The old metal Doomwheel I got cheap on ebay. The base is a resin of unknown make, it came with a set of assorted metal skaven also bought on ebay. The flagpole is off a metal stormvermin.
Another excellent Harlequin miniatures Ver'Men. This time an Assassin.
This one has been dipped, dark tone quickshade.


text:
Michael Denzil Xavier Portillo (Bushey, Engeland, 26 mei 1953) is een voormalig Brits politicus van de Conservatieve Partij.

Portillo was tussen 1987 en 1997 bewindspersoon in de Kabinetten Thatcher I, II, III (1987–1990) en Major I en II (1990–1997). Hij was staatssecretaris voor Sociale Zaken van 1987 tot 1988, onderminister voor Transport van 1988 tot 1990, onderminister voor Lokale Overheid van 1990 tot 1992, onderminister voor Financiën van 1992 tot 1994, minister van Arbeid van 1994 tot 1995 en minister van Defensie van 1995 tot 1997. Hij was vice-leider van de Conservative Party onder William Hague van 1999 tot 2001.

Biografie
Hij werd geboren in een gezin met een Spaanse vader, Luis Gabriel Portillo (1907-1993), en een Schotse moeder, Cora Blyth, dochter van de eigenaar van een fabriek waar uit vlas linnen werd gemaakt in het Schotse Kirkcaldy. Zijn vader moest destijds zijn geboorteland Spanje ontvluchten, omdat hij een republikein was, de verliezende partij tijdens de door Franco gewonnen Spaanse Burgeroorlog.

Britse politiek
Portillo werd voor het eerst in het Britse Lagerhuis verkozen in een tussentijdse verkiezing, die nodig was geworden omdat de houder van de zetel was omgekomen als gevolg van de IRA-bomaanslag van 1984 in Brighton. Portillo was een sterke bewonderaar van Margaret Thatcher en een euroscepticus. Portillo diende als staatssecretaris onder zowel Thatcher als John Major. In 1992 werd hij tot minister benoemd. Hoewel hij als een potentiële uitdager werd gezien van John Major voor het leiderschap van de Conservatieve partij bij het lijsttrekkersreferendum van 1995, bleef Portillo uiteindelijk trouw aan Major. Als minister van Defensie drong Portillo aan op een pure Thatcheriaanse politiek van "helder blauw water" om het beleid van de Conservatieven zo veel mogelijk te onderscheiden van dat van Labour. In die context deed hij in 1995 de uitspraak "You can't trust Labour on defence", een uitspraak waaraan hij later nog met enige regelmaat herinnerd werd.

In zijn periode als minister werd Portillo gezien als potentiële opvolger van Major. Tegen wil en dank werd hij echter het symbool voor de afgang van zijn partij bij de verkiezingen van 1997. In de vernietigende nederlaag die de Conservatieve partij leed, verloor Portillo onverwacht zijn veilig geachte zetel aan een jonge Labour-kandidaat. Het moment waarop openbaar werd gemaakt dat hij zijn zetel kwijt was, werd de naamgever voor het zogenaamde "Portillomoment", waarbij een voorname politicus van een partij wordt weggestemd. Het moment werd later gekozen in de top drie van beste tv-momenten ooit. De uitspraak "Were You Still Up for Portillo?" werd ook de titel voor een boek over de nederlaag.

Portillo maakte in 1999 zijn comeback toen hij de zetel van een overleden lid innam. Hij trad daarna weer toe tot het schaduwkabinet. In 2001, nadat William Hague de verkiezingen verloren had, deed hij een gooi naar het leiderschap van de Conservatieve partij, maar hij moest het na een veelbelovende start afleggen tegen Kenneth Clarke en Iain Duncan Smith. De laatstgenoemde werd partijleider. Portillo bleef nog tot 2005 als backbencher in het parlement.

Sinds 2002 was Portillo al werkzaam in het bedrijfsleven. Als bestuurder van de wapenfabriek BAE Systems moest hij in 2006 ontslag nemen om mogelijke belangenverstrengeling te voorkomen. In dat jaar leidde hij enkele maanden het energiebedrijf Kerr-McGee.

Televisie
Sinds hij zich terugtrok uit politiek en bedrijfsleven, houdt Portillo zich bezig met het presenteren van televisieprogramma's. In het bijzonder de BBC-series Great British Railway Journeys en Continental Railway Journeys in 2010-2013 maakten hem populair. Daarin combineerde hij toeristische informatie (aan de hand van Bradshaw's Descriptive Railway Hand-Book of Great Britain and Ireland, editie 1863, respectievelijk Bradshaw's Continental Railway Guide, editie 1913) met beschouwingen over de invloed van de spoorwegen op de economische ontwikkeling van de gebieden die hij bezocht. Deze programma's zijn ook op de Nederlandse en Vlaamse televisie vertoond.

Brits bestuurder
Brits journalist
Brits minister van Arbeid
Brits minister van Defensie
Brits onderminister
Brits ondernemer
Brits presentator
Brits radiopresentator
Brits staatssecretaris
Conservative Party-politicus (Verenigd Koninkrijk)
Lid van het Lagerhuis (Verenigd Koninkrijk)

redpajama_set_name: RedPajamaWikipedia


During Christmastime, Aunt Cammie always without fail busts out tins upon tins of her famous crockpot candies (chocolate clusters stuffed with nuts). They're served at every family gathering, and we end up taking home at least a dozen. My aunt has tinkered with the recipe through the years and has always envisioned making it with higher quality chocolate. She told me, "You can upscale it, and it can be ours!" So that's exactly what I did.
The first slight change I made: I halved the recipe. If you are planning to gift a bunch of people with this, by all means, double it up. But every year my aunt always ends up with a giant surplus, so I figured it would be nice to scale it down to a reasonable amount of candy. FTR, I have served this batch at two get-togethers and still ended up with enough chocolate for one more party.
Next, toast the nuts in the oven. Raw nuts, no matter what some may tell you, do not taste as good as toasted nuts. With a firmer, crunchier texture and roasted flavor, toasted nuts are the way to go.
In addition, I opted for roasted, salted peanuts. A little salt with chocolate is heaven; however, if you really can't stand the sweet-salty combo, simply opt for roasted, unsalted peanuts. No harm done. I threw those into the crockpot first, followed by chocolate (three varieties: milk, semisweet, and bittersweet), followed by the toasted nuts, which act as a heating blanket to the top half of the chocolate.
The cover goes on, and the crockpot does all the hard labor for you.
What's so awesome about a crockpot is it slowly melts the chocolate evenly without burning it. Once the chocolate has melted down, give it a quick stir. Your work here is almost done.
Dole out the chocolate clusters onto wax paper using two teaspoons. The hardest part is letting the chocolate set, which can take several hours and up to overnight. That's why you should go ahead and get a third teaspoon out to scoop out a "sample." You won't be disappointed!
If you double the recipe, you will need to increase the cook time to 2 hours.
This recipe is really versatile — use your favorite nuts or chocolates. Make it dairy-free or peanut-free, depending on your family's and friends' needs.
Layer ingredients in slow cooker. Cook on low for 1 hour, or until chocolate melts. Do not open lid. Watch time carefully — do not overcook (or else chocolate will burn and stick). After 1 hour, stir mixture.
Cook 2 minutes and then stir again.
Drop by spoonfuls onto wax paper. Let harden completely before transferring to an airtight container.


You are here: How to become an Administrator?
Responsibilities Completing forms, taking internal phone calls, creating reports and organising data. .
What do I need to do to become an Administrator?
Administrators can work in most sectors of the job world. Whether it's for a retail business, transport company, hospital, school, university or travel company, you'll be working hard to make sure all administrative duties are taken care of so the business can run smoothly.
The average pay for an administrator in the UK is £17,158 per year, with salaries normally ranging between £13,083 and £23,317. According to the website payscale.com, salaries do not directly increase in line with years of experience. So administrators with lots of experience do not earn significantly more than those just starting out. However, this role gives you many transferable skills that will help you gain higher paying jobs in the admin industry, or in other sectors of work.
The content of your day-to-day duties will often depend on the type of company that you work for. But common tasks will include completing forms, taking internal phone calls, creating reports and organising data. Administrators may also have some customer-facing duties, such as taking and processing customer orders, dealing with customer issues or complaints, arranging postal deliveries and bookkeeping.
So, how do you land a job as an administrator? Vacancies are often advertised on specialist job boards or on the career page of a large company's website. When applying, make sure you read through the advert fully. Then show how you meet the main points in their criteria on your CV and your cover letter, or on the online application form. Even if you don't meet all of their requirements, it is still worth applying, as long as the job is within your experience remit. There is no use in applying to be the manager of an admin team, if you've never done the job before.
When you get invited to interview, it's essential that you arrive on time and give a great first impression. Be polite, smile and try not to show that you're nervous. After all, an interview is just as much for you to gauge whether you want to do the job, as it is for a potential employer to meet you.
In the modern world, computer skills are vital for any administrator. This includes strong typing and numeracy skills, data entry, computer-based record-keeping and more. This role naturally suits highly organised characters. This means you are able to sort through and process information, and do not need someone checking over all of your work for mistakes. A keen eye for detail and the ability to manage your own workload will also help. You also need to be able to communicate effectively. This includes written and verbal communication with your team and others in the company.
Any experience you have working in an office, answering phone calls or keeping records, will be useful when applying for administrator jobs. When writing your CV and in an interview, also be sure to highlight any examples you have of working well in a team. Working in an administration department, or even if you're the company's only administrator, you'll be working with a wide range of employees.
Employers will also be looking to see that you are capable of meeting deadlines and key performance indicators (KPIs). If you haven't worked in a similar role, think of examples that might show this.
You don't need any formal qualifications for most administrator roles. However, if you want to, you could consider a business degree or business-related national vocational qualification (NVQ). Training provider City & Guilds has information about lots of work-based qualifications on their website. You can choose to start at different levels of NVQ depending on your education and experience in the workplace.
Once you're settled into a new admin role, your daily duties will often start with reading, replying and following up emails. It is likely that most of your work, whether it's communicating with colleagues or customers, will be done via email. Keep your inbox tidy, create labels and anything else that will keep you as organised as possible. Assess your workload for the day and prioritise the most important things. You'll also be supporting other members of staff, and, if you have a customer-facing role, you'll also be attending to phone calls.
If this is your first ever job or first role in the administrative sector, you may start as an admin assistant. This usually means working with a supervisor who will guide you and help manage your workload. It's a great place to get your foot on the ladder and start learning; for most office-based careers it will teach you lots of transferable skills that can be used in a variety of industries.
Once you've got a few years of experience under your belt, or less if you're motivated, you can look to move up to an administrator role, and then progress to a senior administrator. If you like the company you're working for, you can look for internal job vacancies that could expand your skillset. You're more likely to be successful if you've already proven you're hard-working, reliable and an asset in your current role. And sometimes it's necessary to side-step in order to move up.
If you are intending to make a career in the administration world, you may want to think about specialising in a certain sector, such as a legal or medical administrator.
As well as job-specific transferable skills, you'll also develop important soft skills that will be useful in any workplace. These include interpersonal skills, such as liasing with colleagues, sourcing help when you need it and learning how to work well with different types of people. Listening skills and learning how to express an alternative opinion in a professional way is also something you may learn.
Working as an administrator can sometimes feel like a thankless task, and sometimes you may not receive direct praise or credit. But don't let this stop you, keep in mind your own goals, realise when you've done something well and bare in mind what sort of skills you're learning.
This is a great role for anyone starting out in the world of work, and a place to improve your IT and interpersonal skills. Starting out as an admin assistant or administrator doesn't have a clear career path but you can take it into whichever sector interests you, or look at moving on to marketing, human resources, project management or secretarial work.


