text:
by Dr Anton Burkov, PhD (Cantab), LLM (Essex)
Transparency of the Judiciary in Russia
On 1 July 2010 the Federal Law on Transparency of the Judiciary in the Russian Federation came into force.
From the moment that the President of the Russian Federation, Dmitry Medvedev signed and promulgated the Federal Law 262-FZ of 22 December 2008 "On Securing Access to Information on the Activity of Courts in the Russian Federation" (the Law), the Russian courts began preparing for its entry. Russian courts had been preparing for the Law from the moment it was originally signed and promulgated by the President of the Russian Federation in 2008. This article discusses the substance of the Law and the readiness of courts to publish judicial decisions on the internet.
The main aim of the law is to make information on the activity of courts more open to the public, as well as addressing trends in society such as advances in computer technology and the internet. The law would allow access to information on court activity via the following means (Article 6 of the Law):
1.	presence of citizens and representatives of legal persons, and state and municipal organs, at public court hearings;
2.	publication of information (including courts decisions) on courts activity in mass media, Internet, and courts premises;
3.	familiarisation of citizens and representatives of legal persons, state, and municipal organs with archived information of courts activity.
The publication of court decisions is not characteristic of a country with the continental legal system, where statute is main basis of law,. Additionally, it might be thought impossible for a country with such large territories and a high number of courts . Access to the practice of Russian courts has always been a difficult process. With a few exceptions, there had been no mechanism for the publication of courts decisions prior to 1 July 2010. Previously, the Constitutional Court of the Russian Federation had published all of its judgments according to merit and selectively admissible decisions. The Supreme Court published selected judgments and limited extracts from judgments of lower courts in the Bulletin of the Supreme Court. These selected practices had been unofficially published on a number of web-sites and commercial databases. Insight into the practices of the lower courts are largely only available from lawyers and advocates.
Article 15 of the Law on publication of judicial acts online is of greatest interest when considering the publication of judicial acts.
On 23 June 2010 the Chief Justice of the Supreme Court, Viacheslav Lebedev, stated that the Supreme Court had launched its own website, without waiting for the 1 July Law, which gives access to full information on the Court's activity, including its judgments.
Effective implementation of the Law, particularly Article 15, is yet to be monitored and assessed. However, journalists and representatives of non-governmental organisations have already made attempts to clarify the difficulties with the publication of judgments.
On 24 July 2010, representatives of civil society and the judiciary discussed the readiness of justices of the peace, courts of general jurisdiction, and arbitrazh courts for the new Law, which was yet to come into force. They met at a round table, "Access to Justice through Access to Information on Courts Activity" in Yekaterinburg, Sverdlovsk oblast, Russia. Among the participants were representatives of civil society (NGO lawyers, advocates, journalists), the judiciary (Sverdlovsk oblast court and the Arbitrazh court of Sverdlovsk oblast), the Ombudsman of Sverdlovsk oblast, and representatives of the regional legislature – the Commission of Oblast Duma on the preliminary preparation of materials for the consideration of judicial candidates at the sittings of Oblast Duma of Legislative Assembly of Sverdlovsk oblast.
There were representatives of courts at the round table that already function under the Law, as well as courts that are yet to start publishing their judgments. Head of staff and administrator of the Arbitrazh court of Sverdlovsk oblast, Chukavina Tatiana Viacheslavovna, in her report "On Ensuring Access to Information on Activity of Arbitrazh Court of Sverdlovsk Oblast" highlighted the fact that judges in the Arbitrazh court of Sverdlovsk oblast had seen organisational preparation to allow the publication of judicial acts before 2005 – the year when judgments of the arbitrazh court first appeared online. According to Ms Chukavina, open resistance on the part of judges did not characterise the period of transition to online transparency, but it did lead judges to acquire Russian language dictionaries and textbooks on spelling and punctuation. Therefore the online publication of judgments influenced not only the linguistic quality of judgments but also the quality of legal decisions.
Also of interest was a speech by Head of the Department of legal information of Sverdlovsk oblast court, Livshits Arkadiy Afanasievich. In his report "On Ensuring Access to Information on Activity of Sverdlovsk Oblast Court" Mr Livshits expressed dissatisfaction with the Law because it creates "the game of the openness of justice." The major problem was amending personal data (mainly names) in judgments: high labour costs and the absence of a "consumer" in amended judgments (cases heard in closed hearings are not published under the Law). In Mr Livshits' opinion, there is little interest in judgments on cases of "NAME 1 v. NAME 2." On 1 July 2010, there was an amendment to the Law where judgments are published as they enter into force.
It was argued that the Law will not solve the problem of openness and, more importantly, will not lower the number of applications before the European Court of Human Rights, which will inevitably increase due to the amendment of procedures for the consideration of cases European Court of Human Rights cases resulting from Protocol 14 to the Convention for the Protection of Human Rights and Fundamental Freedoms. The procedure for the publication of judicial acts in the system of State Automatic System "Justice" (GAS "Pravosudie") is constructed in such a way that Sverdlovsk oblast court is only responsible for the publication of judgments on its own website. For instance, the district court of Ivdel (situated 500 km north from Yekaterinburg) will deal with the publication of its own judgments.
Justices of the peace have not yet adopted the relevant regional law, not to mention publication of their decisions. Some round table participants noted that it takes longer for a justice of the peace to prepare an online publication than it does to issue a decision.
At the end of the round table, participants unanimously voted for the creation of a Discussion Club to review the question of judicial reform in Russia, and the improvement of cooperation between the judiciary and civil society. The first document was adopted with a resolution from the Governor of Sverdlovsk oblast, Legislative Council of Sverdlovsk Oblast, Council of Judges of Sverdlovsk oblast, Civic Chamber of Sverdlovsk oblast, and other interested parties who put forward a proposal to support an initiative to hold regular public discussions on the problems of cooperation between civil society and the state on the issue of reforming the Russian judiciary and improving the openness of the courts . By itself, the initiative to hold public discussions on reforming judicial system is unique. Judicial reform has underway since 1990, but only in 2004 did representatives of civil society get involved in monitoring judicial reform when the institute of civic representatives in qualification collegiums of judges was established.
The next meeting of the Discussion Club will take place on 22 July 2010, when it will tackle the issue of the implementation of Federal Law of 30 April 2010 N 68-FZ "On Compensation to Citizens for Violation of the Right to a Fair Trial within a Reasonable Time or the Right to Execution of a Judgement within a Reasonable Time." This new Law was drafted in order to stop applications before the ECHR where there was a lack of an effective domestic remedy to secure adequate and sufficient redress for non-enforcement or the delayed enforcement of domestic judgements. We will review this law in future columns.
Published at EU-Russia Center
See in Russian


Outdoor movies are a summer tradition in Raleigh, Durham Chapel Hill, and beyond. Read on to find an outdoor movie series near you. Most are free. Some cost a nominal fee. Some are geared toward families and some are for adults. Follow each link to get necessary details. In some cases we've been able to list the movie schedule.
Also, if you haven't done so yet, you might want to sign up for emails from Triangle on the Cheap. It's the best way to keep up on all the free and cheap things to do. Never more than one email a day. Follow us on Facebook and Twitter too!
June 14-August 30 2019. Mostly on Fridays, but one Thursday.
Tickets are $5, free for kids 12 and under. Bring a blanket or chair as the spacious lawn at Booth Amphitheatre is transformed into an outdoor movie theatre. Gates open at 7 and the movie starts at dusk. No pets. Bring a picnic (beer and wine OK). Most of the movies are family-friendly, but there are a couple suited for adults.
Movies start at dusk on most Saturdays.
Outdoor movies are shown on top of the parking deck at 8:30 p.m. on the select Thursday of each month. Free admission, free popcorn, games and activities for kids and adults. Bring your own lawn chairs or blankets.
Free to attend. Bring lawn chairs or blankets. Food vendors will be on site. No alcohol allowed.
The first film scheduled is for adults. Stay tuned for the rest of the film lineup.
So far a movie on April 26 has been announced.
Admission is free. Movies begin at dusk. Bring blankets or chairs and enjoy concessions that benefit local school PTAs.
Concessions start at 7:00 p.m. free movies start at 8:30 p.m. Food trucks and other concessions on site including beer and wine vendors; no outside alcohol allowed. Feel free to bring chairs or blankets and a picnic. Leashed, well-behaved dogs are allowed.


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You all spend have spent so much time with us, it's the least we can do to give back. You are our mission. You are our purpose. You are our family.
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redpajama_set_name: RedPajamaCommonCrawl


Dreamed I was in an older, upper-class neighborhood and had just finished loading the back of the Flex, with what, I do not recall, but it was a job getting the back hatch to latch. Once successful, the vehicle was now a gloss black third-generation Chevrolet Caprice Classic (with a front grill somewhere between the Winchester's 67 Impala and a 69 Coronet 440 but with a modern Caprice, "look") in which I got behind the wheel and started to drive. Only, in reverse. And of course the brakes didn't work - at all. Neither did the emergency brake which I pulled, pulled some more, and kept pulling, all to no avail.
As the car continued to pick up speed while moving backward, I turned to look behind me trying to steer clear of any obstacles. I was dismayed that I was accelerating towards an intersection, yet thankfully, the light was green. Unfortunately after speeding backward through that one, I quickly approached another - again green. Though I did understand this couldn't go on indefinitely. The next light was red, but I managed to squeeze through without crashing into anyone. I was not, however, so fortunate at the next red light; I scraped the front bumpers of two cars which were crossing the intersection. This fender bender did affect my speed - I slowed considerably, enough to make a turn at the next intersection where I stared a gentle back and forth motion trying to slow down further. I made one more turn up a road with an incline, slowed, and came to a stop against a building in Chinatown.
The two people I'd hit had followed the car and now approached me. I was apologetic as I fished the insurance information from my wallet and handed it to them to copy. That's when Dr. Gregory House emerged from the building I'd hit - it was his practice and he'd come out to tend to the injured. This encompassed him putting his hands up and down my neck and shoulders feeling for any indication of damage.


