to the site today. The demolition team were there and ready to get started. Walking past the site, an elderly man who has lived in the area for over 40 years said it was a momentous day.
I've lived here for over 40 years, they've always been here. But it is a good thing they're going. Although, people used to always know where Ballymun was by those towers. Now I don't know how they'll get here. It is a sad day.
The Ballymun flats were first built in the 1960s.
In order to tackle Dublin's housing issues, seven Ballymun Towers were built on the outskirts of the city between 1966-69.
The towers were initially built for social housing and named after the executed 1916 rebels. Each tower was 15 storeys tall and contained over 90 flats.
The last one standing, Joseph Plunkett Tower, was built in 1967. It has been abandoned since 2013, when its last resident left.
Despite its problems, the people of Ballymun who were born and reared in the blocks hold many fond memories and are proud of their community.
It's difficult to imagine, but before their construction, Ballymun was just a small village surrounded by farmland.
Geraldine Bermingham, who works in the cafe in the civic centre across the road from Joseph Plunkett Tower says she has lived in the area since she was four years old.
There used to be nothing but farms here before the flats. When I first moved here there were cows in fields.
She said it is sad to see the last one go, but said the community spirit left the area when the first flats were knocked down.
I think it was better when all the flats were here – there was more of a community spirit.
The people around would do anything for you. I mean my neighbours are the same neighbours for the last 40 years. People look out for each other here, but I don't think there is that community spirit any more. I think everyone is isolated.
Bermingham said the families that were moved out of the flats were relocated in areas further away, which did damage to the locality.
Your neighbours were your neighbours when you lived in the flats. You could knock in for a bit of sugar, couple of tea bags. I think all that is gone now as the houses they were moved to are that bit more private. There were four or five people on the one landing, so if you were there for 40 years you knew them for the last 40 years, they were like your family. I'd never live anywhere else though.
A few steps from Joseph Plunkett Tower is the Ballymun Shopping Centre – once a place bustling with business, the complex is now empty, full of shuttered up shops and it's eerily quiet.
Linda Sherraod works in the local St Vincent's de Paul shop. She has lived in the area for years and says she remembers Ballymun before the flats were built.
When they were going up it was a massive deal. My sister lived in the fourth storey across the way and they used to have them lovely inside. Then she got one of the houses. It was hard for her when she moved out in the beginning. The flats were brilliant years ago. It was handy when the weather was nice you could dry your clothes out. It was very hard when people had to move out of the flats. Some people wanted to stay and some would go back into them now if they could. They miss the flats.
She said she thought it was a shame for the final tower to be knocked down, saying there are families in the area that need a place to stay.
I think they should have kept that tower and used it to house the homeless. There are a lot of families living in a hotel just across the road there. Think of it. There are over 90 flats in that tower.
Crossing the road with her shopping is Rosaleen Coffey, an elderly woman returning from town.
A lot has changed in the area. The way I look at it now, if people had been able to put some people into it, like the homeless, it would have been a great achievement, but I do know there was something wrong with the whole project, so they had to take it down.
There is a great community here, but I am the type that kind of keeps to themselves. It was a tight-knit community. I loved my flat while I was in it, then I moved over to the house. If I could have took my house over with me, I would have took it, because it was nice. We had good neighbours.
Coffey said there is a different feeling in a house than in a flat.
There was never any trouble, it was quiet. It will be a big change so I wonder what they are going to do with. We've no shops here, there is nothing, only a Supervalu and Centra. Whatever they do, I don't think it will be in my time.
One common thread from people we chatted to is that the demolition of the flats sucked the life out of the community.
The promises of regeneration never fully materialised and the lack of resources and services in the area is impacting on the people.
"I am here 30 years myself," says Bernie, who works in the shopping centre.
It's sad day. People know Ballymun from the towers. It is the end of an era. But the community feel is gone. There used to be a nice coffee shop here where people would meet and chat and now it's gone. I had a man here last week that was just stopped here in his wheelchair. I asked him if he was alright and we got chatting. Then all of a sudden he started crying. He started chatting about his wife and how she had died. It was sad. My daughter used to work in that coffee shop and she lost her job, people used to gather, have a cup of tea, but now there's nowhere to go. That man probably just wanted to talk to someone.
That is something Bermingham agreed with. "There is nothing out here, no schools, no churches," she said.
There is not even a bus to bring the old people to the Omni. There is nothing. Regeneration is a load of crap, this building is half empty.
When I was a kid that shopping centre was buzzing, there was loads of shops – butchers, Penneys, shoe shops, everything. There's not even a local pub, now that The Towers is gone.
Local taxi man Joseph Maxwell said the flats would have been great had they not been left to "wrack and ruin".
There was a great community here, but lots of it seems to have gone. It has changed big time. Underneath the flats there were little units. In each one was a club – children's clubs, men's clubs, pigeon clubs, darts clubs, all along the blocks. When all those flats were pulled down all those clubs were gone as there was no where for them to go – all the community spirit went with it.
The government promised that regeneration would be finished, but it never was.
The demolition of Joespeh Plunkett Tower could take weeks as a long-reach hydraulic 'nibbler' is being used to hack away at the tower until it is no more.
Email "'Some people wanted to stay in the Ballymun flats and would go back now if they could'".
Feedback on "'Some people wanted to stay in the Ballymun flats and would go back now if they could'".


text:
The Super Super Blues Band is an album by blues musicians Howlin' Wolf, Muddy Waters and Bo Diddley released on the Checker label in 1968.