The EURLs –SRM/FV are pleased to invite the NRLs-SRM/FV to the EURL/NRLs Workshop 2018.
The Workshop will be held in Almeria, Spain, from the 27th to the 28th September 2018, at the Hotel Barceló Cabo de Gata (Retamar, Almería-Spain).
In order to facilitate your travel, the EURL-FV can assume directly the cost of the hotel booking and the flight tickets for those eligible participants. Please fill in the form with your data and your preferences and we will book everything for you through our travel agency, so no expenses will have to be reimbursed.
Non-eligible participants will have to book by themselves.
The Workshop Venue will be at the Hotel Barceló Cabo de Gata. There are near hotels to this one. The EURL-FV will try to fix all the eligible participants in this one. The hotel will offer special prices for non-eligible participants in the venue hotel, please check in the workshop webpage.
A bus service will be offered to the eligible participants from the airport to the hotel and back.
Certified analytical standards: current situation and future.
If you decide to stay extra days in Almería, please be aware that the hotel and any other expenses that you may have during those extra days will not be reimbursed.
We hope that we sparked your interest and that you will participate in this workshop. We are looking forward to welcoming you in Almeria.
Click here to download the Preliminary Agenda.
Click here to download Venue Info.
The total amount of the booking must be paid directly at the hotel. The price includes taxes.
No shows before 18:00 hrs on the booked day of arrival shall be charged the amount corresponding to 100% of the total booking.


text:
Home Entertainment News Rappler Rappler Talk Entertainment: Julia Barretto on 'Between Maybes'
Rappler Talk Entertainment: Julia Barretto on 'Between Maybes'
MANILA, Philippines – Black Sheep – the studio that is fast gaining a reputation for creating love stories that hit viewers right in the feels – is gearing up to release Between Maybes, an upcoming film by Jason Paul Laxamana featuring the unexpected but altogether intriguing pairing of Julia Barretto and Gerald Anderson.
In many ways, the film hits all the marks for a romantic movie: boy meets girl in a time of crisis, the chemistry is instant, they fall in love, and it all plays out against a stunning backdrop of a foreign land.
In the film, Julia plays Hazel Ilagan, an actress who takes a break from her overwhelming life to go to Saga, Japan. There she meets Louie Puyat, a man who has had to deal with the deportation of his parents. They meet and eventually start a romance – but only until Hazel has to go home.
In this interview, we chat with Julia about her role, what it was like to film in Japan, how it was working with Gerald, and what she thinks makes the film more than just a romantic movie.
Catch the conversation by bookmarking this page or heading to fb.com/rapplerdotcom. – Rappler.com

redpajama_set_name: RedPajamaCommonCrawl


text:
Watch Captain Underpants Online
Watch Captain Underpants 2017 Online, Captain Underpants Putlocker, Two mischievous kids hypnotize their mean high school principal and turn him into their comic book creation, the kind-hearted and elastic-banded Captain Underpant..Watch Captain Underpants Online,
Captain Underpants 2017 Cast and Crew
Director David Soren
Writers Dav Pilkey (book), Nicholas Stoller (screenplay)
Cast Kevin Hart, Nick Kroll, Kristen Schaal
Captain Underpants 2017 Synopsis
"Captain Underpants Full Movie" The "Captain Underpants" book series tells the story of two mischievous kids, George Beard and Harold Hutchins, who hypnotize their school principal and turn him into their comic book creation, Captain Underpants. Scholastic first launched the "Captain Underpants" book series in September of 1997 and there are over 50 million Pilkey books in print in the U.S. alone. Eight "Captain Underpants" books have been published in 19 countries and several have debuted at #1 on various best-seller lists
Captain Underpants Hindi dubbed,


There are a plethora of top 10 tips on how to get your day off to a successful start, such as waking early, getting in your morning workout, eating a healthy breakfast, and planning and strategizing for the day.
What about some of the more obscure morning habits of successful people?
How many of us spend countless minutes each morning trying to decide what to wear, only to step out in the bright sunshine realizing you've paired black socks with brown shoes, or the tie you picked does not fit the color profile of your suit.
According to Jason Abbruzzese at Mashable.com, some of the brightest minds of our time, people like Steve Jobs, and Mark Zuckerberg, opted out of a flashy wardrobe and instead chose to stick to the basics, every day.
This gives them more time to strategize on how to take over the world, or, as Mark Zuckerberg was quoted as saying in that same article, "I really want to clear my life to make it so that I have to make as few decisions as possible about anything except how to best serve this community."
If your only motivation for getting out of bed in the morning is a sense of duty, then likely the snooze button will win out over your good intentions. If your morning ritual includes an activity that you actually look forward to and that brings you some pleasure, this could tempt you out from under the covers.
Anna Wintour, editor in chief for Vogue magazine, starts her day with an hour-long tennis match. And Margaret Thatcher woke early to listen the popular morning radio program "Farming Today" to prepare herself for the day.
Both of these successful women custom tailored a morning ritual to fit their desires and needs. So if that morning cup of joe and curling up on the couch to read the newspaper is your push out of the bed, at least you're heading in the right direction.
You tried to get in the groove this morning, rising at 5, getting in your morning jog around the block, but just as you start to prepare your morning smoothie, you get a call. You're needed in the office ASAP.
The project you planned to brainstorm this morning over coffee will need to be conference room ready in an hour. Will you make the most of that 30-minute train ride to work in order to succeed? Successful people don't wait for the perfect circumstance to work.
According to an excerpt from Mason Currey's book "Daily Rituals" at Guardian.com, "One of the most dangerous procrastination-enabling beliefs is the idea that you must find exactly the right environment before you can get down to work." He says that Agatha Christie, for example, never used a desk and could use any stable tabletop for her typewriter.
One of things I do is get in an hour of email and organization in the morning before I head into the office. Knowing what my day will be like before it gets started helps me stay focused and be ready if my schedule happens to change during the day.


More 1983 alumni from Northwestern HS Springfield, OH have posted profiles on Classmates.com®. Click here to register for free at Classmates.com® and view other 1983 alumni.
Alumni from the Northwestern High School class of 1983 that have been added to this alumni directory are shown on this page. All of the people on this page graduated in '83 from NHS. You can register for free to add your name to the NHS alumni directory.


text:
\section{Introduction}

The \pam\ spectrometer \citep{picozza_pamela_2007} is a space instrument designed for the study
of primary charged particles and antiparticles in a wide energy
interval, mainly from tens of MeV to ${\approx}$ 1.2 TeV for protons. It was launched in an elliptical orbit at
an altitude between 350 and 610 km and inclination of 70 degree in June
2006. The main scientific goal of \pam\ is the measurement of the particle and antiparticle component in galactic cosmic rays \citep{adriani_anomalous_2009,
adriani_new_2009}, the study of galactic cosmic ray modulation by solar activity, and
solar energetic particles \citep{casolino_cosmic-ray_2006,de_simone_study_2009}. This paper reports the \pam\ measurements of the solar proton
and helium fluxes in the energy range from below 100 MeV/n to several
GeV/n during the December 13 and 14, 2006 solar particle events.

The problem concerning mechanism and site of solar energetic
particles (SEP) acceleration remains an open question. Certainly, SEP may be produced
 after powerful explosive events on the Sun,
accompanied by solar flares, Coronal Mass Ejections (CME), bursts of
solar X /gamma-rays and radio emission \citep{reames_particle_1999}. It
is clear that not a single mechanism is involved into the SEP generation.
Stochastic acceleration, shock acceleration, and acceleration by the
DC electric fields in the process of magnetic reconnection are the
main candidates. Acceleration of SEP may take place in the flare
region, solar corona and even in the interplanetary space. It should be
kept in mind that SEP themselves, while propagating, create conditions for the energy redistribution
\citep{tylka_new_2001,lee_coupled_2005}. Therefore, the energy spectrum of
SEP provides valuable information for study of solar and interplanetary plasma
processes. Most energetic particles are usually (not always) accelerated
during short time close to the energy explosion, thus the first
particles arriving at the observer site keep more information
about the primary acceleration process. Less energetic SEP may be
accelerated during hours and even days. Conditions for particle
acceleration in the corona and interplanetary space are determined by temporal and spatial evolution of a shock \citep[e.g.][]{ellison_shock_1985}.