text:
AU Summit tells state parties to invest in girls' education - Graphic Online
AU Summit tells state parties to invest in girls' education
BY: Gender Desk report
AU Goodwill Ambassador for the campaign to end Earlier Child Marriage (ECM), Ms Nyaradzayi Gumbonzvanda (inset) addressing the summit
The second African Union (AU) Summit on Ending Child Marriage in Africa (held in Accra recently) has called on state parties to invest in the education of girls to build a better social and economic status for their future.
The four-day event,held from November 20 to 24, 2018, on the theme: "Enough with the Silence," was an initiative of the AU and it brought together hundreds of delegates from over 30 African countries, including four First Ladies from Ghana, Niger, Liberia and Sierra Leone and the AU Commissioner for Social Affairs, Mrs Amira Elfadil Mohammed Elfadil.
The second AU Girls summit sought to address the core need of investing in adolescent education, specifically access to services such as sexual health care, sexuality education and rights protection.
It looked at progress made on commitments, interventions, measures and recommendations of keeping girls in school and facilitating Sexual and Reproductive Health Rights (SRHR).
In line with efforts to end child marriage and other harmful traditional practices against girls, DANIDA, in partnership with Save the Children, used the occasion to launch a Sahel Regional programme which sought to increase organisational capacities of regional civils society organisations and youth networks in order to effectively engage the African Union to influence social and political change on Ending Child Marriage and Children on the Move in the Sahel.
The summit was a follow-up to the first AU Girls Summit held in 2015 in Zambia which was aimed at sharing experiences and good practices and ultimately initiating discussions and programmes to end child marriage at the country, regional and international levels by drawing experiences from countries that have launched such campaigns.
Among some of the key recommendations made after the summit was the need for state parties to strengthen integrated girl-centred comprehensive sexuality education and adolescent-friendly sexual and reproductive health and rights (SRHR) services for girls in and out of school, with focus on conflict zones, refugee camps, youth with disabilities, girls in prisons among others.
It also called for emphasis on SRHR education for parents and teachers and on countries to help 'break the silence' by empowering young people, especially girls, to be able to stand up, speak up and challenge harmful socio-cultural, religious and traditional norms and values and most importantly for the authorities to amply listen to the voices our girls, voices of those who are at risk.
The summit also recommended a legal framework for government to enact laws and policies that would prohibit child marriage and ensure the full implementation of such law or policy.
It also called for the full inclusion of Persons Living with Disability (PLWD) by accelerating and opening up discussions further to include other vulnerable girls in conflict zones, deprived areas and most importantly persons living with disability, saying they were four times more vulnerable to acts of child marriage.
They also called for resource allocation which they said was critical to ending child marriage.
It also recommended the strengthening of support for alternatives to child marriage, especially by making schools accessibly, enjoyable and affordable in the bid to keep girls interested.
Finally, it called for collaboration and a multisectoral approach to ending child marriage through concerted effort, urging the government departments, local institutions, private sector, media, international agencies, parents, traditional and religious leaders and every individual to get involved in ending child marriage in African.
Girls not bride
As part of the summit, WiLDAF, with support from Save the Children, held a side event with delegates from the Sahel Region including Mali, Burkina Faso, Mauritania, Niger, Senegal and Chad to assess the progress made in ending child marriage in the region.
They also shared experiences on lessons learnt, best practices and also to strategise on how to provide better protection for children against early marriage by bringing the key actors to work together.
The AU Goodwill Ambassador for the campaign to end Earlier Child Marriage (ECM), Ms Nyaradzayi Gumbonzvanda, urged the participants to fully commit to the cause of ending child marriage by standing up, speaking out and solving our own problems.
Other contributions from participants focused on accelerating efforts to push for sound and holistic programming, adequate resources allocation and legislative reform, especially setting the legal age of marriage at 18 for girls and boys.


text:
Rio da Vargem kan syfta på följande platser:

Brasilien

 Riacho da Vargem (periodiskt vattendrag i Brasilien, Bahia),
 Rio da Várzea (vattendrag i Brasilien, Bahia),
 Rio da Vargem (periodiskt vattendrag), Bahia,
 Rio da Vargem (vattendrag), Paraná,
 Ribeirão da Vargem, vattendrag, Santa Catarina,
 Rio Mourão, vattendrag, Paraná,

Robotskapade Brasilienförgreningar

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}

The Galactic magnetic field (GMF) plays an important role in the
propagation of cosmic rays even at highest energies. Expected
deflections --- of order few degrees or larger --- are comparable or
exceed the angular resolution of the existing cosmic ray
experiments. Such deflections may therefore be observable. Their
understanding is crucial when searching for sources of the
highest-energy cosmic rays if the latter are charged particles.

The detailed study of deflections of ultra-high energy proton
primaries in the GMF is particularly important if the deflections in
{\em extra-galactic} magnetic fields are small. According to the
results of Refs.~\cite{Dolag} this is likely to be the case (see,
however, Ref.~\cite{Sigl}).

The Galactic magnetic field has been shown to have both regular and
turbulent components. The regular component is thought to have a
spiral structure reminiscent of the Galactic arms with one or more
reversals toward inner (and probably also outer) Galaxy and the
magnitude of order $3~\mu$G in the vicinity of the Earth
\cite{GMFmodels}. The corresponding global model of GMF was
constructed in Ref.~\cite{Stanev:1996qj} and is often used in the
discussion of propagation of cosmic ray primaries in the Galaxy.
According to this model, protons with energy $4\times 10^{19}$~eV can
be deflected in the regular GMF by $\sim 5^\circ$. There are
indications that such a coherent deflections may indeed be
present~\cite{Tinyakov:2001ir,Gorbunov:2002hk,Teshima,Tinyakov:2003nu}
in the cosmic ray data.

The random component of GMF causes the spread of arrival directions of UHECR
around the mean position, thus diluting (and potentially destroying) important
information about the actual location of the source
\cite{Kronberg:1993vk}. Under certain conditions on the magnetic field it may
also lead to the ``lensing'' of cosmic rays \cite{Harari:2002dy,Harari:2002fj}
provided the number of sources contributing to the observed UHECR flux is
small, as is favored by the statistics of clustering
\cite{Dubovsky:2000gv}. Thus, the influence of a random fields is not simply
destructive, but may give useful information on the cosmic rays and GMF
itself.

Observationally, the magnitude of the random component of GMF is
comparable to the magnitude of the regular one. However, the
deflections of cosmic ray primaries in the random field are expected
to be considerably smaller.  Indeed, if the correlation length $L_c$
of the random component is much smaller than the propagation distance
$D$, the deflections caused by the random field are proportional to
$\sqrt{DL_c}$, see e.g. Ref.~\cite{Berezinsky_book}, while the
deflections in the regular field are proportional to the distance $D$
itself. Usually the deflections in the random field are estimated as
(see e.g. Ref.~\cite{Roulet:2003rr})
\begin{equation}
\delta_r = 0.6^\circ\cdot
\left({10^{20}~{\rm eV} \over E/Z} \right)
\left({B_r \over 4~\mu{\rm G}}\right)
\sqrt{D\over 3~{\rm kpc}}\,
\sqrt{L_c\over 50~{\rm pc}}\; ,
\label{FstEstimeate}
\end{equation}
where $E$ is the energy of CR primary and $B_r$ is the rms value of the
random magnetic field strength. However, the global picture of GMF is
very complicated. The magnetic field may be structured on relatively
large scales, including possibility of magnetic bubbles, sheets,
filaments, magnetic ``winds'' etc., so one cannot rely on (and be
restricted to) a generic estimate uniformly over the whole sky.

The rms deflections of cosmic ray primaries in the random field are determined
unambiguously by the magnetic field power spectrum. The latter can be
extracted from observations, see e.g. Ref. \cite{Minter}. Several existing
measurements of the GMF power spectrum indicate that the correlation length
can be large in some directions on the sky. In this case the deflections are
no longer proportional to $\sqrt{DL_c}$, and the estimate (\ref{FstEstimeate})
does not apply.

The purpose of the present paper is to estimate the deflections of
UHECR primaries in the turbulent component of the Galactic magnetic
field taking into account  possible dependence of GMF parameters on the region
of the sky and the possibility of large corelation length.
We express the UHECR deflections directly through the observable
parameters characterizing the power spectrum of the magnetic field.
To this end we derive the relation between the mean square deflection
and the power spectrum (PWS) of the GMF fluctuations. The result is
most conveniently represented through the factor $R$ defined as
\begin{equation}
\frac{\delta_r}{\delta_u} = \frac{B_r}{B_{u,\bot}}\, R\; ,
\label{thR_thU_Def}
\end{equation}
where $\delta_r$ and $\delta_u$ are deflections in the random and
uniform components of GMF, respectively, and $B_{u,\bot}$ is a
projection of a uniform field onto the direction orthogonal to the
line of sight. The factor $R$ varies between 0 and 1 and is expressed
in terms of the power spectrum of the random field by
Eq.~(\ref{theta2-fin}). Moreover, we show that it is a function of a
single observable parameter $\theta_c$, the angular scale of the break
in the relevant structure function of GMF.  In the case of small
correlation length when the estimate (\ref{FstEstimeate}) applies, one
has $R \sim \sqrt{\theta_c}$. The values of $R$ in our Galaxy derived
from the existing observational data vary in the range $R\sim
0.03-0.3$. This implies typical deflections of a $4\times 10^{19}$~eV
proton in the random field of order $0.2^\circ - 1.5^\circ$ depending
on the direction.

The paper is organized as follows. In
Sect.~\ref{sect:cor.length.and.PS} we recall the relations between the
power spectrum and the correlation length and introduce the
notations. In Sec.~\ref{observations} we describe existing
observations of the random magnetic field, in particular, the
random-to-uniform ratio and the parameters of the power spectrum. In
Sect.~\ref{deflections} we turn to the deflections of UHECR in the
random magnetic field and derive the expression for the coefficient
$R$. Sect.~\ref{conclusions} summarizes our results.

\section{Turbulent field}

\subsection{Correlation length and power spectrum of GMF}
\label{sect:cor.length.and.PS}

To introduce notations and specify our assumptions, let us first
consider the statistical properties of a random magnetic field
$B_a({\bf r})$, where $a=1,2,3$.  We define the Fourier components of
the magnetic field according to
\[
B_a ({\bf r}) =
\int d^3q B_a({\bf q}) {\rm e}^{ i {\bf rq}}.
\]
Here $B_a$ refers to the fluctuating component of the total magnetic
field; the regular part of GMF has to be treated separately.  In what
follows we assume that the fluctuations obey Gaussian statistics and
are spatially homogeneous and isotropic.

The last two assumptions deserve a comment. The statistical
characteristics of the magnetic field are different in different sky
patches. Our analysis and results should be applied to each of these
patches separately. We assume that statistical properties of GMF are
(approximately) constant over a single patch. Also, within one patch
the magnetic field fluctuations may not be isotropic, with the
preferred direction being set by the regular component of GMF. The
present data are not sufficient to establish or rule out the isotropy
of GMF fluctuations. With the more precise data this assumption may
need to be reconsidered, and the analysis may need to be refined.