Reception

AllMusic reviewer Ken Chang stated "Wolf adamantly refuses to back down from his rivals, resulting in a flood of contentious studio banter that turns out to be more entertaining than the otherwise unmemorable music from this stylistic train wreck. Although Wolf and Waters duke it out in earnest on the blues standards, the presence of Diddley (and his rave-up repertoire) makes the prospect of an ensemble impossible; in the end, there are just too many clashing ingredients to make the mix digestible. ... At least it sounds like they had fun doing it".

Track listing
 "Long Distance Call" (McKinley Morganfield) – 9:10
 "Medley: Ooh Baby / Wrecking My Love Life" (Ellas McDaniel / Clifton James, Kay McDaniel) – 6:28
 "Sweet Little Angel" (Robert Nighthawk) – 6:30
 "Spoonful" (Willie Dixon) – 4:10
 "Diddley Daddy" (McDaniel) – 5:10
 "The Red Rooster" (Dixon) – 7:20
 "Goin' Down Slow" (James B. Oden) – 4:47

Personnel
Howlin' Wolf – vocals, guitar, harmonica
Muddy Waters – vocals, guitar
Bo Diddley – vocals, guitar
Otis Spann – piano
Hubert Sumlin – guitar
Buddy Guy – bass
Frank Kirkland – drums
Cookie Vee – vocals

References

1968 albums
Howlin' Wolf albums
Muddy Waters albums
Bo Diddley albums
Checker Records albums
Collaborative albums

redpajama_set_name: RedPajamaWikipedia


This lavender dog hat is a great way to keep your dog's head nice and warm. Attached to the front of the hat is a small off white flower with a button center. Two ties at the bottom make this hat convenient to put on and take off. Hat measures approximately 16 inches around and 7 inches tall. Stays put with two 16 inch long ties.


text:
Q: Error trying to define type Relation [(a,b)] as an instance of Category class I'm exploring some possible implementations of R subset of AxB, each with its limits and possibilities. I would also like, when possible, to define them as instances of the Category class or Semigroupoid class.
I have chosen the list of pairs since, with regard to the operation of composing lists, it only places types of the elements of the pair the constraint of being instances of the Eq class.
Now I'm stuck on this compiler error message: "No instance for (Eq a) arising from a use of '°'"
What's wrong?
{-# LANGUAGE GADTs #-}

module RelationT where

import Data.List
import Control.Category as Cat

data RelationT a b where
  Id :: RelationT a a
  RT :: (Eq a, Eq b) => [(a,b)] -> RelationT a b

instance Category RelationT where
  id = Id
  Id . r = r
  r . Id = r
  r1 . r2 = r1 ° r2 -- error:  No instance for (Eq a) arising from a use of '°'

(°) :: (Eq a, Eq b, Eq t) => RelationT t b -> RelationT a t -> RelationT a b
RT r1 ° RT r2 = RT $ nub $ go r1 r2
    where
    go [] r =  []
    go r [] =  []
    go xys2 ( ((x1,y1): xys1)) =  go2 x1 y1 xys2 [] ++ go xys2  xys1
        where
        go2 x y [] acc = acc
        go2 x y ((w,z):wzs) acc
          | y == w = go2 x y wzs ((x,z):acc)
          | otherwise = go2 x y wzs acc

-- ex. RT [(1,'a'),(4,'b'),(5,'c'),(10,'d')] ° RT [(3,10),(1,5),(1,1)]
-- > RT [(3,'d'),(1,'c'),(1,'a')]

A: If you're storing the Eq constraints in a GADT, there's no need to require that from the signature: by pattern-matching on the relation-values, the constraint will already be in scope. So, just change the signature to
(°) :: RelationT t b -> RelationT a t -> RelationT a b

The (Eq a, Eq b, Eq c) information will still be available within the function body, because you've pattern-matched RT r1 and RT r2 there, which if successful witness that all the types have an Eq instance.
That said: in my experience, this trick of storing a constraint in a GADT leads quickly into trouble when you want to do more involved stuff with your category. The problem is, the standard Category class is not really suitable for a relation type like this, because it only supports categories which have exactly the same objects as Hask – i.e., all Haskell types. But your relation category really has only equality-comparable types as objects; with the extra Id constructor you're forcibly extending it to also include relations between non-eq types, but there only the identity relation is available... that's quite a fragile hack.
The proper way out is to use a typeclass which allows the categories to have a more restricted notion of objects to begin with. The simplest means to do that are constraint kinds. From my constrained-categories package:
{-# LANGUAGE TypeFamilies, ConstraintKinds #-}
import GHC.Exts (Constraint)

class Category k where
  type Object k o :: Constraint
  id :: Object k a => k a a
  (.) :: (Object k a, Object k b, Object k c)
         => k b c -> k a b -> k a c

Then you can make the instance
data RelationT a b where
  Id :: RelationT a a
  RT :: [(a,b)] -> RelationT a b

instance Category RelationT where
  type Object RelationT o = Eq o
  id = Id
  (.) = (°)