Since the energy range of SEP extends over more than 5 orders of
magnitude, and the SEP fluxes occupy more than 8 orders of
magnitude, the SEP energy spectrum has never been measured by a
single instrument. The bulk of the SEP observations has been
performed on spacecraft and covers the particle energy below
several hundreds MeV/n, whereas the relativistic solar particles
have been observed by ground-based installations and remain less
elucidated. This kind of observations and associated modeling can
also be used to issue radiation alerts to be used by manned and
unmanned missions. A multi-detector study of the solar particle
event occurring in 2005 and the corresponding  GLE69 was performed
on-ground using NM and SREM  radiation environment units in space
\cite{astra-7-1-2011}

It is not yet clear if relativistic solar particles require a
special scenario for their generation. Some authors believe that
relativistic solar protons have two components - the fast and the
delayed ones. The fast component is initially accelerated in the
flare region
\citep[e.g.][]{vashenyuk_relativistic_2006,vashenyuk_characteristics_2008,vashenyuk_relativistic_2008,mccracken_two_2008},
probably via magnetic field reconnection, whereas another
mechanism, probably shock or stochastic acceleration, generates
the second particle component.
\cite{bieber_spaceship_2004,bieber_relativistic_2005} argue
against two components and in favour of the CME-driven shock as a
main accelerator of the whole SEP population. A wide variety in
concomitant acceleration conditions supports the point that
various mechanisms play the main role in different SEP events
\citep{bombardieri_improved_2008,bazilevskaya_early_2009}.
Detailed studies of more solar particle spectra in wide energy
range are needed to resolve this problem.

Since ground-based instruments can only detect secondary cosmic rays, knowledge of response to the primary particles is necessary in order to find SEP fluxes in space.
Some methods were developed \citep{shea_possible_1982,cramp_october_1997,bieber_spaceship_2004,plainaki_modeling_2007,vashenyuk_relativistic_2006} to derive energy spectra and angular anisotropy of solar particles using the enhancements in the count rates of neutron monitors. Nevertheless, the particle fluxes derived from the neutron monitor data are model dependent.

Before the \pam\ launch, direct measurements of the relativistic solar particles
were not fulfilled. The aim of this paper is to present the results of
the first direct measurements by a single instrument of the solar
protons in the energy range from 80 MeV to several GeV and the helium
nuclei from 75 MeV/n up to $\sim$ 700 MeV/n during the SEP events of
December 13 and 14, 2006. The absolute intensities and energy spectra
are compared with the results of direct (GOES, ACE) and indirect (neutron monitors, IceTop) measurements.

\section{Instrument Description}

The \pam\ spectrometer (Figure \ref{fig_pam}) consists of a number of highly
redundant detectors capable of particles detection trough the
determination of their charge, mass, rigidity and
velocity over a very wide energy range. Total weight
of \pam\ is 470 kg; power consumption is 355 W.

A more detailed description of the device and the data handling can be
found in \citep{picozza_pamela_2007,casolino_pamela_2006,casolino_yoda++:_2006}. The core of the instrument is a
spectrometer, constituted by permanent magnet with a silicon microstrip tracker
providing momentum and charge (with sign) information
\citep{adriani_powerful_2003}. The permanent magnet is 43.66 cm high and
constructed of 5 modules with high residual magnetic induction (0.43 T)
providing an almost constant magnetic field value in the cavity. The
tracking system \citep{ricciarini_pamela_2007} is composed of 6 planes of
high-precision Si microstrip detectors, positioned between the 5
magnetic modules of the tower, with uniform vertical spacing of 8.9
cm. Each silicon plane performs measurements of energy release and track position with a
precision of about $3.0\; \mu m$ (X - bending view) and $11.5\; \mu m$ (Y
view).

A scintillator system \citep{barbarino_pamela_2003} provides trigger, charge
and time of flight (TOF) information. It is composed of three double
layers S1, S2, and S3, divided in various bars for a total of 48
scintillator paddles. It is also used to reject albedo particles which cross
the detector from bottom to top.

An anticoincidence system (CARD, CAT, and CAS) is used to reject spurious events in the off-line phase.

A silicon-tungsten calorimeter \citep{boezio_high_2002} is used to perform
hadron/lepton separation. It is composed of 44 silicon layers
interleaved by tungsten planes for a total of $16.3\;X_0$ (radiation lengths) and $0.6 \; \lambda_i$ (nuclear interaction lengths).

A shower tail catcher S4 and a neutron detector at the bottom of the
apparatus are used to increase lepton/hadron separation.

Around the detectors are housed the readout electronics, the interfaces
with the CPU and all primary and secondary power supplies. All systems
are redundant with the exception of
the CPU which is more tolerant to failures. The system is enclosed in a
pressurized container located on one side of the Resurs-DK1 satellite.

\section{Data Selection and Analysis Criteria}

\subsection{Geometrical Factor and Top of the Payload correction}
 The Geometrical factor ($G_f$) of the detector has been evaluated defining a
 fiducial area consisting of a frame of $0.15 ~cm$ from the walls of the $13.1\times 16.1~cm^2$ wide magnetic cavity. Only particles inside this fiducial area have been selected. This reduced volume ensures that all particles entering the magnetic cavity
 cross the scintillators and do not hit the magnet walls. The value of $G_f=19.93$ $
cm^2 sr$, constant within $1 \%$, has been estimated
 with a numerical calculation and cross-checked with a Monte Carlo simulation where all the physical interaction processes are
inactive, with the exclusion of particle bending in the magnetic
field. The two values of $G_f$ have been found in agreement within $0.1\%$.

Interactions losses, due to local interactions where taken into account as a scale factor added to the Geometrical Factor. Protons and helium nuclei may be lost due to scattering and/or hadronic interactions in the $2~mm$ Al thick pressurized container in which \pam\ is housed or in the top of the detector.
Correction factors amounts to $\simeq 6\%$ for protons and $\simeq 12\%$ for He due to the different cross section of the two species.

\subsection{Trigger system}

In low radiation regions, close to the geomagnetic equator and outside the South Atlantic Anomaly, where \pam\ crosses the trapped protons of the inner Van Allen belt, particles must cross at least one of the two layers of the three scintillator systems ($S1$, $S2$, $S3$) to provide a valid trigger. In low cutoff regions or in the Van Allen belts, where particle rate is higher, $S1$ signal is not required to avoid random triggers due to the high number of particles.
Given the low energy of solar particles compared to the galactic nuclei, in this analysis we have used particles selected in high latitude regions and thus taken with only ($S2$ and $S3$) configuration.

\subsection{Live Time}

 The live time $t_{live}$
 of the apparatus is evaluated using the scintillator and trigger system.
 The counters for the live and dead time ($t_{live}$, $t_{dead}$) are cross-checked with the on-board time of the CPU, measuring the
 acquisition time ($t_{acq}=t_{live}+t_{dead}$), to remove
 possible systematic errors due the counting method. The error associated with clock resolution is negligible compared to other sources of systematic errors.

\subsection{Event Selection}

\subsubsection{Time of flight system selection}

In this analysis we have selected events that do not produce secondary particles in the $S1$ and $S2$ scintillators and in the tracker, requiring a single fitted track within the spectrometer fiducial acceptance and a maximum of one paddle hit in $S1$ and $S2$ matching the extrapolated from the tracker trajectory.

Particles interacting in the satellite can produce showers with
different secondaries hitting the scintillator pads. These showers
may produce random coincidences in the scintillators: they are rejected
by means of anticoincidence and TOF cuts. We require the absence of hits in the anticoincidences around
the empty area between $S1$ and $S2$ and around the top magnetic
cavity (CARD and CAT respectively).
No constraints
on the anticoincidences around the magnet (CAS) and $S3$ have been put, since they are more often
hit by backscattered secondaries produced in the calorimeter. The
probability for such particles to hit CARD and CAT has
been estimated with experimental data and cross-checked with
Monte Carlo simulations. This efficiency has been included in the proton flux estimation.
No constraints on the anticoincidence have been imposed for helium.

The timing information of the TOF
scintillator paddles along the extrapolated trajectory is used to evaluate the $\beta$ of the particle.
Albedo particles crossing the detector from bottom to top are
discarded by requiring a positive $\beta $.

\subsubsection{Proton and Helium identification}

 Since average energy
loss of a charged particle through matter follows Bethe Bloch formula, $dE/dx
\varpropto Z^2/\beta^2$ (neglecting logarithmic terms), the
measurement of the average energy released in the tracker planes
for a given event at a given rigidity can be used to identify different particles.
Proton and helium candidates have been selected requiring
 energy loss in the
tracker planes compatible with Z=1 and Z=2 nuclei.

Cuts in the energy loss (dE/dx) vs. rigidity remove positrons,
pions and particles with $Z\geq 2$ as shown in Figure \ref{fig_dedx}.
 The bands in the Figure due to protons and helium nuclei which have energy loss in the tracker $Z^2=4$
times protons, are identified. Events with small energy losses
below 1 GV are due to positrons, relativistic also at low rigidities
and the background of secondary pions. The contribution from these two particles are negligble respect to protons above 1 GV. The black
lines show the rigidity dependent cuts used to select the proton and helium
samples. From the same figure the deuterium contribution at low rigidities can also be identified, resulting in a band with
energy releases higher than protons. In this work we did not discriminated between isotopes.

Using the redundancy of energy loss measurements in tracker and TOF, residual contamination of protons in the helium sample has been found to be below 0.5$\%$ in the energy range used for this work.

\subsubsection{Geomagnetic Selection}

The high
inclination ($70^{\circ}$) orbit of the Resurs-DK1 satellite allows particles of different origin and nature to be studied. To separate the primary (solar and
galactic) component from the reentrant albedo component (particles produced
in cosmic ray interactions with the atmosphere below the cutoff
and propagating along Earth's magnetic field line), we evaluated the local geomagnetic cutoff $G$ in
the St\"{o}rmer approximation~\citep{shea_estimating_1987}. The value of $G=14.9/L^2$ - valid for vertically incident particles - is
estimated calculating the McIlwain $L$ shell with IGRF magnetic field model along the orbit~\citep{IGF2011}. Particles were selected requiring $R>1.3
\: G$ to remove any effect due to directionality in the detector and Earth's penumbral regions.

\subsubsection{Tracker selection}

Particle rigidity is obtained fitting it's track in the
spectrometer. In this analysis we selected events with a single track fully contained inside the fiducial acceptance.

For each particle, the tracking system provides up to 12 position measurements
(6 in the bending view), which are interpolated with a trajectory evaluated by integrating the
equations of motion in the magnetic field.
At low rigidies (below $\simeq  1 \:GV $) we have corrected for the energy loss in the detector.