With the above assumptions, all correlators of the magnetic field can
be expressed in terms of the two-point correlation function which can
be written as
\begin{equation}
\langle B_a^{~}({\bf q})  B_b^*({\bf q}') \rangle
= { {\cal B}(q)\over 2 q^3} (\delta_{ab}-n_a n_b)\delta^3({\bf q-q'}),
\label{BB*}
\end{equation}
where $n_a = q_a/q$ is a unit vector in the direction of ${\bf q}$ and
the projection tensor ensures the divergence-free nature of the
magnetic field, $q_a B^a ({\bf q}) = 0$.  The dimensional
normalization factors are chosen in such a way that the power spectrum
${\cal B}(q)$ has physical units of $B^2$, i.e. in our case it is
measured in the units of (Gauss)$^2$. The correlation function of the
magnetic field fluctuations is defined as
\begin{equation}
\begin{aligned}
\xi(r)&=&\langle B_a({\bf r_0})B^a({\bf r_0+r}) \rangle =
\int\frac{d^3q}{q^3}\; {\cal B}(q)\; \mbox{e}^{-i{\bf qr}} \hfill ~\\ &=&
4\pi\int_0^\infty\frac{dq\,}{q}{\cal B}(q)\; \frac{\sin (qr)}{qr}
~. \hfill ~~~~~~~~~~~~~~~~~~~~~
\end{aligned}
\label{variance}
\end{equation}
It determines the rms value of the field amplitude $B_r$,
\begin{equation}
B_r^2 \equiv  \langle B_a B^a \rangle = \xi(0) \; ,
\label{Br}
\end{equation}
and the correlation length $L_c$,
\begin{equation}
L_c \equiv  \frac{\int_0^\infty dr\; \xi(r)}{\xi(0)} \; .
\label{correlationlength}
\end{equation}
The energy density contained in a random component of the magnetic
field is related to the field variance as $\rho_B = B_r^2/8\pi$.

As will be discussed in Sect.~\ref{obs:pws}, in a certain range of
momenta the existing observations support a power-law behavior of
power spectra of the magnetic field fluctuations,
\begin{equation}
{\cal B}(q) \propto \frac{1}{q^{\alpha-1}}\; .
\label{Bpws1}
\end{equation}
Since the energy density in the magnetic field is finite, there has to
be a break in the pure power-law behavior, which can be parametrized as
\begin{equation}
{\cal B}(q) = \left\{
\begin{aligned}
&A\left( {q_c\over q}\right)^{\alpha_1-1} \hskip 0.5cm \mbox{at~~ $q<q_c$}\\
&A\left( {q_c\over q}\right)^{\alpha_2-1} \hskip 0.5cm  \mbox{at~~ $q>q_c$}\; ,
\end{aligned}
\right.
\label{Bpws}
\end{equation}
where $A$ is a normalization constant and $q_c$ is the momentum scale
at which the break in the spectrum occurs.  (Note that abrupt
ultraviolet and infrared cut-off can be modeled as $\alpha_2 \rightarrow
\infty$ and $\alpha_1 \rightarrow -\infty$, respectively.)
In what follows we assume this form of GMF power spectrum.
The variance $B_r$, and consequently the energy density, converges if
$\alpha_1<1$ and $\alpha_2 >1$. Summing up contributions from both
parts of the spectrum one finds
\begin{equation}
B_r^2 = 4\pi A \; \frac{\alpha_2-\alpha_1}{(\alpha_2-1)(1-\alpha_1)} \; .
\label{Bvariance}
\end{equation}
Finiteness of the correlation length requires stronger constraint,
$\alpha_1<0$. One then has
\begin{equation}
L_c = {\pi\over 2 q_c}\,{(\alpha_1-1)(\alpha_2-1)\over \alpha_1\alpha_2}\; .
\label{correlationlength2}
\end{equation}
If $0<\alpha_1<1$, the correlation length diverges at small momenta
and is dominated by the largest possible distance scale in the
problem. Deflections of cosmic rays are most significant in this case.

\subsection{A physical picture and observables}
\label{sect:picture}

A toy model leading to the PWS with the break is illustrated in
Fig.~\ref{fig:scheme}. Here the turbulent magnetic field is contained
within the bubble-like structures. Denote by $L_E$ the typical size
of the largest energy-containing eddies, which is also called an outer
scale of turbulence or energy injection scale. It is often assumed
that $L_E$ corresponds to a typical size of the supernova remnants, and
that inside eddies the PWS corresponds to MHD or Kolmogorov
turbulence. With the assumption that fluctuations in different
``bubbles'' are uncorrelated, the corresponding correlation function
can be approximated as
\begin{equation}
\begin{array}{ll}
\xi(r) = R^{2/3}_E - r^{2/3} \quad &\mbox{at $r<R_E$},\\
\xi(r) = 0 & \mbox{at $r>R_E$},
\end{array}
\label{xiEddies}
\end{equation}
where $R_E = L_E/2$. Using Eq.~(\ref{correlationlength}) we see that
the correlation length of the magnetic field fluctuations is related
to the scale $L_E$ as $L_c = L_E/5$. Similar expression for the
correlation function can be also obtained from Eq.~(\ref{variance})
assuming Kolmogorov spectrum, $\alpha_2 = 5/3$, with infrared cut-off
at a momentum scale $q_c \sim 2\pi/L_E$.
\begin{figure}
\epsfig{file=scheme.eps,%
width=200pt
clip=}
\caption{Schematic view of the turbulent field and the underlying geometry.
At small angles, $\theta < \theta_c = L_E/D$, there are correlated
fluctuations along the entire length of the lines of sight. At large angles
only neighboring structures contribute to correlations.}
\label{fig:scheme}
\end{figure}

In this example the 3d correlation function is zero at large
separations.  In general, however, the fluctuations may be present on
large scales as well. This is the case, e.g., when the Kolmogorov
turbulence is contained not within the ``bubbles'' as above, but
within long sheets or filaments. When substantial power is present in
fluctuations up to the largest scales, the correlation length may
diverge.

Three-dimensional power spectrum of the magnetic field fluctuations,
${\cal B}(q)$, and the corresponding 3d correlation function are not
measured directly.  Instead, one measures the parameters of the
two-dimensional angular correlation function $K(\theta)$ of some
physical observable which can be, e.g., the intensity of the polarized
synchrotron radiation or Faraday rotation measure along different
directions, see Sect.~\ref{observations} for examples. For such
observables the relation between 3d correlation function and the
angular correlation function involves integration along the line of
sight as illustrated in Fig.~\ref{fig:scheme}. For example, in the
case of Faraday rotation measure of extragalactic sources such
relation reads
\begin{equation}
K(\theta) \propto \int_0^D dr_1 dr_2 \;
\xi_{\rm RM}^{~}(|\bf{r}_1-\bf{r}_2|).
\label{volume2angle}
\end{equation}
The directly measurable quantities are the structure
function
\begin{equation}
\frac{1}{2} \, S(\theta) = K(0) - K(\theta) ,
\label{SF}
\end{equation}
and the two-dimensional power spectrum $C_l$ which at
small angles is related to $K(\theta )$ by the Hankel transform
\begin{equation}
K(\theta ) = \frac{1}{2\pi}\int_0^{\infty}C_l\,{\rm J_0}(l\theta )\; ldl .
\label{Cl1}
\end{equation}
Here the multipole $l$ corresponds to a typical angular scale of $\theta =
\pi/l$.

In the case of the power-law behavior of the power spectrum,
Eq.~(\ref{Bpws1}), both $S(\theta)$ and $C_l$ also follow power laws,
$S(\theta) \propto \theta^\beta$ and $C_l \propto l^{-\gamma}$. In
a certain range of $\alpha$ (see Appendix~\ref{apendix} for
details) the three exponents are related as
\begin{eqnarray}
\label{KandC1}
&& \beta = \alpha, \\
&& \gamma =  \alpha+2 .
\label{KandC2}
\end{eqnarray}
Eq.~(\ref{KandC1}) is valid when $0 < \alpha < 2$. When the
correlation length is finite, $K(\theta) \rightarrow 0$ at
sufficiently large angles, and the structure function approaches
constant (cf. Eq.~(\ref{SF})). Therefore, $\beta_1 = 0$ for any
negative $\alpha_1$. On the other hand, at negative $\alpha$ the
relation (\ref{KandC2}) holds. Making use of these two relations, the
exponent $\alpha$ can be deduced from the observable quantities $\beta$
and $\gamma$. However, systematic observational effects (e.g., Faraday
depolarization and finite beam width in the case of polarized
synchrotron radiation) should be absent or accounted for.

The momentum scale $q_c$ at which the break in ${\cal B}(q)$ occurs is
not observed directly either. Instead, one observes the break in the
power-law behavior of $S(\theta)$ at some angular scale $\theta_c$ (or
the break of $C_l$ at some multipole $l_c$). The scale $q_c$ can be
estimated using the relation $l_c = Dq_c/2$, or
\begin{equation}
q_c = \frac{2\pi}{\theta_c D}\; ,
\label{qs_t}
\end{equation}
see Appendix~\ref{apendix}. These relations involve another unknown parameter,
the propagation distance in the magnetic field, $D$.  Fortunately, in the
expression for the cosmic ray deflections $q_c$ and $D$ enter as the product
$q_cD$, so the result can be conveniently expressed in terms of the observable
parameter $\theta_c$.

In the model of Fig.~\ref{fig:scheme}, the structure function at small angular
scales $\theta < \theta_c = L_E/D$ should reflect Kolmogorov turbulence,
$\beta_2 = 5/3$. On larger angular scales the structure function should
gradually become flat, $\beta_1 \rightarrow 0$. The correlation function in
this case decays on large scales as $K(\theta) \propto \theta^{-1}$, which
corresponds to $C_l \propto l^{-1}$ \cite{Cho:2002qk}.  In other words,
existence of small (compared to $D$) correlation length corresponds to
$\beta_1 = 0$ and $\gamma_1 = 1$.

\section{Observations of random component of GMF}
\label{observations}

Current knowledge of the Galactic magnetic field is based on: (i) Faraday
rotation measurements of Galactic and extragalactic radio sources, (ii)
starlight polarization data, and (iii) observations of diffuse Galactic
synchrotron emission. Different methods are sensitive to the magnetic field in
regions with different physical conditions. Faraday rotation is sensitive to a
field in a warm ionized medium, stellar polarization measurements sample the
field in regions occupied by interstellar dust grains, while synchrotron
radiation originates from regions containing fast electrons.

Faraday rotation measure (RM) is sensitive to the projection of the
magnetic field on the line of sight. The field direction along the
line of sight is given by the sign of RM. The magnitude of the random
field $B_r$ can be estimated by analyzing the deviations of RM from
the uniform field along different directions.

Stellar and synchrotron polarization data contain information about
the field perpendicular to the line of sight. This property is
convenient for our purposes since the plane-of-the-sky component of
the magnetic field determines also the deflections of UHECR primary
particles. The ratio of the amplitudes of the random to the uniform
magnetic field components can be estimated along a single
direction. To extract the power spectrum one has to study angular
correlation function of the polarization data.

\subsection{The relative strength of uniform and random fields}
\label{BrBu}

{\it Synchrotron emission.} The total magnetic field strength is
related to the synchrotron emissivity, while the polarization of the
Galactic diffuse synchrotron background offers a method for
determining the ratio of uniform to random field strengths. Namely,
the observed fractional polarization $p_{\rm obs}$ along a given
direction obeys \cite{Ginzburg}
\begin{equation}
\frac{p_{\rm obs}}{p_{\rm max}} =
\frac{B^2_{u,\bot}}{B^2_{u,\bot}+B^2_{r,\bot}} \; ,
\label{FracPolarization}
\end{equation}
where the subscript $\bot$ on $B_u$ and $B_r$ refers to the
plane-of-the-sky components of uniform and random field,
respectively. In Eq.~(\ref{FracPolarization}) $p_{\rm max}$ is the
fractional polarization that would be observed for a perfectly uniform
field, $p_{\rm max} \approx 0.72$. The fractional polarization of
$p_{\rm obs} \approx 35\%$ was found in Ref.~ \cite{Spoelstra} to be a
typical maximum for our Galaxy. This implies
\begin{equation}
B_{u,\bot}/B_{r,\bot} \approx 1 \; .
\label{BratioSynch}
\end{equation}
Note that this ratio depends upon direction. For instance, in the
direction of the Galactic anti-center $p_{\rm obs} \approx 20\%$ (being
averaged over $-20^\circ < b < 20^\circ$), which corresponds to
$B_{u,\bot}/B_{r,\bot} \approx 0.62$.  The typical coherence length was
estimated in Ref.~\cite{Spoelstra} to be less than $75$ pc, while the
distance to the region where polarized emission originates was found
to be about $\sim 0.5$~kpc.

{\it Starlight polarization.} Polarization in starlight appears
because of selective absorption by interstellar dust grains whose
minor axis is aligned with the magnetic field $\bf{B}$.  The same
expression, Eq.~(\ref{FracPolarization}), is valid for the starlight
polarization data as well (with $p_{\rm max}$ being related to dust
extinction). The resulting magnitude of the random component of
magnetic field derived from the starlight polarization data is
consistent with Eq. (\ref{BratioSynch}). For example, the estimate of
Ref.~\cite{Fosalba:2001wr} reads $B_{u,\bot}/B_{r,\bot} \approx 0.8$.

{\it Faraday rotation.} Unlike polarization data, the Faraday rotation
measure is sensitive to the magnetic field component parallel to the
line of sight. Another disadvantage of this method is that it does not
allow to find the ratio of random to uniform components of the
magnetic field along a given direction. However, this information can
be extracted from the residuals of a fit to a uniform field provided
RMs in many neighboring directions are known. For instance, such kind
of study for a particular region of the sky of about $10^\circ \times
10^\circ$ centered at $(l,b) \approx (140^\circ,-40^\circ)$ was
carried out in Ref.~\cite{Minter}.  It was found that $B_r \approx
B_u$, in agreement with Eq.~(\ref{BratioSynch}).

\subsection{The power spectrum of magnetic field fluctuations}
\label{obs:pws}

{\it Synchrotron emission.}  The statistical properties of polarized
synchrotron emission depend upon direction on the sky and are
different for different observables.  In Ref.~\cite{Giardino:2002qi}
the angular power spectra (APS) of the Parkes survey of the Southern
Galactic plane at 2.4 GHz were analyzed. It was found that in the
multipole range $40<l<250$ ($0.7^\circ<\theta<5^\circ$)
the APS of $E$ and $B$ components of the polarized signal has the
slope $\gamma \approx 1.5$, and the power spectrum of polarization
angle corresponds to $\gamma \approx 1.7$.
Similar results were found in
Refs.~\cite{Bruscoli:2002fp,Baccigalupi:2000pm} for other Galactic
latitudes.  In particular, while being close to $1.5$ on average, the
slopes of $E$ and $B$ components in the multipole range $l<1000$
($\theta>10'$) were found \cite{Bruscoli:2002fp} to be in the range $1
< \gamma < 2.7$ depending on the particular region of the sky and the
survey used.

Negative values of $\alpha$ (derived with the use of
Eq.(\ref{KandC2}), if applicable) indicate that in many sky patches
the correlation length of magnetic field may be small.

{\it Starlight polarization.}  The angular power spectrum of the
starlight polarization for the Galactic plane data ($|b| < 10^\circ$)
is consistent with $\gamma \approx 1.5$ for all angular scales $\theta
> 10'$ (or $l<1000$), see Ref.~\cite{Fosalba:2001wr}.

{\it Faraday rotation.}  Structure functions of the rotation measure
of extragalactic radio sources were studied in
Refs.~\cite{Simonetti1,Simonetti2,Minter,Clegg,Sun:2004mt}. Three
different sky patches were considered in Ref.~\cite{Simonetti1}. In
two patches the index $\beta_1$ of the structure function of rotation
measure was found to be consistent with zero on large angular scales
$> 2^\circ$, while in the third positive $\beta$ was observed. There
is a clear drop in the structure function on small angular scales
$\theta < 0.1^\circ$, \cite{Simonetti1,Simonetti2}. Therefore, the
break in the spectrum has to be at angular scales $0.1^\circ <
\theta_c < 2^\circ$ ($\theta_c$ cannot be quantified more precisely as
there are no data points at these intermediate angular scales).

In Ref.~\cite{Sun:2004mt} shallow (with $\beta_1 < 0.3$) structure
functions in several sky regions near the Galactic plain were found over the
range $0.3^\circ < \theta_c < 10^\circ$. Similar result was obtained in
Ref.~\cite{Clegg}.

Minter and Spangler \cite{Minter} have studied structure functions of
RM from polarized extragalactic sources for a particular region with
previously mapped emission measure of warm ionized medium. In this
paper fluctuations in electron density were factored out and the power
spectrum of fluctuating magnetic field was determined. The spectrum of
random magnetic field derived in Ref.~\cite{Minter} can be
parametrized by Eq.~(\ref{Bpws}) with $A \approx 4.5\times 10^{-2}\;
\mu G^2$.  At large scales the angular structure function is
consistent with the two-dimensional turbulence, $\alpha_1=2/3$, while
at small scales $q>q_c$ the spectrum coincides with the Kolmogorov
turbulence $\alpha_2=5/3$. The break in the spectrum occurs at
$\theta_c \sim 0.07^\circ$ which corresponds to $2\pi/q_c \approx
3.6$~pc assuming $D = 3$~kpc. With the parameters found in
Ref.~\cite{Minter}, Eq.~(\ref{Bvariance}) gives $B_r \approx 1.6\; \mu
G$. Note that for the uniform component of the magnetic field in the
same region one has $B_u \approx 2.2\; \mu G$ and $B_{u,||} \approx
-0.8 \; \mu G$.  The slope of $\alpha_1=2/3$ was measured up to
$2\pi/q\sim 80$~pc. Thus, in this particular sky patch the
correlation length of magnetic field fluctuations either diverges or
is larger than 80~pc.

Power spectra and the structure functions of the rotation measure
of the diffuse Galactic polarized radio background in several sky
patches near the Galactic plain were studied in
Ref.~\cite{Haverkorn:2003ad}.  Angular power spectra show a spectral
index $\gamma_1 \approx 1$, while the structure functions are
approximately flat, $\beta_1 \approx 0$ in the range $0.1^\circ <
\theta < 10^\circ$. This is indicative of the field uncorrelated on
large scales.  The structure functions may show a break at $\theta_c$
close to $0.3^\circ$, which is at the same spatial scales ($\approx
3.9$ pc assuming a path length of 600 pc) as a break in the structure
function in the RMs of extragalactic sources of Ref.~\cite{Minter}.
Note that the RM of extragalactic sources probes the complete line of
sight through the Galaxy, whereas, as a result of depolarization, the
synchrotron emission observed at low frequencies only probes the
nearby interstellar medium. In a similar study \cite{Haverkorn:2004fw}
in anther sky region, a shallow structure function of the rotation
measures was found, $\beta_1 \approx 0.2$ for $4'< \theta < 5^\circ$,
while at smaller angular scales the structure function steepens.

\section{UHECR deflections in the random magnetic field}
\label{deflections}

In this section we show that the knowledge of the ratio
$B_{u,\bot}/B_r$, the exponents $\alpha_1$ and $\alpha_2$, and the
angular scale $\theta_c$ is sufficient to quantify the spread of
deflections of UHECR primaries caused by the random component of GMF.
As we have seen in Sect.~\ref{BrBu}, the existing observations suggest
that the magnitudes of the random and uniform components of GMF are
comparable. In what follows it will be convenient to normalize the
deflection due to the random field to the deflection $\delta_u$ which
would occur in the uniform field over the same distance and at the
same particle energy and charge.  After traveling the distance $D$ in
a uniform magnetic field, a particle with the electric charge $Ze$ and
energy $E$ is deflected by an angle \footnote{To be precise, the
product $D B_{u,\bot}$ should be replaced by the integral along the
line of sight $\int_0^D dx, B_{u,\bot(x)}$. This subtlety is
particularly important for directions close to the Galactic plane.}
\begin{equation}
\delta_u = {ZeD\over  E}\, B_{u,\bot}  \;.
\label{DeflBu}
\end{equation}
This has to be compared to the mean square deflection angle
$\delta_r$ in the random component of the Galactic magnetic filed.

\subsection{Mean square deflection in terms of magnetic field power spectrum}

Deflections of UHECR primaries by random magnetic field were studied
in many papers, see e.g. Refs.~%
\cite{Berezinsky:1989ji,Blasi:1998xp,Sigl:1998dd,Achterberg:1999vr,%
Stanev:2000fb,Casse:2001be,Yoshiguchi:2002rb,Aloisio:2004jd}. However,
usually the main focus is the diffusive regime in the extra-galactic
magnetic field.  Deflections in the turbulent component of GMF were
studied in Refs.~\cite{Harari:2002dy,Harari:2002fj}, with the emphasis
on the possibility of magnetic field reconstruction with future high
statistics cosmic ray data. A generic turbulent component of GMF with
a simplifying assumption of a cell-like structure was also included in
the Monte-Carlo simulations of Ref.~\cite{Prouza:2003yf}. To our
knowledge, estimates of UHECR deflections in the random field based on
measurements of the MF power spectra in specific sky patches do not
exist in the literature. The UHECR deflections in the situation when
the coherence length is not small (which might be relevant for the
case of realistic GMF) was not studied in detail either.