The Maximum Detectable Rigidity (MDR) for a given detector is defined as the rigidity for which the relative error on the rigidity $\Delta R/R=100\%$ and varies between 200 GV and 1.5 TV, depending on delta-ray production and event's topology.
In this analysis, therefore, the particle rigidity is well below the MDR and thus is no MDR requirements have been applied.

\subsubsection{Selection efficiencies and residual contamination}

The tracker efficiency has been measured selecting a sample of
events which leave straight tracks in the calorimeter and do not
interact hadronically. These tracks were propagated back through \pam\ acceptance and tracker efficiency has been evaluated.

The total selection efficiencies for both species has been obtained as a product of Tracker, TOF (anticoincidence) efficiencies. The resulting efficiencies for proton and helium nuclei after all above mentioned cuts are shown in Figure \ref{fig_eff}. For a detail discussion see  \cite{adriani_pamela_2011}.

Although we put strong requirements on Tracker, TOF and anticoincidence systems, nevertheless there is residual contamination of secondary particles produced on the top of the payload entering the \pam\ acceptance window and passing selection cuts. The maximum contribution to the background for protons comes from secondary single-charge particles (positrons and pions). In case of helium, rejection power of our selection cuts is enough to make residual contamination negligible. In order to estimate this contamination we carried out a $2 \pi$ Monte Carlo simulation of the protons and helium nuclei hitting the \pam\ pressurized container. Two different hadronic interactions packages, based on Fluka \citep{battistoni_fluka_2007, ferrari_fluka:_2005} and Geant 4 \citep{allison_geant4_2006, agostinelli_g4--simulation_2003}, have been employed to simulate these interactions. This background decreases with increasing energy and amounts to less than few percents at 1 GV. Flux attenuation was estimated with an energy dependent simulation and it is constant above several GV.

\section{December 13 and 14, 2006 Solar Particle Events}

\subsection{General description}

The most significant SEP fluxes detected by \pam\,
were started on December 6, 13 and 14, 2006 and originated from the active
region NOAA 10930. December 6 event originated at the East limb
resulting in a gradual proton event reaching the Earth on December 7
and lasting until the events of December 13 and 14. Due to a
scheduled maintenance procedure, no data were collected by PAMELA tracker
during December 6 event, requiring a different analysis approach that will be discussed in a forthcoming paper. On December
13 2006, at 0214 UT an X3.4/4B solar flare occurred in the same active
region NOAA 10930 (S06W23) \citep{NOAA2011}. The intensity of
the event was quite unusual for a solar minimum condition.
This event produced also a full-halo Coronal Mass Ejection (CME) with the sky
plane projected speed of 1774 km/s \citep{adata2011}. The forward shock of the CME
reached Earth at 1438 UT on December 14, causing a Forbush decrease of
galactic cosmic ray intensities which lasted for several days.

The flare X1.5 (S06W46) at 2107 UT on December 14 gave
start to a new growth of particle intensity as recorded by \pam\ and
other satellites. The maximum energy of protons was below 1
GeV, therefore no ground level enhancement (GLE) was recorded.
The corresponding CME had a velocity of 1042 km/s.

Figure \ref{fig_time_profile}
shows the solar particles intensity time profiles with
various energies as observed by the \pam\ spectrometer, GOES-11 and neutron monitors.
Ground-based neutron monitors started recording of SEP
at 0248 UT, while the near-Earth satellites responded later to SEP of lower
energies. First solar protons arrived at the Earth's
orbit with anisotropic pitch-angular distribution which resulted in
different intensity-time profiles at neutron monitors situated at
location with the same geomagnetic cutoff $R_c$ but
different asymptotic directions of incoming particles.
A highly collimated bunch of relativistic solar particles was observed by the
muon hodoscope URAGAN at 0256-0304 UT \citep{timashkov_ground-level_2008}.
Anisotropy vanished by 0430 UT \citep{vashenyuk_characteristics_2008}.

The whole energy range of SEP detectable by the \pam\
spectrometer can only be taken in the high latitude regions,
where the geomagnetic cutoff is lower than the rigidity of solar particles.
Measurements were performed during 5 passages of \pam\ through the polar regions on December
13. Data were missed from 1000 UT of December 13 till 0914 UT of
December 14 because of onboard system reset of the satellite.

The results of \pam\ measurement during the December 13 and 14, 2006
SEP events are shown in Figure \ref{fig_13} and \ref{fig_14}
respectively. The quiet time galactic spectra were measured in
November 2006. The first (southern) polar passage of \pam\ started at
0318 UT and showed strongly flattening of p and He spectra at energies $\sim$200 MeV/n. The helium
spectrum in the initial phase of the December 13 event is almost similar in
shape to the proton one, but flatter at energies below 200 MeV/n. In the event of December 13 the initial
spectra were rather hard and changed significantly at least till
1000 UT. Further evolution of the proton and helium spectra was
rather smooth even in spite of a Forbush effect in the middle of
December 14, until arrival at $\sim$2300 UT of the SEP accelerated in
the flare at 2107 UT on December 14. The intensity of $\sim$100 MeV protons
firstly increased till $\sim$0400 UT on December 13 and stayed at almost the same
level for at least 4 hours, while higher energy particles were rather
rapidly removed from the Earth's vicinity. After that, the particle
intensity decreased, but the spectrum shape was almost constant. Flux
intensity did not decrease to the solar quiet levels because of the
onset of December 14 event. During this event spectral form slightly flattened in the lower energy
part thus remaining quasi-exponential. The highest proton energy for
this event was around 500 MeV.

We have examined temporal behavior of proton-to-helium ratio in the both solar events. For this analysis the rigidity spectra were evaluated with rigidity intervals chosen in accordance with \cite{adriani_pamela_2011}. Figure \ref{fig_ratio} presents the proton-to-helium ratio obtained in selected time intervals. The galactic background was not subtracted and is shown as a black curves. It is seen in the left panel of  Figure \ref{fig_ratio} that at the beginning of the December 13 event the ratio was almost the same as for GCR (note that SEP intensity was highest at that time). The subsequent measurements showed the enhancement of He relative to protons up to the late December 14 when the high rigidity He virtually disappeared after subtraction of the galactic flux. Such a behavior may to a first approximation be interpreted as a result of faster removing of solar protons from the Earth's orbit. Protons have higher velocity than He of the same rigidity therefore the diffusion coefficient of He at the same rigidity is smaller and protons leave faster.  Further analysis needs a particle propagation modeling. Right panel of Figure \ref{fig_ratio} clearly shows that no solar helium with rigidity above 1 GV was observed in the event of December 14.

No analysis directed to search of $^2H$ and $^3He$ has been performed yet.
No electrons or positrons of solar origin were found by the
\pam. However, it should be noted that the energy threshold of \pam\ is at $\sim$ 50 MeV, therefore rather high for solar electrons.

\subsection{Initial phase of the December 13, 2006 event}

The first arriving particles are objects of special interest because they provide more information about mechanism and conditions of acceleration. As it was mentioned, solar particles at the initial phase of the December 13 event demonstrated highly anisotropic angular distribution. In such conditions the asymptotic directions of particles arriving at PAMELA should be taken into account.

The geomagnetic field acts not only as rigidity analyzer but also as an angular analyzer of charged particles coming from space. Because of declining in the geomagnetic field a particle with certain rigidity above the geomagnetic cutoff $R_c$ can arrive at a given site only from a definite direction outside the magnetosphere (asymptotic direction). Therefore, at any point of its orbit PAMELA accepted particles with certain rigidity from only one asymptotic direction.

At the moment of the first particle arrival \pam\ was at the
latitude of 40N moving to the equator. Therefore the low energy
particles could not reach the \pam\ detector. In addition, viewing
directions of \pam\ were changed rapidly while the spacecraft
moved along the orbit. This can be seen in the upper panel of
Figure \ref{fig_axis} where the asymptotic directions of 7 GV and
10 GV protons arriving at \pam\ are shown for the initial phase of
the SEP event. The asymptotic viewing directions of \pam\ has been
calculated with the program of \cite{gvozdevsky_b.b._private_2009}
using the back-tracing of solar particle trajectories and the
magnetospheric model of \cite{tsyganenko_model_2002}. It is in
reasonable agreement with \cite{plainaki2009AdSpR..43..518P}
obtained with the Tsyganenko 1989 model. The direction of the SEP
anisotropy axis, i.e. direction from which the bulk of SEP comes
is also plotted \citep{vashenyuk_characteristics_2008}. According
to Figure \ref{fig_axis}, \pam\ viewing directions at the early
phase of the SEP event would allow the solar protons in the range
of 7-10 GV to be recorded by \pam\ at 0248-0250 UT as these
particles arrived within a $\sim$30 degree cone around the SEP
flux axis. However, above 3 GeV the statistic is poor and we have
found no increase of proton flux there. Changes in the viewing
directions of \pam\ resulted in rapid receding of its favorable
direction of acceptance from the solar proton anisotropy axis. By
0256 UT (when a collimated particle bunch was observed by
\cite{timashkov_ground-level_2008}) the geomagnetic cutoff of
\pam\ was 12 GV and only protons with rigidity between 15 and 17
GV could come from directions close to the anisotropy axis.

The lower panel of Figure \ref{fig_axis} shows the asymptotic
directions of particles with different energies arriving at \pam\ in
the beginning of the event and at the most optimal time of observation
when the energy spectrum of particles with energies above $\sim$80
MeV/n was measured. For comparison, the asymptotic directions for the
Apatity neutron monitor and for the IceTop installation \citep{abbasi_solar_2008} are shown in
Figure \ref{fig_axis}.

\subsection{Comparison with other data}

In Figure \ref{fig_comp} the differential spectra of \pam\, with the galactic background subtracted are compared with other experiments. Each panel corresponds to different time period.

In the low-energy range \pam\ particle fluxes can be
compared with other spacecraft measurements. The GOES \citep{GOES2011-1} fluxes are in moderate agreement with \pam\ ones, with exception for the most energetic GOES band (160-500 MeV) where GOES fluxes are several times higher. The same is true for GOES helium spectra. This could be due to contamination of lower energy particles in these GOES channels. On the other hand, the \pam\ helium fluxes are in a good agreement with measurements, performed by ACE/SIS \citep{ACE2011} in the adjacent energy interval.