Propagation of UHECR primaries in the Galaxy is quasi-rectilinear,
with typical deflection angles not exceeding $10^\circ-20^\circ$ even
for lowest energies. The contribution of turbulent field in these
deflections is expected to be even smaller.  Therefore, a ballistic
approximation gives a good description of UHECR propagation. In this
regime, the deflection angles are characterized by the following line
integrals,
\begin{equation}
\delta_i = {Ze\over E} \int_0^D dz \; \epsilon_{ik} B_k (z)\; ,
\label{theta}
\end{equation}
where the axis $z$ is chosen along the particle trajectory and indices
$i,k=1,2$ label two orthogonal directions. The mean square deflections are
\begin{equation}
\delta_r^2 \equiv
\langle \delta_i\delta^i\rangle
= {Z^2e^2\over E^2} \int\!\!\!\int_0^D dz\, dz'
\;\epsilon_{ik}\epsilon_{jp} \langle B_k (z) B_p (z')\rangle \; .
\label{theta2}
\end{equation}
Here the average is taken over the ensemble of different realizations
of the turbulent magnetic field $B_a(x)$. For a statistically
homogeneous random field the correlator in Eq.~(\ref{theta2})
is  the function of $r = z'-z$
\begin{equation}
\epsilon_{ik}\epsilon_{jp} \langle B_k(z)B_p(z')\rangle =
\xi_{11}(r) + \xi_{22}(r) \equiv \xi_{\bot}(r)\; ,
\label{isotropic}
\end{equation}
where $\xi_{ii}(r) \equiv \langle B_i (z) B_i (z+r)\rangle$ (no
summation over $i$).  Using Eq.~(\ref{BB*}) which enforces the
divergence-free constraint one finds
\[
\xi_{\bot}(r) = 4\pi\int_0^\infty  {dq \,  \over q} {\cal B}(q)
\left[\frac{\sin (qr)}{qr}+\frac{\cos (qr)}{q^2r^2}-\frac{\sin (qr)}{q^3r^3}
\right] \; .
\]
This relation implies
\begin{equation}
\int_0^{\infty}dr\; \xi_{\bot}(r) = \frac{1}{2}\int_0^{\infty}dr\; \xi(r) \; .
\label{Lxibot}
\end{equation}
Note that the assumption of chaotically oriented magnetic cells, which
is often made, would give instead $\xi_{\bot}(r)= (2/3)\; \xi(r)$.
However, this assumption is inconsistent with the divergence-free
nature of the magnetic field.

Changing variables in Eq.~(\ref{theta2}) from $z$, $z'$ to $r$ and
$u=(z+z')$ one obtains
\begin{equation}
\delta_r^2 =  {2Z^2e^2\over E^2} \;B^2_r
\int_0^{D} du \int_0^{u} dr\; \frac{\xi_{\bot}(r)}{\xi(0)}\; ,
\label{theta3}
\end{equation}
where Eq.~(\ref{Br}) was used.  It is convenient to represent the
result as a ratio of rms deflections in random field to the deflection
in the uniform field $\delta_u$ given by Eq. (\ref{DeflBu}). Thus,
we arrive at Eq.~(\ref{thR_thU_Def})
where the dimensionless factor $R$ is
\begin{equation}
R^2 \equiv \frac{2}{D^2} \;
\int_0^{D} du \int_0^{u} dr\; \frac{\xi_{\bot}(r)}{\xi(0)}\; .
\label{R_Def}
\end{equation}
This factor varies between zero  and one.

If the correlation length $L_c$ defined by
Eq.~(\ref{correlationlength}) is much smaller than the propagation
distance $D$, the upper limit in the integral over $r$ can be extended
to infinity. One then finds
\begin{equation}
R^2 =   \frac{L_c}{D} \; .
\label{thetaLc}
\end{equation}
In the general case, the expression Eq.~(\ref{R_Def}) can be brought to the
form
\begin{equation}
R^2 =
\frac{4\pi}{D\xi(0)}
\int_0^\infty  {dq \,  \over q^2} {\cal B}(q) \,f(Dq)\; ,
\label{theta2-fin}
\end{equation}
where
\begin{equation}
f(x) = {\rm Si}(x) + \frac{\cos x}{x} - \frac{\sin x}{x^2}\; ,
\label{functionF}
\end{equation}
and~ ${\rm Si}(x) = \int_0^x dy\, \sin(y)/y$ ~is the integral sine
function.  At small arguments the function $f(x)$ grows linearly as
$f(x) = 2x/3 + O(x^3)$, while at $x\mathrel{\gtap} 2\pi$ it rapidly converges to
the asymptotic value $\pi/2$.

\subsection{Mean square deflections in the random component of GMF}
\label{finalresults}

With the assumption that the power-law spectrum of the turbulent
magnetic field is given by Eq.~(\ref{Bpws}), as supported by the
existing observations, Eq.~(\ref{theta2-fin}) gives
\begin{eqnarray}
\label{Rgeneral}
&&R^2=\frac{(\alpha_2-1)(1-\alpha_1)}{(\alpha_2-\alpha_1)}\;\times\\
&&\left[(Dq_c)^{\alpha_1-1}\,\int_0^{Dq_c} {dy f(y)\over y^{1+\alpha_1}}
+(Dq_c)^{\alpha_2-1}\,\int_{Dq_c}^\infty {dy f(y)\over y^{1+\alpha_2}}
\right]\; ,
\nonumber
\end{eqnarray}
where $f(y)$ is defined in Eq.~(\ref{functionF}). As one can see, the final
result depends on the product $Dq_c$. Therefore, with the use of
Eq.~(\ref{qs_t}) it can be rewritten in terms of the single directly observable
scale $\theta_c= 2\pi/Dq_c$.

In the case $Dq_c \gg \pi$ and $\alpha_1 <0$ (when both integrals are
saturated at $y=Dq_c$), we recover Eq.~(\ref{thetaLc}),
\begin{equation}
R =\sqrt{\frac{L_c}{D}} =
\sqrt{\frac{\theta_c}{4}\,
\frac{(\alpha_1-1)(\alpha_2-1)}{\alpha_1\alpha_2}} .
\end{equation}
For $\alpha_1$ varying within $0.2 < \alpha_1 < 0.8$ and
$\alpha_2=5/3$ (which corresponds to the Kolmogorov turbulence), there
exists an approximate analytic expression for $R$ which holds with an
accuracy of about 10\%,
\begin{equation}
R \approx (Dq_c)^{(\alpha_1-1)/2} = (\theta_c/2\pi)^{(1-\alpha_1)/2}\; .
\end{equation}
In the general case the factor $R$ has to be calculated numerically. Its
dependence on $\alpha_1$ for $\alpha_2=5/3$ in three cases $\theta_c=6^\circ$,
$\theta_c=0.6^\circ$ and $\theta_c=0.06^\circ$ is shown in Fig.~\ref{fig:Ra}
by the dotted, dashed and solid lines, respectively. We recall now that in
many ``low'' resolution all-sky studies the steepening of APS is not
detected, up to large multipoles, $l\sim 1000$. This suggests that $\theta_c <
10'$ and the dashed line in Fig.~\ref{fig:Ra} may serve as an  upper
limit for the factor $R$.

The labeled data-points in Fig.~\ref{fig:Ra} represent the data based
on the Faraday rotation measurements. The corresponding survey regions
are shown in Fig.~\ref{fig:regions} as colored patches labeled in the
same way as the data-points by A (Ref.~\cite{Minter}), B1,B2
(Refs.~\cite{Simonetti1,Simonetti2}), C1,C2
(Ref.~\cite{Haverkorn:2003ad}), D (Ref.~\cite{Haverkorn:2004fw}) and
E1,E2,E2 (Ref.~\cite{Sun:2004mt}). Only in the region A the transition
to the Kolgomogorov turbulence was detected at the scale $\theta_c
\sim 0.07^\circ$.  Though in some other regions an indication for the
break was observed, the transition to the spectra with $\alpha_2 > 1$
was not established. The corresponding limits on $\theta_c$ are shown
as downward arrows.  As explained in the Appendix~\ref{apendix}, any
negative $\alpha$ corresponds to $\beta = 0$ in the structure
functions. Therefore, we plot data-points with $\beta = 0$ as downward
arrows at $\alpha_1 = 0$ turning to the left (pointing to the region
of negative $\alpha_1$). Finally, in the regions C1,C2 both the
structure functions and the APS of rotation measure were obtained
\cite{Haverkorn:2003ad} resulting in $\beta \approx 0$ and $\gamma
\approx 1$.  This allows to specify $\alpha_1$ in these regions as
$\alpha_1 \mathrel{\ltap} -1$.
\begin{figure}
\epsfig{file=Ra.eps,%
width=230pt
clip=}
\caption{The coefficient R as a function of $\alpha_1$ is shown by dotted,
dashed and solid curves for $\theta_c=6^\circ, ~0.6^\circ$ and $0.06^\circ$
respectively. The data-points correspond to the APS derived for sky regions
A-E, as discussed in the text. These regions are displayed in
Fig.~\ref{fig:regions}. }
\label{fig:Ra}
\end{figure}

Small observed values of (or upper limits on) $\theta_c$ indicate that
either the scale $2\pi/q_c$ is small, or the extent of GMF along given
direction, $D$, is large. In either case the resulting coefficient $R$
is small, $0.02 < R < 0.2$. Note that the application of
Eq.~(\ref{thR_thU_Def}) to the directions along the Galactic plane
should be done with care. Namely, deflections in the regular field
cannot be approximated by a simple relation (\ref{DeflBu}), but should
be replaced by the integral along the line of sight. Existing field
reversals can diminish deflections in the regular field considerably.

\begin{figure}
\epsfig{file=mfregions.eps,%
width=230pt
clip=}
\caption{Regions A-E in Galactic coordinates where the break in
the APS was detected. Corresponding values of $R$ for these
regions are shown as data-points in Fig.~\ref{fig:Ra}. }
\label{fig:regions}
\end{figure}

\section{Conclusions}
\label{conclusions}

Deflections of UHECR in the random component of the Galactic magnetic field
are usually discussed in the limit when the correlation length $L_c$ is much
smaller than the propagation distance $D$. However, even in this limit both
the correlation length and the propagation distance in GMF (and therefore
typical deflections) vary with direction. Moreover, the existing GMF data
suggest that the assumption of small correlation length may not be valid
uniformly all over the sky.

We have calculated deflections in a more general approach which does not
require correlation length to be small and relies directly on the spectrum of
GMF fluctuations measured in a relatively small patch of the sky.  Our method
therefore automatically takes into account variations of the GMF
characteristics with direction.  We have shown that the ratio of the
deflections in the random and uniform components of GMF,
Eq.~(\ref{thR_thU_Def}), is expressed in terms of the factor $R$ which depends
on the spectrum of the magnetic field fluctuations as given by
Eq.~(\ref{theta2-fin}). For the power-law spectrum with a single break the
factor $R$ can be written as a function of one directly observable parameter
$\theta_c$, the angular scale of the break in the relevant structure function.
In the case of a small correlation length one finds $R \sim \sqrt{\theta_c}$.

Using the measurements of the GMF power spectrum in the sky regions
where it is available, we have shown that the deflections in the
random component are small, $0.03-0.3$ of the deflections in the
uniform field, see Fig.~\ref{fig:Ra}. This is sufficiently small not
to preclude identification of sources of UHECR using methods of
Refs.~\cite{Tinyakov:2001nr,Tinyakov:2003nu,Tinyakov:2001ir}. For
instance, the deflection of a proton with energy $E=4\times 10^{19}$
eV due to the random component of GMF is expected to be about
$0.2^\circ - 1.5^\circ$ depending on the direction. This is below the
resolution of the AGASA experiment, but can be above the resolution of
the HiRes detector in the stereo mode and the expected resolution of
the Pierre Auger experiment. Thus, the detailed study of the random
component of GMF is particularly important for the interpretation of
data which will be collected by the new generation of UHECR
experiments. To this end, the all-sky map of the essential parameters
determining the power spectra of GMF is highly desirable. These maps
may be obtained from the measurements of Faraday rotation and maps of
diffuse polarized synchrotron Galactic emission.

\section*{Acknowledgments}

We are grateful to S. Dubovsky, D. Grasso, M. Haverkorn and V. Rubakov for
useful comments.  The work of P.T. is supported in part by the Swiss Science
Foundation, grant 20-67958.02 and by IISN, Belgian Science Policy (under
contract IAP V/27).

redpajama_set_name: RedPajamaArXiv


Recreation in natural areas has been promoted for numerous reasons (e.g., health, nature appreciation, education, financial gain) and leisure time spent in protected areas has increased substantially in popularity in recent decades. However, upkeep of such protected areas represents considerable financial outlay and to recoup these costs, tourism potentially provides a self-financing mechanism for ecological sustainability. In Australia, the adventure sport of canyoning has increased in popularity in the Blue Mountains National Park (Australia), part of a recently declared World Heritage Area, in parallel with an overall increase in wilderness recreation. This study sought canyoners' perceptions of visit impacts, together with their attitudes to potential management of these unique areas. It also compares findings with American wilderness research outcomes. The results identify that the current level of traffic through the canyons was not considered to be detrimental to canyon visit enjoyment. While the findings were broadly similar, even at much lower visitation levels than American wilderness recreationists tolerate, Australian canyoners avoid heavily trafficked canyons. Although perceptions and attitudes differed with level of experience, overall, the conclusion is that the visitors encountered were tolerant of other canyoners and the discarded debris of past excursions. In this context, it is not surprising that most canyoners did not see an immediate need to implement further management restrictions.


text:
Maggie Claypool
Imagination's journey unfolds one word at a time
Winter Blahs, Book Review — First Night, Short Story — Well…The Lock is Smart
I Might Need an Attitude Adjustment
Winter is approximately 19 days old. I've had enough.
The days are getting longer. That's something.
That's all I got.
Book Review: First Night by Carol Sabik-Jaffe
First Night, by Carol Sabik-Jaffee, takes place over two short days. As promised, it's a romance where two people coincidentally (or IS it coincidentally?), literally, run into each other and end up spending most of New Year's Eve and New Year's Day together.
As is fitting with such a whirlwind tale, the prose is fast flowing, keeping this an incredibly light and breezy read. At times, the choice of descriptive words is quirky, but it seems mostly in keeping with the nature of the main character Maria Vigliano.
We quickly see two sides to Maria. There's New York Maria who is uptight, constantly doubts herself and her skills/talents, and is fearful that at any time she'll suddenly lose her job. Then, there's Philly Maria, who is a take charge, sometimes rash, firecracker. Maria is very grounded by her large extended family and upbringing, and although she initially makes a case for not adhering to her helicopter mother's rules for living, she's consciously aware of them at all times.
Maria's background differs from that of her New Year's romance, Hunter Reed whose parents divorced when he was young. At that time, Hunter asked to be sent to boarding school and his parents were good with that because it allowed them to start new lives. The closeness of Maria's family is something Hunter has never experienced before, and it enhances his attraction to Maria.
Hunter is only in Philly for New Year's because a cleaning woman, Olympia, in his D.C. office convinces him that he needs to go out, and so he takes a train to meet up with his Penn State buddies to party and go to the First Night Ball. Maria, who professed that she would rather hole up in her small NYC apartment, yields to pressure from her mother to help with her family's Mummers Parade preparations, and heads to Philly on a train. Both trains are delayed by some undisclosed problem on the tracks at Wilmington, DE (possibly a body on the tracks), and so they run into each other at the 30th Street Station when they're rushing to get cabs.
Then Maria's cousins (girls who go "woooo"), talk her into going to the First Night Ball where, after travailing a series of wacky events trying to get there, a friend sneaks them in. She and Hunter meet up again, and share a small New Year's kiss, but then Maria steals a horse carriage when she learns her father has been injured and is in the hospital. The Woooo Girls are still with Hunter and his friends, and so Hunter and Maria are reunited, and share another, much more romantic, early morning carriage ride before Maria has to take over preparation for her family's Mummers Parade performance.
At this point, Olympia shows up again. She helps Maria get costumes ready, and lectures Maria on letting people help her. Then when they run out of materials, and Maria goes to fetch more, Olympia somehow completes all the remaining costumes and disappears. She shows up again to save the day at the parade, too.
The book never explains who – or WHAT – Olympia is, but I believe some clues are laid Hopefully, in the promised Sequel, A Second Chance, we'll not only see how Maria and Hunter's romance develops, learn whether the Woooo Girls continue to see Hunter's friends, and get introduced to the social climbing Holly back at Maria's office; but, we'll also finally learn about Olympia.
This is a very entertaining read, and I look forward to the sequel!
Well. . .The Lock is Smart
Brenda opened the front door to see what the UPS driver had just dropped off on her porch. She wasn't expecting any deliveries and so had no idea what it could be. She found two relatively small packages of exactly the same size and weight. She looked to see who they were from. "What the. . ." she said quietly to herself.
One was from TruLok, and the other was from SikreTech. She already knew what was inside, but she opened them both to verify, and, as expected, she found identical keyless entry smart locks. Exasperated, she got online to see if she'd been charged for the double order. What she found was that TruLok had refunded her money for the original lock she'd purchased that had failed six months after she'd purchased and installed it. But, there were no additional charges on her credit card.
"What a screw-up," she said out loud. She definitely wanted one of the locks because she hadn't yet found a new one. But, it wasn't right to keep them both and the refund. So, although the last thing she wanted to do was spend another four hours on the phone with TruLok and SikreTech, she decided to do the right thing and tell TruLok that they could reverse the credit or whatever they needed to do. So, she pulled up the email that had her help desk ticket number in it and dialed TruLok's number.
After being on hold 12 minutes, a cheery voice with a Latino accent said, "Thank you for calling TruLok. My name is Hector. How may I help you today?"
Brenda replied, not as cheerily, "Hello, Hector. My ticket number is 78ZHIT45B1."
"Okay, let me check that. Hmmm. Nothing comes up. Let me make sure I wrote that down right: 78Z81T45B1. Yes?"
"No. 7. 8. Z. H as in Hector. I as in me, myself and I. T4581."
Hector paused, and then said, "Uhm, I got 78ZH, but not the rest of it."
"T4581."
"Okay, let's do that again." A couple seconds later, Hector said, "No, still nothing. 78ZHT4581."
Brenda sighed. "You left out the 'I" that follows the H as in Hector."
"78ZHIT4581?"
"Yes," Brenda replied, relieved.
"Okay, let's see. Oh, yes, I see. Your 1083Z Smart Lock stopped working."
Brenda interrupted, "Yes, but, hold on. . ."
"Please hold. I'll be right with you."
About a minute later Hector came back on the line and said, "The problem you describe is with the electronic portion of the lock, and so, we need to transfer you to SikreTech for the troubleshooting. Please hold, and I will transfer you."
"HECTOR!" Brenda yelled.
"I don't need to talk with SikreTech. Well, at least not yet. Let me tell you what happened."
Hector replied, "Miss, I cannot help you. It is better you let me transfer you to get the best customer service."
Brenda said in her most authoritative voice, the one she reserved primarily for the office, "Hector, you need to listen to me. Please. I do not need to talk with SikreTech or anyone else. I need to speak with you."
"Okay," he said reluctantly.
"I already went through troubleshooting with SikreTech. They said that the brain of the lock is defective, and that the whole lock has to be replaced. But, they didn't have any more in stock, so they said I needed to call TruLok back and tell you that I needed a replacement lock."
"Oh, Miss," Hector interrupted. "I cannot just send you a lock."
"Well, apparently, you can because you did, but that's not what I'm asking you to do."
Hector said, "But, you just said you were calling to tell us to send. . ."
Brenda jumped in with, "Hector, please just listen to me. I already called TruLok and asked for the replacement lock. I spoke with someone named Carlos, and he put in the request to send me a replacement lock."
"Soo," Hector began.
More loudly: "Hector, listen. Two weeks later, TruLok sent me a letter telling me that all the 1083Z locks were out-of-stock, and that TruLok would be issuing me a refund."
"Well, then," Hector said sadly, "I am sorry, but I cannot help you get a lock if there are no locks."
Brenda growled, "Hector I'm not asking you for a lock. I need to talk with someone about reversing the refund because I now have two locks and you refunded my money, too."
Brenda heard Hector whisper to someone else, and the only word she understood was "loca."
"Yes, Hector," she said loudly, "I am loca because I'm trying to fix the screw-up your company made."
Hector said hurriedly, "I am transferring you to customer service."
Brenda heard a ringing sound and then a recording that said, "You have reached TruLok's customer resolution office. Please hold for the next available specialist."
"I'm giving you no more than two minutes to pick up," Brenda grumbled.
A few seconds later, an Asian voice said hurriedly, "This is Jenny. How may I help you?"
"Jenny, TruLok, has made a mistake."
"Made a mistake? How?"
Brenda laughed, "Well, I don't really know how they made the mistake, but you've sent me two locks and refunded my credit card."
"You got two locks?"
"Yes. Delivered today."
"Then there is no mistake. Two locks means two charges on your card."
"Oh my God," Brenda exclaimed. "You're not understanding me. I bought a lock. It didn't work. You said there were no locks and were giving my money back. Then you sent two locks."
"You sure two locks came from TruLok?"
Slowly, knowing in her heart this was a trap, Brenda said, "No. . .one of them came from SikreTech."
"TruLok is not responsible for what SikreTech sends. We only bill you for our lock. So, the mistake is not with TruLok. I will transfer you to SikreTech."
"No!" Brenda yelled. "I'm not saying this well, and you're not understanding me. TruLok made the mistake that I'm trying to get fixed right now on my credit card."
"There is no mistake," Jenny said impatiently.
Brenda knew she should've just given up at that point, but Jenny's attitude pissed her off. "Let me speak to a supervisor, please," Brenda said crisply.
"It will make no difference. Supervisor will say the same thing."
"Let.Me.Speak.To.A.Supervisor.Please," Brenda said through gritted teeth.
She heard something that sounded like someone slapping the phone's speaker, and then Jenny said. "Supervisor here. What is your problem?"
"Jenny, I know that's you," Brenda said.
"Not Jenny. I'm Jenny's supervisor."
"No, you're not. Please get me a supervisor immediately."
"Why do you want to get me in trouble, Karen?" Jenny demanded.
Brenda took a deep breath and said, "I don't want to get anyone in trouble. I'm just trying to get someone who will understand the mistake."
Brenda heard Jenny and a couple other people speaking in another language, and then Jenny said ,"I transfer you to Supervisor Alice."
"Thank you, Jenny."
Another Asian sounding woman immediately came on the phone and said, "Hello. Do you have a ticket number?"
Brenda sighed and said, "Yes. It's 7. 8. Z as in Zoo. H as in Happy. I as in. . .igloo. T as in Tom. 4. 5. 8. 1."
Alice said, "Glue? I don't understand."
"No, I. I!"
"No I? I didn't have I!"
Brenda said, "Let me try one more time. 7.8.Z.H.I.T.4.5.8.1."
"That's not what you said the first time."
"That's the ticket number, Alice. I was trying to make sure you understood the letters."
"Why do you think I don't understand letters? I speak fluent English!"
Brenda said wearily, "Yes, yes, you do Alice. Would you please look up my ticket?"
"Oh, I see. Something is wrong with the electric lock. You do need to talk with SikreTech."
"No, Alice, I don't."
"Yes, you do. I am transferring you now."
Brenda looked at her phone in amazement, and was getting ready to just hit END, when a voice with a European accent said, "Thank you for calling SikreTech. How may I help you today?"
Brenda said to herself, "Okay one more try." To the SikreTech representative she said, "Let me give you my ticket number."
"No, need, Ms. Garrett. It came across when TruLok transferred the call."
"Huh, well I guess then that Jenny and Alice were shining me on," Brenda replied bitterly.
"Never mind," Brenda said quickly. "Let me just get my story out, okay?"
"Certainly," came the courteous reply.
Feeling hopeful, Brenda spit out, "Okay, so I bought a lock. It failed. TruLok said it was SikreTech's responsibility. SikreTech said that it couldn't be fixed and that TruLok needed to send me a new lock. I called TruLok, they said they'd send a lock. Then they said there were no locks, and they were refunding my money, which they did. Then I got a lock from TruLok and a lock from SikreTech."
"Hmmm," said the nameless SikreTech representative. "I show no lock issued to you from SikreTech."
"Well, I have a lock that shows it was shipped from Norway by SikreTech."
"No, we did not send you a lock."
"From the SikreTech Distribution Center in Bergen, Norway."
"No. Not ours. Our records are impeccable."
"Really," Brenda said. "So, somebody else in Bergen, Norway just decided to send me a $300 lock out of the blue and made it look like it was from SikreTech."
"I would not presume the source. All I can tell you is that we did not send it."
"Why would someone send a SikreTech lock and make it look like SikreTech sent it?"
"I would not presume the motive. I assure you it did not come from SikreTech. We cannot take back a lock we didn't issue."
Sardonically, Brenda replied, "Well, I guess I have some Norwegian secret admirer."
The SikreTech rep said arrogantly, "Again, that is not a matter on which I will comment. As for the other lock and the refund, you'll have to talk with TruLok about that."
"Yeah, that ain't happening." Brenda growled.
In a somewhat more helpful tone the rep said, "I understand your frustration. You should never have been transferred here. I will not transfer you back to the customer service center. Instead, I will transfer you to their administrative offices in Davenport, Iowa, USA."
"Okay," Brenda said unsure.
"Thank you for your business, and have a lovely day. I'm transferring you now."
A man with a Midwest accent immediately picked up the call, "Hello. TruLok USA! My name is Tom. How may I help you?"
"Did my ticket number transfer with the call?" Brenda demanded.
"Yes, it did. Am I speaking with Brenda Garrett?"
"How are you today, Ms. Garrett?"
"Tom, that is not a freaking question you want to ask me right now. I have been around the world for the past hour on this call. You guys made a mistake, and I'm trying to rectify it. Let me tell you quickly what the issue is."
"Oh, no need, Ms. Garrett, I see it all here."
"No, I don't think it's all there."
Tom said, slightly less upbeat, "I promise you it is. And, we're going to take care of this right now. I'm going to put you on hold for just a moment. Now, don't you go away!"
"For the love of God."
Two minutes later Tom came back on the line. "Okay," he cheerfully said. "I've put the order in, and it should be delivered within a week."
"No, Tom, you're not understanding the problem. There's a refund. . ."
"Ms. Garrett, I'm sorry, but our warranty specifically says that we will replace the lock if there is a replacement available, which there is. I'm sorry, but we cannot issue a refund for your lock. Do you want the replacement lock?"
Brenda was quiet for just a moment, laughed and said, "Sure. Send another lock."
mmclaypool
2 responses to "Winter Blahs, Book Review — First Night, Short Story — Well…The Lock is Smart"
Denise Sisofo
I laughed out loud to this
Thanks for reading it!