At high energy, our data can be compared with the IceTop shower array \citep{abbasi_solar_2008} and the NM network\citep{vashenyuk_characteristics_2008}. The results of the IceTop shower array are plotted in Figure \ref{fig_comp}a, b specially taken at the time intervals of \pam\ observations \citep{kuwabara_t._private_2009}. The IceTop installation has detected
secondary particles, generated by the solar energetic particles,
i.e. the calculated yield functions have been used to reconstruct the
primary SEP fluxes. The IceTop results are depicted only in the energy
range over which this detector was actually seeing a significant number of
particles. The SEP fluxes obtained by \pam\ and
those obtained by IceTop is in relatively good agreement. However, at 0318-0329 UT (Figure \ref{fig_comp}a) the
power-law shape of the IceTop spectrum does not match the \pam\
spectrum which is more exponential-like. At 0406-0420 UT (Figure
\ref{fig_comp}b) the spectra of \pam\ and that of IceTop are virtually coincident in
the overlapping energy range.

The energy spectra from the NM network have been derived
from the early phase of the event (before 0300 UT on December 13) till
$\sim$ 0500 UT on December 13 \citep{balabin_yu.v.__2009}. As already mentioned, \pam\ missed the early phase of the event and took the first measurement at 0318-0329 UT,
during mildly anisotropic particle arrival (Figure \ref{fig_comp}a). A shape of the
\pam\ proton spectrum is close to that derived from the neutron
monitor network at energies between 700 MeV and 2 GeV. At lower energies
the \pam\ spectrum is harder; at $E\;>\; 2\,$ GeV the
uncertainty in the \pam\ spectrum is high because of small statistics.
The absolute intensities of protons from \pam\ are somewhat lower than those
derived from neutron monitors even at energies above 1 GeV. To some
extent, discrepancy between the \pam\ and neutron monitor spectra may
be caused by the flux anisotropy.

The GLE parameters for this event have also been calculated using
the NM-BANGLE model  \cite{NMBANGLE2009AdSpR..43..474P}. The
direct comparison of the particle fluxes is difficult since these
data in \cite{NMBANGLE2009AdSpR..43..474P} are given only for
integral energy spectra (see their Figure 3). An estimation shows
that the results of the NM-BANGLE model are very close to the
spectra obtained by \cite{vashenyuk_characteristics_2008} and
therefore differ from the PAMELA results in similar manner.
    Figure
\ref{fig_time_profile}, shows that during the first polar passage
of \pam\ (0318-0329 UT) the Apatity and Barentsburg neutron
monitors demonstrated different rate enhancements, i.e. the SEP
fluxes were still anisotropic. The neutron monitor spectrum refers
to the direction of the anisotropy axis where the proton intensity
is maximal. The \pam\ viewing directions for the protons below 3
GV (see lower panel of Figure \ref{fig_axis}) were not very close
to the anisotropy axis, therefore the \pam\ fluxes may be lower
than derived from neutron monitors. By the next \pam\ polar
passage (0406-0420 UT) discrepancy between the \pam\ and neutron
monitor spectra increased (Figure \ref{fig_comp}b). Since the flux
anisotropy becames lower, one should expect better consistency
between the \pam\ and neutron monitor data. On the contrary,
observations show discrepancy which persisted at around 0500 UT
(Figure \ref{fig_comp}c). Particle fluxes changed slowly at
0800-1000 UT, so in order to increase statistical significance,
the \pam\ results were averaged over 0850-0944 UT (Figure.
\ref{fig_comp}d). By this time the effect on the neutron monitor
network was already too small for determining the solar proton
spectrum. However, the \pam\ results were confirmed by an
independent observation of the LPI balloon-borne detector
\citep{stozhkov_y.i_fluxes_2007} which measured solar proton
energy spectrum in the stratosphere at 0946-1046 UT. Energy of
solar protons is determined in the LPI experiment from absorption
of protons in the air, so this is also a direct measurement of
solar protons although in the limited energy interval
\citep{bazilevskaya_solar_2010}. The good agreement between proton
data of the two instruments in the energy range 90 MeV - 400 MeV
is an additional check that our efficiency and systematics are
under control.

\section{The energy spectrum fitting}
The observed spectral shape may give some indications on
the acceleration mechanism \citep{casolino_two_2008}. The proton
energy spectrum measured in the early phase of the event, which is most
close to the time of primary acceleration (0318-0349 UT), was fitted by
the functions representative of various acceleration processes:

\begin{eqnarray}
\Phi_p = A\; e^{-E/E_0} \label{eq:expkine}\\
\Phi_p = A\; e^{-R/R_0} \label{eq:exprig}\\
\Phi_p = A\; R^{-\gamma-\delta(R-R_0) / R_0} \label{eq:plawmod}\\
\Phi_p = A\; R\;K_2\;(R / c\,\alpha\,T)^{1/2} \label{eq:bessel}
\end{eqnarray}
where $\Phi_p$ is the proton flux intensity, $E$ is kinetic energy, $R$ is magnetic rigidity, c is particle velocity, and $K_2$ is
a modified Bessel function of order 2, with $\alpha\;T$ as free
parameter ($\alpha$ representing an acceleration rate and $T$ the escape
time from the acceleration region). An exponential in kinetic energy (\ref{eq:expkine})
or rigidity (\ref{eq:exprig}) function is typical for simple models of DC acceleration
\citep{vashenyuk_relativistic_2006,vashenyuk_characteristics_2008,vashenyuk_relativistic_2008},
a power law is
indicative of shock acceleration
\citep{axford_acceleration_1981,krymskii_regular_1977,ellison_shock_1985},
and Bessel function is resulted from stochastic
acceleration \citep{mcguire_energy_1984}. The best fit parameters of
approximation are presented in Table~\ref{tabfits}.
\begin{table}[!h]
\centering
\begin{tabular}{|l|l|c|l|c|}

\hline
Function & A, $cm^{-2} sr^{-1} s^{-1} GV^{-1} (GeV^{-1})$ &
\multicolumn{2}{|c|}{Parameters} & $\chi^2 / ndf$\\
\hline
$A \cdot exp(-E/E_0)$ & $(68.2 \pm 0.9) $ & $E_0$, MeV & $(262 \pm 2)$ & 3.0\\
\hline
$A \cdot exp(-R/R_0)$ & $(179 \pm 3)$ & $R_0$, MV & $(366 \pm 2)$ & 7.6\\
\hline
\multirow{2}{*}{$A \cdot R^{-\gamma-\delta(R-R_0)/R_0}$, $R_0=1 GV$} & \multirow{2}{*}{$(13.1 \pm 0.1)$} & $\gamma$
& $(2.70 \pm 0.02)$ & \multirow{2}{*}{4.1}\\
\cline{3-4}
& & $\delta$ & $(1.99 \pm 0.06)$ & \\
\hline
$A \cdot R \cdot (K_2\,(R / c \cdot \alpha \cdot T))^{1/2}$ & $(106
\pm 2)$ & $\alpha \; T$ & $(1.71 \pm 0.01)$ & 6.4\\
\hline
\end{tabular}
\caption{The best fit parameters of the solar proton spectra in the energy interval 80 MeV -- 4 GeV in the early phase of the event (0318 - 0349 UT).}
\label{tabfits}
\end{table}

It should be mentioned that even if the resulting fits reproduce rather nicely
the spectral shape, $\chi^2$ values are high for all of them
 (see Table~\ref{tabfits}), showing that these analytical formulas do
not correctly describe the spectrum in the whole energy range. The best
fit is obtained for the exponential in kinetic energy function (\ref{eq:expkine}), however it
fails to describe the highest and lowest energy tails where the
observed spectrum is harder (in the $R\;>\; 2.5\, GV$ and $R\;<\;1.7$ GV range). It proves that no single mechanism can describe the SEP
energy spectrum in the wide energy interval. The previous successful
attempts of the SEP spectra fitting \citep[e.g.][]{cramp_october_1997,vashenyuk_characteristics_2008} were possible only for narrower energy range.

\section{Discussion and conclusion}

The \pam\ spectrometer was the first instrument which directly measured the
relativistic SEP in the near Earth space. It is important since all previous such measurements were fulfilled with the ground-based installation and the derived SEP fluxes depended on the instrument response functions. The spectra of solar protons in the energy range 80 MeV - 3 GeV and helium 75 MeV/n - 1 GeV/n were measured during the first polar \pam\ passage at 0318-0329
UT. There is a good agreement between the protons fluxes
measured by \pam\ and those obtained by the IceTop installation
\citep{abbasi_solar_2008,kuwabara_t._private_2009}. Keeping in mind accuracy of estimation
of absolute SEP intensities from the neutron monitor data
\citep{vashenyuk_relativistic_2006,plainaki_modeling_2007,bombardieri_improved_2008,NMBANGLE2009AdSpR..43..474P}, reasonable
agreement can be stated between the \pam\ and neutron monitor SEP
fluxes. However, the \pam\ spectra are always harder in the low-energy
interval probably indicating that neutron monitor yield functions are
underestimated below $\sim$700 MeV. During the second polar \pam\ passage the
difference between the SEP fluxes taken from \pam\ and neutron monitors
has become larger while agreement between \pam\ and IceTop remained
very good. The correctness of the \pam\ observations was also confirmed by
agreement with the direct SEP measurement on a balloon in the
atmosphere.

Evolution of intensity and spectral shape of relativistic solar protons
is often used to derive some information about SEP generation
\citep{bombardieri_improved_2008,vashenyuk_relativistic_2006,vashenyuk_characteristics_2008,vashenyuk_relativistic_2008,mccracken_two_2008, moraal_analysis_2008}. The indications were found that the first arriving relativistic particles would be accelerated in the flare region and have an exponential spectrum whereas the latter particles would be accelerated by a CME-driven shock and have a power-law spectrum. In this case an appropriate dynamics of the energy spectrum could be observed by \pam. Being at the low latitudes \pam\ missed the earliest anisotropic phase of the event of December 13. The results of the first \pam\ observation around 0320 UT on December 13 confirmed existence of a hard quasi-exponential spectrum expected from the magnetic reconnection in the flare region. However, in spite of changes in the SEP intensity a quasi-exponential spectrum persisted, actually till the advent of the newly generated protons of the December 14 event. It should be noted that in the energy interval relevant to the neutron monitor observations ($>$ 500 MeV) the spectrum could be fitted by a power law beginning from $\sim$1000 UT, however at lower energies the spectrum was flatter. We did not find any spectral form which would fit the observed spectra satisfactorily in the whole energy range and could prove a certain dominating mechanism of SEP acceleration. A quasi-exponential spectrum and fast temporal evolution of particle fluxes during several hours were present only in the event of December 13 when the relativistic protons were generated. In the event of December 14, without relativistic particles, a form of the solar proton energy spectra changed little and was almost power-law throughout the event. In addition, no Helium with energy above $\sim$100 MeV/n was observed in the December 14 event. This may be indicative of special conditions leading to acceleration of particles up to relativistic energy.