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She is also very good at drawing fouls. Ranked as the No.


I would like to rsvp for chamber luncheon – having difficulty with paypal? My paypal accouont is tied to an obsolete phone number and there is no mechanism for contacting paypal to change a phone number.
Can I bring a check.
I noticed the old Robinson home on Old Hickory Blvd. is being fenced off and prepared for some type of demolition. Can you tell me if the house will become part of development and what this will entail?
The house will remain as a sort of club house for a retirement age community being built around it.
You can contact John Shepard for more info: (615) 922-2218 or jshepard@elmingtoncapital.com.
Old Hickory Area Chamber of Commerce, Proudly powered by WordPress.


Though he's best known as the onetime voice of CNN, James Earl Jones now says his heart belongs to rival MSNBC.
During an interview with Tavis Smiley and Dr Cornel West, the actor said he "can't get enough of" the far-left cable talk network. Jones also said he is known to "even venture into the right-wing talk shows sometimes".
West then interjected with the idea that Jones is seeking to discover why the other side is wrong, which didn't meet with any objection by the guest.
The Star Wars actor then went on to disparage Tea Party activists by comparing them to his "racist" grandmother, who supposedly instilled expert knowledge on the subject to a young Jones.
via The Radio Equalizer: Brian Maloney: James Earl Jones: I Can't Get Enough MSNBC.
When Barack Obama asserted – in advance of a jury trial or grand jury investigation, let alone a completed police investigation – that he identified with young Trayvon Martin, the black teenager shot and killed in Florida, it was an extraordinarily reactionary moment with possible ramifications of interference with the justice system.
But it was not surprising.
Since obtaining the presidency, Barack Obama has led a Democratic Party that would be better called The Society for the Preservation of Racism.
via Roger L. Simon » Obama, the Democrats, and The Society for the Preservation of Racism.
Obama has benefited from the specter of racism and would have never climbed so high had he not been at least half black. He's the first affirmative action president and you can't blame him for promoting racism. Perpetuating a skewed reality of race relations and discrimination against minorities will allow charlatans like Obama to advance without requiring him to demonstrate any real effort or talent. So we're stuck with this empty suit till the end of 2012. Will the nation have enough since to give this goof his walking papers?