\section*{Acknowledgment}

We acknowledge support from The Italian Space Agency (ASI), Deutsches
Zentrum f\"ur Luft und Raumfahrt (DLR), The Swedish National Space Board, The Swedish Research Council, the Russian Space Agency (Roscosmos) and the Russian Foundation for Basic Research. We thank the IceTop team and the Polar Geophysical Institute cosmic ray group (Apatity) for providing the IceTop and the neutron
monitor spectra at the times of \pam\ measurements, the ACE SIS
\ instrument team and the ACE Science Center for providing the ACE
data. Our thanks are also to all people who make their results
accessible through the Internet.
\bigskip

redpajama_set_name: RedPajamaArXiv


Discussion in 'Programming' started by Architheutis, Apr 16, 2019.
I created a patrolling knight with rusty amour. That makes sounds with every step he does.
heard). The sound must move with the x- and y position of the enemy.
I`ve found out, yet, that can be solved by the emitter.
I`ve set in the creation code of the player idle a global emitter ("fxEmitter").
As you can see, I wrote a remark line above the emitter activation.
enemies position, if he comes or if he goes away.
The rusty sound is started 60 times per seconds, a rapidfire of that sound.
How can I tell gml, just restart playing the audio, after it is ready with playing that sound (1 Second)?
I hope I could explain myself as good as possible!?
Thankful for every hint of you.
You might also consider just triggering the sound on a certain frame of your animation using image_index.
Create an alarm when your Warrior is walking then in alarm event check if he is walking then play the sound.
// Play the sound 1/2 seconds.
Thank you guys, for giving me these hints!
@obscene: I often used image_index-triggering methods. That works fine - less is more.
But I decided to make it with the first suggestion you made. I think, it´s more elegant.
And I want to become an expert one day ;-) And I want to understand EVERYTHING!
here, whiches give my many examples for the implemention.
@Edwin: That works "extremely excellent" ;-) Thank you, for that alternative.
I could use it in another parts of my game coding.
Have a nice and successful day.
Another alternative is creating a ticking variable and using it with mod expression.


text:
Q: How to correctly configure typeRoots option? I've got a strangely shaped yarn monorepo. Here's how it looks:
monorepo root
├── frontend
│   ├── dashboard <-- not a yarn workspace
│   |   ├── src
│   |   ├── node_modules
│   |   ├── tsconfig.json
├── node_modules <-- hoisted by yarn
├── packages
│   ├── other typescript project <-- yarn workspace
│   |   ├── tsconfig.json
│   |   ├── node_modules

I've configured all tsconfig.json files to have this setting:
compilerOptions: {
  "typeRoots": [
     "./node_modules/@types/"
   ]
}

I've also got exclude configured:
"exclude": [
    "node_modules/**/*",
    "../../node_modules/**/*"
  ]

When I'm inside frontend/dashboard and I run tsc, I'm getting the following output:
node_modules/@types/react/index.d.ts:3088:14 - error TS2300: Duplicate identifier 'LibraryManagedAttributes'.

3088         type LibraryManagedAttributes<C, P> = C extends React.MemoExoticComponent<infer T> | React.LazyExoticComponent<infer T>
                  ~~~~~~~~~~~~~~~~~~~~~~~~

  ../../node_modules/@types/react/index.d.ts:3100:14
    3100         type LibraryManagedAttributes<C, P> = C extends React.MemoExoticComponent<infer T> | React.LazyExoticComponent<infer T>
                      ~~~~~~~~~~~~~~~~~~~~~~~~
    'LibraryManagedAttributes' was also declared here.

I don't understand why Typescript is climbing outside of the typeRoots directories?

redpajama_set_name: RedPajamaStackExchange


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It's also important to contact an attorney promptly after suffering an injury because time is not on your side. Whether it's an auto accident or a workers' compensation claim, there are deadlines you will be held to, and the courts are often quite strict about them. It's important to allow your lawyer to stay on top of any requirements you must keep.
At Carabin & Shaw, we understand what it's like to wonder what accidents are considered personal injuries. You want to be made whole again, and that is why you need an advocate protecting your rights. Many of those injured in accidents aren't sure who to call or what to do, and are left feeling overwhelmed by their circumstances. Our attorneys believe everyone should have the opportunity to have someone fighting for them.
We understand the physical and emotional trauma that accompany Rockport personal injury, and our attorneys have been hard at work for years giving a voice to our clients and earning their trust. Working with us is easy. Simply call our office, set up an appointment to meet with one of our lawyers in Rockport, and let us get to work for you. We'll thoroughly evaluate your case and are committed to making sure you receive the compensation you deserve.
Don't allow the stress of personal injury after an accident disrupt your life. Call one of our attorneys in Rockport. Your first consultation with us is free of charge and we won't collect any money from you until we are successful in winning your case. Call our law offices for your free consultation today at 361-790-7788 or toll-free at 800-862-1260.


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Home » Blog » Va'yakhail: (Exodus 35:1-38:21) Our Community, Our Self
Va'yakhail: (Exodus 35:1-38:21) Our Community, Our Self
The Western Wall, Jerusalem/Steve Lubetkin Photo. Used by permission.
The Mishkan is the focus of this portion. Moses calls together the Israelites, issues detailed instructions as to the creation of the Mishkan, and calls Bezalel and "every skilled person" to take the gifts from people and begin the work.
As you would expect, there are numerous commentaries on the portion and the meaning of the Mishkan. I just completed a very interesting series of teaching weekends at congregations across the USA. Literally from coast to coast; small under 300 members to mega-congregations of thousands. In each, in their own way, the community that people were a part of was a topic of much conversation and intense feeling. These were people who have chosen to give the "gift" (terumah) of their time and person to the building and maintaining of their community. Each of their hearts were moved to be there. It was not about theology, rather it was all about the relationships that they had forged and maintained. Rabbi Steven Carr Reuben, in his new book on Mordecai Kaplan, reminds us that "All of us, regardless of age, gender, status, are necessary for any community to survive and thrive" ("A Year With Mordecai Kaplan" Rabbi Steven Carr Reuben. JPS. 2019. p. 84)
The value of community and relationships was present at every stop. The age group of the attendees of our sessions were all over 50 years of age. Relationships, to us, are primary in our life. The synagogue, the religious community, remains the central institution for the transmission and continuance of community. In a Jewish world that is, to say the least, in flux and transition, the synagogue remains the key address for creating and maintaining sacred human relationships. And it is these human relationships that allow for the various pathways to our relationship with the Sacred. The detailed instructions for the building of the Mishkan can be seen, thus, as symbolic language for us today. What this portion may also be trying to teach us is that what we bring to our community does determine the type of community that we have. Each of us, in our own way, seeks community. As we have said many times, as we get older, community and relationships become ever more precious and important. To channel the portion, each of us is called upon to bring what we can bring, our own special gift, to make a community. This is our challenge.


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Pursuing Your Premises Liability Claim
Property owners have a duty to keep their premises safe. When spills go uncleaned and repairs unmade, or snow and ice is not removed, dangerous conditions pose a threat to the health and safety of the innocent. If you slipped and fell, tripped or were otherwise injured due to a dangerous property condition, you may be entitled to compensation.
At Jainchill & Beckert, LLC, in Plainville, we will help you get the compensation you need to treat your injuries, make up for lost wages and continue supporting your family after a slip-and-fall accident.
Were You Injured By A Dangerous Property Condition?
Icy sidewalks, uneven pavement, poor lighting, inadequate security, rickety stairs, poorly organized shelving and other dangerous conditions can cause serious injuries, including:
At Jainchill & Beckert, LLC, we make sure you are compensated for the full extent of your injuries.
Will you be able to return to work? Will you need repeated surgery or ongoing physical therapy? Will you suffer from pain for the rest of your life?
Once we know how you will be impacted in the long term, we will pursue damages that fully compensate you for your injuries.
Pursuing Your Right To Compensation Doesn't Have To Be Stressful
Many people who come to our office feel overwhelmed and intimidated. They've never been involved in a lawsuit before and don't know what to expect from the legal system.
At Jainchill & Beckert, LLC, we take away fear of the unknown. Our lawyers will sit down with you and explain your rights and legal options. We will explain the benefits and drawbacks of various legal paths and work with you to develop a strategy that is right for you.
Contact Our Firm To Get Started
Aaron Jainchill and Bill Beckert are skilled trial attorneys — they build strong, effective personal injury claims that get results. Make sure you get the compensation you deserve after a slip-and-fall accident. Contact our firm today at 860-351-3552 for a consultation.
Slip-And-Fall FAQs
© 2020 by Jainchill & Beckert, LLC. All rights reserved. Disclaimer | Site Map


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Category: "Seeking Help from Public"
MAN MISSING FROM CRETE RESIDENCE - SEEKING HELP FROM PUBLIC
Missing Person, Seeking Help from Public
The Will County Sheriff's Office is seeking help from the public in locating Raymond Martin, a Crete Township man, who was last seen on Saturday, May 22nd. Martin left the care of his family on foot around 7:30pm from his home that is near the E. Exchange and S. Klemme Road area. Martin suffers from dementia and requires medication.
Mr. Martin is described as a male/white, age 63, 5'11" in height, and about 155 lbs. He has brown hair, brown eyes, and light skin complexion. He has a tattoo on his left upper arm that reads: "Ray" and a religious cross tattoo on his left ring finger. Martin was last seen wearing a red flannel long-sleeved shirt, blue jeans, and black shoes. He has no cell phone, cash, or bank cards with him.
It is believed that Martin was observed hitchhiking on Exchange Road between Route 394 and just across the Indiana border. Martin is known to frequent the Matteson and south side of Chicago areas.
If you see Raymond Martin or have any information about his whereabouts, please contact 911 or Laraway Communications Center at 815-727-8575. You may also reach out to Will County Sheriff's Detective DeMato at 815-727-8574 ext: 4912 (cdemato@willcosheriff.org).
SHERIFF'S OFFICE SEEKING HELP TO IDENTIFY SUSPECT IN AGGRAVATED BATTERY OF NEW LENOX BUSINESS OWNER
General, Seeking Help from Public
The Will County Sheriff's Office is seeking assistance from the public regarding the identification of a suspect involved in an aggravated battery complaint. On June 12, 2020 at 5:30pm, Sheriff's deputies were dispatched to a battery complaint at Shades of Darkness Window Tinting, located at 13957 W. Illinois Highway in New Lenox Township. Upon arrival, deputies spoke with the owner, Wayne Deutsch of Orland Park.
Deutsch stated that an unknown male black subject with a large beard had beaten him. Deutsch stated that he had previously done work on the subject's vehicle. Deutsch stated that the subject came into the store asking for a refund on the window tint that the subject paid for. Deutsch and the subject had words, and the subject left the store. Moments later the male black subject returned and started a physical confrontation with Deutsch. The male black subject began beating Deutsch as he fell to the floor. The subject fled the scene in a dark colored Chrysler 300 with tinted windows.
Deutsch refused medical treatment on scene, and sheriff's detectives immediately began an investigation into the incident. Deutsch was unwilling to provide detectives with information pertaining to the identity of the suspect. Detectives were advised on June 14, that Deutsch had been in the hospital and suffered from multiple broken ribs with fluid in his lungs.
On June 17, Sheriff's detectives were advised that Wayne Deutsch had succumbed to his injuries and the Cook County Medical Examiner's Office would be performing an autopsy the following day.
As of this writing, the Will County Sheriff's Office has not received any official information pertaining to the manner and cause of death as it relates to Wayne Deutsch.
The case remains active and detectives are following all leads. The Sheriff's Investigation Unit is asking for help in identifying the suspect in this photo. If anyone has any information related to this incident, please contact Detective Sean Moran at 815-727-8574 at extension 4914.
TWO GAS STATION ARMED ROBBERIES IN FOUR DAYS - SEEKING HELP FROM PUBLIC
Over the past few months, several armed robberies have occurred at gas stations in Will County Sheriff's jurisdictions, as well as municipal Will County areas. The Sheriff's Office has been working diligently with other law enforcement agencies in attempting to identify and arrest the offenders.
This morning around 5:40am, Speedway Gas Station, located at 7218 Lincoln Highway in Frankfort Township, was robbed for the second time in four days; also on 12/20/2019 at 4:30am. In this morning's robbery, there were two offenders and on 12/20, there were three offenders. Initial reports indicate that the offenders are the same individuals in each of these robberies and similarities suggest they have been involved in recent robberies in other jurisdictions.
The individuals are identified as male blacks, mostly unidentifiable, wearing dark clothing, gloves, and ski masks, armed with handguns. In both incidents, the offenders enter the store, fully covered, and order the employees and a customer to the ground by gunpoint. Employees are ordered to the back room while the offenders load cartons of Newport cigarettes into large garbage bags and take any currency that is in the register. In some of the robberies, offenders have stolen customers' wallets.
The vehicles used in recent area robberies have been identified as a white Jeep Grand Cherokee or a white Kia Optima. Both vehicles have been observed on video surveillance with the registration plates covered by black garbage bags.
Will County Sheriff's detectives are asking the public for assistance in identifying these individuals. Crime tips can be given by calling the Sheriff's Investigations Division at 815-727-8574 or online at Crime Stoppers. Please visit: www.crimestoppersofwillcounty.org. You can remain anonymous. There is a cash reward for any tips that lead to the arrest and conviction of these individuals.
The Sheriff's Office is also asking the public to call 911 immediately if you observe a vehicle in the eastern sections of Will County with black garbage bags or any other obvious obstruction on a vehicles license plate.
*Photos attached (four total). -end-


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Bohinc je  priimek v Sloveniji, ki ga je po podatkih Statističnega urada Republike Slovenije na dan 1. januarja 2010 uporabljo 539 oseb in je med vsemi priimki po pogostosti uporabe uvrščen na 540. mesto.

Znani nosilci priimka
 Andrej Bohinc – več znanih ljudi
 Anton Bohinc (1931—2018), župnik, zadnji predsednik Duhovniškega društva (pred razpustitvijo)
 Jakob Bohinc (1831—1912), mariborski stolni župnik
 Janez Bohinc (*1942), športni delavec, športni strelec
 Jože Bohinc (1928—2022),
 Klemen Bohinc, biofizik, ddr., prof. ZF UL
 Lara Bohinc (*1972), oblikovalka nakita v Londonu
 Marina Bohinc, igralka
 Nika Bohinc (1979—2009, Filipini), novinarka, filmska kritičarka
 Pavle Bohinc (1911—1991), farmacevt, univ. profesor
 Renata Bohinc, manekenka
 Rado Bohinc (*1949), pravnik in politik, univ. profesor
 Rok Bohinc, improvizator, stand-up komik, igralec, scenarist in voditelj iz Kranja
 Špela Bohinc (*1995), plavalka

priimek Bohinec:
Jaromira Bohinec (1919—2017), pianstka, klavirska pedagoginja
Monika Bohinec (*1979), pevka mezzosopranistka
Valter Bohinec (1898—1984), geograf, speleolog, katrograf, bibliotekar

Glej tudi
priimke Boh, Bohinec, Bohinjec, Bohanec
priimka Blejc, Blejec
Bohinj

Zunanje povezave

Slovenski priimki


Funny Bunny is an extreme and super cool game about a cute little bunny. Help the bunny to jump over the platform.
Get hours of fun time in this classic jumping game with stunning graphics that attracts everyone. On your way collect carrot to get extra bonus points.
You have to collect all eggs coming in your way, each egg has different amount of score.
You have to beware of the black egg, although it has no harm but it will subtract your score.
Crazy, colorful and challenging unlimited game play is especially developed for those who loves bunny.


Sel Souris is a small island two hours off the coast of Gibraltar. You've never been there. Almost nobody has, except for the geniuses and leftovers and madmen who defined outsider culture in the twentieth century.
Souria is a collection of two stories of the island, of the interface there with something rich and strange, a thing that we can only see reflected in shadows, Sel Souris is a small island two hours off the coast of Gibraltar. You've never been there. Almost nobody has, except for the geniuses and leftovers and madmen who defined outsider culture in the twentieth century.
Souria is a collection of two stories of the island, of the interface there with something rich and strange, a thing that we can only see reflected in shadows, in hints, or reflected in the eyes of mad outsiders. In Sel Souris, the veil between what is real and what is imagined is so thin that it may not exist at all.
Press button "GET DOWNLOAD LINKS" and wait 15 seconds. This time is necessary for links search to download Souria in all e-book formats.


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Tory Benefits Freeze Will See Two Million Disabled People Lose £2 Billion
By Tony Winterburn • 06 December 2020 • 9:27
Tory Benefits Freeze Will See Two Million Disabled People Lose £2 Billion.
At least 2 million disabled people in the UK will lose out as current cuts of £660 could increase to £1000, meaning a planned £20-a-week rise will be given to other Universal Credit claimants instead.
Employment Secretary Therese Coffey said necessary computer system changes would take months and a future increase could not be ruled out. But Shadow Pensions Secretary Marsha de Cordova said: "It is time the Government ended this discrimination." The Tories won't say whether the £20 rise will extend beyond April or whether disabled people on ESA will ever get it.
Lucy Hamilton, of poverty action group the Joseph Rowntree Foundation, said: "Millions face fear over Christmas and even greater hardship next year. It's important that it's rectified now." The revelations come the day after it was reported tens of thousands of people will see their Universal Credit payments cut this Christmas. That's because a measure put in place to try and protect people who've recently started using the six-in-one benefit is set to run out. As the so-called 'grace period' ends, it could hit as many as 160,000 households.
The grace period exempts people from the benefit cap, the cap limits the total amount of money working-age people can claim regardless of what they qualify for on other measures- for example, it applies if you get Housing Benefit or Universal Credit, your benefits will be capped if you get more than the limit that applies for your circumstances.
The number of people affected by the cap has more than doubled since coronavirus hit Britain and unemployment went through the roof.
Thank you for taking the time to read this news article "Tory Benefits Freeze Will See Two Million Disabled People Lose £2 Billion". For more UK daily news, Spanish daily news and Global news stories, visit the Euro Weekly News home page.
Vladimir Rogov calls IAEA reports of explosions near the Zaporizhzhya NPP a provocation
Tony Winterburn
Share your story with us by emailing [email protected], by calling +34 951 38 61 61 or by messaging our Facebook page www.facebook.com/EuroWeeklyNews


Are you traveling to Nashville, TN for a concert, bachelorette party, or other festivities?
In preparation for the escape room conference in Nashville July 27-29, 2018, we took a trip down to Music City and explored its booming escape room scene.
You can play some great games in downtown Nashville. If you have (or can rent) a car, we also recommend you drive 30 minutes south to Franklin, TN and 40 minutes southeast to Murfreesboro, TN. These recommendations cover Nashville, Franklin, and Murfreesboro together, which collectively make one fine escape room market.
Here are our escape room recommendations near Nashville, TN to help you choose the games you'll enjoy most.


Hirofumi Hotta of JPRS Received the ICANN 2017 Multistakeholder Ethos Award / Japan Registry Services Co., Ltd.
Japan Registry Services Co., Ltd. (JPRS: Chiyoda-ku, Tokyo; President Koki Higashida) today announced that Hirofumi Hotta, Director of JPRS, was awarded the 2017 Multistakeholder Ethos Award by ICANN on June 26, 2017.
The Multistakeholder Ethos Award honors members of the ICANN community who have served in essential roles in multiple ICANN working groups or committees and, for many years, made outstanding contributions to ICANN's multistakeholder model of Internet governance. ICANN recognized Hotta's contributions in ICANN community, presented the 2017 Multistakeholder Ethos Award at ICANN59 in Johannesburg, South Africa.
In the Award Ceremony, Hotta was introduced to the audience that he was well-qualified as a recipient who had played a pivotal role in ICANN community, demonstrated the spirit of collaboration for promoting consensus, proven his commitment to ICANN's multistakeholder model through 18 years of active participation and dedication.
In his acceptance speech, Hotta expressed his sincere appreciation to all the people who have led him, who have worked with him, and who have supported him, including all the community members.
JPRS will continue to support and be engaged in the multistakeholder ICANN process and contribute to the sound development of the Internet in the future.