illinois state board of education job openingsMusic education is really helpful for children and adults. Ersen, Ahmet, Alper Ünlü, and Ahmet Güleç. 2004. Façade conservation of an early 20th century apartment creating in Istanbul. ODTU Mimarlik Fakultesi dergisi = METU Journal of the Faculty of Architecture 20 (1-2): 77-92. Caldenby, Claes, and Ola Wedebrunn, eds. 2010. Living and Dying in the Urban Modernity: Denmark, Estonia, Finland, Iceland, Latvia, Lithuania, Norway, Sweden: Nordic-Baltic Experiences. København: Docomomo Denmark Royal Danish Academy of Fine Arts, School of Architecture.
This is where all the accounting goes on to preserve track of the debt. All the states have to send reports to Washington D.C. Washington D.C. has to send reports to the (GAO). Take a look at your state Comptroller's Annual Report to the Governor of your state. I found it in the library located in the city of the corporate state capital. Appear beneath Trust Fund" for each and every state sub-corporation like the state courts, IRS, Banks, Education, and so forth. you will be amazed at the quantity of cash being pumped into the Trust Fund from the different Corporate State Departmental Revenues (all revenue is referred to as taxes: fines, costs, licenses, and so on.). There are millions and billions of your hard earned worthless federal reserve notes, dollars", becoming held in trust."This money is being siphoned off into the coffers of the International Bankers although the corporate government officials are hounding you for a lot more and a lot more tax dollars.
Cowell, Elspeth. 1994. The Canadian Pavilion at the 1939 New York World's Fair and the improvement of Modernism in Canada. Bulletin (Society for the Study of Architecture in Canada) 19 (1): 13-20. Esher, Lionel. 1981. A Broken Wave: The Rebuilding of England, 1940-1980. London: Allen Lane. Sexton, Randolph Williams. 1929. The Logic of Contemporary Architecture: Exteriors and Interiors of Contemporary American Buildings. New York,: Architectural Book Publishing Organization.
board of educationThe State Board of Education does not help organizations making use of the Washington State Achievement Index to concern a series of A – F- grades for schools. Croci, G., A. Viskovic, A. Herzalla, M. Erdik, M. Akdoğan, G. de Canio, and L. Antonelli. 2010. Seismic assessment by numerical analyses and shaking table tests for complicated masonry structures: The Hagia Irene case study. In 7th International Conference on Structural Analysis of Historic Constructions: Strengthening and Retrofitting. ed. Xianglin Gu and Xiaobin Song. 777-82. Advanced Supplies Study vol. 133-134. Stafa-Zuerich and Enfield, N.H.: Trans Tech.
ings from the early 20th century: The case of Ortigia: Corso Matteotti. In Architettura e materiali del Novecento: Conservazione, restauro, manutenzione: Atti del Convegno di studi, Bressanone 13-16 luglio 2004, edited by Guido Biscontin and Guido Driussi, 411-20. Scienza e beni culturali 20. Marghera-Venezia: Arcadia ricerche. Jackson, Lesley. 1998. Modern: Architecture and Interiors of the 1950s. London: Phaidon Press.
Goodstein, Ethel S. 1988. Modern architecture and Canadian national identity. American Evaluation of Canadian Research 18 (2): 127-59. 1951 – On Could 18, throughout a joint meeting with the American Law Institute in Washington, D.C., the UCC was authorized. Later that year the ABA formally approved the code as nicely. Considered the outstanding accomplishment of the Conference, the Code remains the ULC's signature product.
Baxter, Alan. 2001. Twentieth-century buildings. Journal of Architectural Conservation 7 (two): 27-30. Casciato, Maristella, and Emilie d'Orgeix, eds. 2012. Modern day Architectures: The Rise of a Heritage. Wavre, Belgium: Mardaga. Barry, Robin. 2001. The Building of Buildings. New York: Wiley. Mansbach, S. A. 2006. Modernist architecture and nationalist aspiration in the baltic: Two case studies. Journal of the Society of Architectural Historians 65 (1): 92-111.
Gatley, Julia. 2010. The heritage identification of modern day public housing: The New Zealand instance. Journal of Architecture 15 (five): 683-96. Powys, A. R., and Society for the Protection of Ancient Buildings (London England). 1929. Repair of Ancient Buildings. London: J.M. Dent & Sons, Ltd. Smith, Elizabeth A. T., and Esther McCoy. 1998. Blueprints for Modern day Living: History and Legacy of the Case Study Houses. 1st MIT pbk. ed. Los Angeles Cambridge, Mass.: Museum of Modern Art MIT Press.
Benton, Tim, Charlotte Benton, and Dennis Sharp, eds. 1975. Architecture and Style, 1890-1939: An International Anthology of Original Articles. New York: Whitney Library of Style. Grignolo, Roberta, and Bruno Reichlin, eds. 2012. Lo spazio interno moderno come oggetto di salvaguardia = Modern day Interior Space as an Object of Preservation. Mendrisio Cinisello Balsamo, Milano: Mendrisio Academy Press Silvana.
National Lawyers Guild– PhiladelphiaNadia Hewka nhewka@ The National Lawyers Guild is committed to the need to have for standard and progressive change in the structure of our political and financial technique. Via its members-lawyers, law students, jailhouse lawyers and legal workers united in chapters and committees-the Guild works locally, nationally and internationally as an efficient political and social force in the service of the people. Our aims: to get rid of racism to safeguard and strengthen the rights of workers, ladies, farmers and minority groups, upon whom the welfare of the entire nation depends to preserve and defend our civil rights and liberties in the face of persistent attacks upon them to use the law as an instrument for the protection of the people, rather than for their repression.
Ball, Norman R. 1988. Building Canada: A History of Public Functions. Toronto: University of Toronto Press. Payne, Alina Alexandra. 2012. From Ornament to Object: Genealogies of Architectural Modernism. New Haven: Yale University Press. Cherry, Martin. 1995. Defending industrial buildings: The role of listing. In Managing the Industrial Heritage, edited by Marilyn Palmer and Peter Neaverson, 119-24. Leicester Archaeological Monographs No. two. Leicester: College of Archaeological Studies, University of Leicester.
illinois state board of education addressPsychiatric education has turn out to be a really promising field of medical education. Burman, Peter, Keith Garner, and Leo Schmidt, eds. 1996. The Conservation of Twentieth Century Historic Buildings: Proceedings of a Conference Held at the Institute of Sophisticated Architectural Studies, the University of York, four-six Could 1993. York: Institute of Advanced Architectural Research, University of York. Allan, John. 2010. Private privilege – public duty: Examples of current English knowledge in modern conservation. Journal of Architecture 15 (five): 651-70.
It is Historical information that the original Union States created the Federal Government, nonetheless, for all sensible purposes, the Federal government has taken control of her Creators", the Individuals of the States.) She has turn into a beast out of manage for energy. She has for her trade names the following: United States", U.S.", U.S.A.", United States of America", Washington D.C., District of Columbia, Feds. and Federal Government. She has her own U.S. Army, Navy, Air Force, Marines, Parks, Post Office and so on. and so on. and so forth. Due to the fact she is claiming to be bankrupt, she freely provides her land, her personnel, and the income she steals from the Americans through the IRS. and her state corporations, to the United Nations and the International Bankers as payment for her debt. The UN and the International Bankers use this money and solutions for different globe wide projects, such as war.
Bruegmann, Robert. 1994. Modernism at Mid-Century: The Architecture of the United States Air Force Academy. Chicago: University of Chicago Press. Longstreth, Richard. 2012. A Historical Bibliography of Architecture, Landscape Architecture, and Urbanism in the United States considering that Planet War II. Evansville, IN: Recent Past Preservation Network. Benevolo, Leonardo. 1971. History of Modern day Architecture. 2 vols. Cambridge, Mass.: M.I.T. Press.
The Bankers said, Appear. You can do it either of two methods. The effortless way or the difficult way." You just accept the bankruptcy and we'll let you out of the depression. If you do not, you're on your own." So all the countries involved agreed, simply because they realized that the International bankers had them by the throat. The nations as a result agreed that more than a period of several years that they would pass statutes and legislation for the implementation of the bankruptcy in favor of the international bankers.
Johnson, Donald Leslie. 1980. Assessment of 20th Century Architecture: Notes for Conservationists. Canberra, A.C.T.: Australian Heritage Commission. British Requirements Institution. 2005. BS 6576:2005: Code of Practice for Diagnosis of Rising Damp in Walls of Buildings and Installation of Chemical Damp-Proof Courses. London: BSI. Cavalcanti, Lauro. 2009. The role of Modernists in the establishment of Brazilian cultural heritage. Future Anterior: Journal of Historic Preservation History, Theory and Criticism 6 (two): 14-31.
Amongst the principal aims of the Getty Conservation Institute's Conserving Modern Architecture Initiative (CMAI) is the production of publications and sources that will assist in advancing this field of conservation. In the first edition of Conserving Twentieth Century Built Heritage: A Bibliography, published in the fall of 2011, the editors committed to updating the publication periodically in order to capture the most current literature in this rapidly growing area of conservation practice. To that end, the GCI is pleased to release this second edition, which captures materials published because 2011, as effectively as a number of older functions that had been omitted from the very first edition. The structure of this document follows the original, with minor revi- sions to some of the chapter titles to greater reflect content.
Some of the bibliographies cited above could initially seem to be a lot more comprehensive than the present work. When conservation of twentieth-century heritage very first started to achieve momentum, quite limited literature was available on the topic. The bibliographies made within the English Heritage volumes, for example, captured as numerous documents as could be identified at the time. Given that the mid- 1990s, there has been significantly a lot more scholarship on this problem resulting in a quantity of conference proceedings, articles, and books. The GCI has sought to incorporate this far more recent literature, whilst excluding many of the editorials and short journal commentaries that have been present in the earlier volumes.
Sustainability and Adaptive Reuse (chapter five) gives references to texts, guides, and case studies that clarify principles or give examples of adaptive reuse, as well as power conservation, sustainable practices, and mechanical ser- vices in twentieth-century buildings and structures. Sabbioni, C., Brimblecombe Peter, and Could Cassar. 2010. The Atlas of Climate Adjust Influence on European Cultural Heritage: Scientific Analysis and Management Methods. EC Cultural Heritage Investigation Series. London and New York: Anthem.
illinois state board of education fax numberThe State Board of Education does not assistance organizations making use of the Washington State Achievement Index to concern a series of A – F- grades for schools. Hines, Thomas S. 2010. Architecture of the Sun: Los Angeles Modernism, 1900-1970. New York: Rizzoli. Morton, W. Brown, III. 1976. Field procedures for examining humidity in masonry buildings. Bulletin of the Association for Preservation Technologies 8 (2): two-19. Croci, G., and A. Viskovic. 1993. Causes of the failures of Coliseum over the centuries and evaluation of the security levels. In Public Assembly Structures: From Antiquity to the Present: Proceedings of the IASS-MSU International Symposium, May possibly 24-28, 1993, Istanbul, Türkiye. Istanbul: Mimar Sinan Universitesi.
Bricker, Lauren Weiss, Luis Hoyos, and Judith Sheine, eds. 2007. Engaging the Recent Past. Unique problem. Journal of Architectural Education 61 (2). Here is what is going to very swiftly happen internationally. All of the governments about the planet are going to unite. They will generate one massive giant credit union for collecting the debt for the International Bankers. We have permitted ourselves do get into this quite sad predicament, but THAT IS THE WAY IT IS.
Benente, Michela, and Manuela Mattone. 2004. Gli interventi sull'esistente in occasione delle olimpiadi di Torino 2006: Il restauro come riscrittura" dell'architettura Interventions on current structures on the occasion of the 2006 Olympics in Turin: Restoration as rewriting" architecture. In Architettura e materiali del Novecento: Conservazione, restauro, manutenzione: Atti del Convegno di studi, Bressanone 13-16 luglio 2004, edited by Guido Biscontin and Guido Driussi, 673-82. Scienza e beni culturali 20. Marghera-Venezia: Arcadia ricerche.
International Working-Celebration for Documentation and Conservation of Buildings, Websites and Neighbourhoods of the Contemporary Movement. 1998. Conference Proceedings: Vision and Reality: Social Elements of Architecture and Urban Preparing in the Contemporary Movement. International DOCOMOMO Conference. Stockholm Delft: Swedish Museum of Architecture DOCOMOMO.
Albani, Francesca, Luca Bertolini, Marco Manera, and Fabrizio Valvassori. 2004. La conservazione dei materiali dell'architettura contemporanea: Calcestruzzo armato, pietra e rame in un edificio di Figini e Pollini a Milano The conservation of components in contemporary architecture: Reinforced concrete, stone and copper in a Figini and Pollini constructing in Milan. In Architettura e materiali del Novecento: Conservazione, restauro, manutenzione: Atti del Convegno di studi, Bressanone 13-16 luglio 2004, edited by Guido Biscontin and Guido Driussi, 871-80. Scienza e beni culturali 20. Marghera-Venezia: Arcadia ricerche.
Berlucchi, Nicola, and Cecilia Catacchio. 2004. Restauro di un'architettura moderna a Venezia: La sede del INAIL di Giuseppe Samonà, spunti di riflessione Restoration of a modern day architectural operate in Venice: The INAIL headquarters by Giuseppe Samonà, some aspects to consider. In Architettura e materiali del Novecento: Conservazione, restauro, manutenzione: Atti del Convegno di studi, Bressanone 13-16 luglio 2004, edited by Guido Biscontin and Guido Driussi, 1261-69. Scienza e beni culturali 20. Marghera-Venezia: Arcadia ricerche.
Cohen, Jean-Louis. 2008. Le Corbusier's Centrosoyuz in Moscow. Future Anterior: Journal of Historic Preservation History, Theory and Criticism five (1): 52-61. Hough, Jessica, and Mónica Ramírez-Montagut, eds. 2008. Revisiting the Glass Property: Contemporary Art and Modern Architecture. Ridgefield, Conn. Oakland, Calif. New Haven: Aldrich Modern Art Museum Mills College Museum of Art Yale University Press.
Caneva, Giulia, Daniele Di Stefano, Ciriaco Giampaoloc, and Sandra Ricci. 2004. Stone cavity and porosity as a limiting factor for biological colonisation: The travertine of Lungotevere (Rome). In Proceedings of the 10th International Congress on Deterioration and Conservation of Stone, Stockholm June 27 – July two, 2004. ed. Daniel Kwiatkowski and Runo Löfvendahl. Vol. 1. 227-32. Stockholm: ICOMOS, Sweden.