NASA calls the simulation a breakthrough in the observation of black holes and in the understanding of the universe.
When two black holes collide, space shivers like Jell-O. With the help of a supercomputer to simulate this event, NASA seeks to prove Albert Einstein's theories and unveil the universe's secrets.
The NASA supercomputer Columbia just performed its largest astrophysical calculation ever: a 3D simulation of two black holes merging (click here to view video).
"This merger is a cataclysmic event, second only to the Big Bang in the amount of energy it produces," Joan Centrella, chief of the NASA Gravitational Astrophysics Laboratory in Greenbelt, Md., said Tuesday in a press teleconference.
NASA called the successful simulation a breakthrough in the observation of black holes and in the understanding of the entire universe. In fact, NASA claims that it might even provide the ultimate proof for Einstein's theory of general relativity.
Black holes occur when large stars burn up all their energy and collapse into bodies of enormous density. Their gravity is so strong that it absorbs everything around them--even light.
When two of these bodies collide, they emit more energy than the light of all the stars in the universe combined. Space shivers like a bowl of Jell-O around them, when gravitational waves spread at light speed. It is the pattern of these waves that NASA has now managed to simulate.
"Gravitational waves are going to give us an entirely new window on the universe," said Peter Saulson, a physics professor at Syracuse University involved in the project. He compared the results with the discovery of radio waves, infrared light and x-rays.
"Each time astronomers were able to open a new window, the universe showed a new face," he said. "Now that we are about to open up the gravitational wave window, we should again see a whole new different view of the universe."
Einstein explored the forces of gravity in his general relativity theory, predicting phenomena like black holes and gravitational radiation long before they could be proved. It is not until now, more than 90 years later, that scientists have managed to test these, back then inconceivable, predictions, Centrella said. "This has been a holy grail quest for the last 30 years."
Earlier trials failed since the equations based on Einstein's general relativity theory were so complicated that they made supercomputers crash; the enormous gravity of black holes cause disturbances in time and space, making time stop and space shrink and expand.
NASA researchers have managed to transform the theory into mathematical algorithms and run through it through Columbia, the . Its 2,032 interconnected 512 Intel Itanium 2 processors ran for 80 hours, in an operation that would have taken 18 years for a single processor to perform.
The result was a model of the gravitational wave pattern of the black hole collision, which turned out to be the same regardless of the bodies' starting positions. Knowing the pattern, scientists can look for and interpret it in space, Centrella said.
"This is not something made up, like in a science-fiction movie," Centrella said. "We have confidence that these results are the real deal, that we have the true gravitational fingerprint predicted by Einstein for the black hole merger."
In fact, scientists are already out there looking. The National Science Foundation's Laser Interferometer Gravitational Wave Observatory (LIGO) in Hanford, Wash., is scanning space for the waves. Now they know what to look for, said Paul Hertz, chief scientist at NASA headquarters in Washington, D.C.
"Today we're throwing down the gauntlet for Einstein's theory of general relativity," Hertz said. "When LIGO detects gravitational waves from merging black holes, we will know whether Einstein's theory is right, or whether Einstein's theory is wrong."


Author Media Kits: What the heck do I need?
In past posts we've discussed author websites, how to cultivate your author PERSONA via your website, and what your site needs to contain. In this post, we'll take a moment to do a deep dive into the contents of your author media kit.
So...What the heck do I need to include in my media kit?
Where should you put this information on my website? You can make a new tab named 'Media Kit' or include this information on a combination 'Events & Media' page. Or you can include your media kit as part of your 'About Me' or 'Contact' page.
Consider adding a media kit to your website.
You will make a lasting impression and be perceived as an organized professional.


These are the required Confirmation Specific Classes for those who are beginning their 3rd year of classes. These classes will be your final preparation for your Sacrament of Confirmation. Please email Annemarie if you have not registered.


2Department of Parasitology, College of Medicine, Hallym University, Chuncheon, Korea.
3Institute of Medical Education, Hallym University, Chuncheon, Korea.
PURPOSE: In order to apply the item response theory to test results, the assumptions made about unidimensionality and item goodness-of-fitness should be tested before analysis. To know if the Korean Medical Licensing Examination results fulfill these assumptions, appropriate tests were done on these two features. METHODS: Three results(from three subjects) of the Korean Medical Licensing Examination, done in January 2004, were converted into 1, 0 data. The Holland and Rosenbaum Method(HRMH) and DETECT were used to test unidimensionality. The Winsteps was used to test goodness-of-fitness according to the Rasch model. RESULTS: Unidimensionality was rejected by HRMH but accepted by DETECT. With the Rasch model, 2 out of 550 items were inadequate. Each 137, 73 and 455 examinees out of 3,881 were inadequate in three subjects of 126, 400 and 24 items. CONCLUSION: The above results suggest that DETECT is desirable for testing unidimensionality of high-stakes tests with more than 100 items. According to the Rasch model, the Korean Medical Licensing Examination fulfills the goodness-of-fitness to be analyzed according to the item response theory.


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Q: how to write a file object on server response and without saving file on server? I am using Spring with DWR . I want to return a file object as response , however I save the file (to be sent) at server temporary location and then send its location as href for anchor tag on client side , however I wonder if there could be a way to throw the file directly to browser on response object without saving it temporarily on server.
I expected if there could be a way to send file as a response via DWR.

A:
public ModelAndView writeFileContentInResponse(HttpServletRequest request, HttpServletResponse response) throws IOException {

        FileInputStream inputStream = new FileInputStream("FileInputStreamDemo.java");  //read the file

        response.setHeader("Content-Disposition","attachment; filename=test.txt");
        try {
            int c;
            while ((c = inputStream.read()) != -1) {
            response.getWriter().write(c);
            }
        } finally {
            if (inputStream != null)
                inputStream.close();
                response.getWriter().close();
        }

        }

A: It has been years since I've used Spring, and I'm unfamiliar with DWR, but the essence of your question is basic to the web.
The answer is yes, you can.  In effect, you need to set the HTTP header Content-Disposition: attachment, then stream down the contents.  All of this will be in the response to the original request (as opposed to sending back a link).
The actual code to achieve this will depend on your circumstances, but this should get you started.

A: you call the method from Java Script, right? I didn't really understand how Spring is related in this flow, but as far as I know DWR allows you to produce Java Script Stubs and call the Java methods of the exposed bean directly on server right from your java script client code.
You can read the file byte-by-byte and return it from your java method as long as it really returns a byte array.
However what would you do with this byte array on client?
I just think in this specific flow you shouldn't use the DWR but rather issue an ordinar AJAX request (if DWR can wrap it somehow for convenience - great). This request shouldn't come to DWRServlet, but rather be proceeded by a regular servlet/some web-based framework, like Spring MVC :)
Once the request comes to the servlet, use
response.setHeader("Content-Disposition","attachment; filename=test.txt");
as was already stated.
Hope this helps,
Good luck!
Mark

A: An example which return a excel to download from client:
//Java side:
public FileTransfer getExcel(Parametros param){
   byte[] result = <here get data>;
   InputStream myInputStream = new ByteArrayInputStream(result);
   String excelFormat = "application/vnd.openxmlformats-officedocument.spreadsheetml.sheet";
   FileTransfer dwrExcelFile = new FileTransfer("excel.xlsx", excelFormat, myInputStream);
   return dwrExcelFile;
}

//Javascript side:
function downloadExcelFile() {
  dwr.engine.setTimeout(59000);
  var params = <params_to_send>;
  <Java_class>.getExcel(params, {callback:function(dataFromServer) {
    downloadExcelCallback(dataFromServer);
  }});
}

function downloadExcelCallback(data) {
   dwr.engine.openInDownload(data);
}


I wrote the treatment and developed the story of this TV-Event-Movie in cooperation with Daniel Mann and Marco Gilles (www.gilles-mann.de).
Go to the IMDB-site of this film and get more info.
LOGLINE: Based on well-known motives of Theodor Storms novella, THE RIDER ON THE WHITE HORSE traces the story of dykemaster Hauke Haiens life.
We are in the 18th century, on the rough North German coast where Hauke Haien plans to build an indestructible dyke to protect his family and to lead them all into a better future. Obsessed by this ambition, his fate irrevocably connected with the dyke, Hauke Haien defies the laws of nature.
INFO: I wrote the adaption-script of the novella by Theodor Storm (a famous german author of the 19th century).
I received grants awarded for development of the script and project by Filmstiftung NRW and the FAA.
Please have a look at the first few pages of the script and feel the magic (PDF-DOWNLOAD (english)) ( PDF-Download (deutsch)).
At my work-site you'll find the Moodboard-Clips of this project (category "film-shorts").
The german word "Grind" means the scab on a wound, consisting of coagulated blood, wound secretion and tissue fluid.
LOGLINE: Thirty-three-year-old marine biologist Anja Haake gets back to her birthplace, the island Grindland, after 25 years. She wants to examine the stranding of four humpback whales. In the course of her work, she gets on to a terrible secret.
INFO: I wrote the script for this thriller (TV or cinema), the project is developing. The script was funded by the Filmstiftung NRW.
Here you can read the first pages of the script and get closer to the secret (PDF Download (deutsch)).
LOGLINE: A child faces death and fights against evil ghosts in the german 17th century.
With the help of the mysterious Ghostman an old ghost hunter and a troop of good ghosts the young boy tries to fight against evil.
Have a look at the first moodboard by Gunter Grossholz, a german storyboard artist and painter (PDF Download).
LOGLINE: An epic story from 1930 to 2015 in Europe. It's a story about war and its eeriness.
A story about a WWII-childhood and the daemons coming long after the end of the WWII.
The WWII is present in the modern Europe.
LOGLINE : This script, written with my Co-Author Axel Melzener, is based on my short BIOPOLIS.
Have a look at the amazing moods by Gunter Grossholz, a german storyboardartist and painter (PDF Download).


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