The eight vitamins that make up the B complex are very important to the diet, supporting many important physical and mental processes. For anyone interested in feeling their best every day, a sufficient daily intake of this essential set of vitamins is an absolute necessity.
The Vitamin B complex is made up of several separate vitamins. These are B1, also called thiamine, B2, also known as riboflavin, B3, which is also referred to as niacin, B6, also called pyridoxine, B9, commonly called folic acid, B12, also known as cyanocobalamin, biotin and pantothenic acid.
These vitamins are essential to helping the body to convert food to energy, as well as to breaking down the fats and proteins that make the nervous system run efficiently. They support oral health, muscle tone, and help to keep the skin, hair and eyes healthy. The Vitamin B complex also helps to maintain mental functioning, including thinking and short-term memory.
Because of the many important tasks performed in the body by the Vitamin B complex, deficiencies can result in serious health problems and disease, affecting mind and body. Perhaps of these, beriberi is the most well known. This can come from a consistent and serious lack of thiamine in the diet. Symptoms include anemia and muscular weakness and spasms, particularly in the legs. Atrophy of the muscles and even paralysis can occur.
There are many physical problems that result from a failure to consume sufficient amounts of the Vitamin B complex.
The negative effects can include a lack physical coordination, the eyes can become light sensitive, open sores can appear on the internal and external parts of the mouth, the teeth can become sensitive, the tongue can become swollen, severe and continuous diarrhea can occur, and the skin can develop lesions. Serious failures in the nervous system and brain damage can also stem from a lack of these vitamins.
In addition the myriad of physical symptoms associated with ongoing and serious deficiencies in the Vitamin B complex, there are also significant mental symptoms as well. These include dementia, confusion and other mental disabilities.
In many cases, even serious symptoms caused by a lack of B vitamins can be alleviated with Vitamin B complex based treatments. However, some types of damage can be permanent. It is far better to avoid such debilitating symptoms by making sure to consume sufficient daily amounts of the very important Vitamin B complex.
Vegetarians, especially those following vegan diets, need to be particularly aware of their Vitamin B complex intake, as many of the richest sources are animal based. If vegetarian, it is important to be knowledgeable about the nutritional content of the food you consume, particularly for families raising vegetarian children. Many find Vitamin B complex supplements to be a safe and sure means of making sure that the daily intake of these essential nutrients are met.
Because they are so essential to many important aspects of physical health and mental functioning, we should all take care to meet the daily intake requirements of each of the vitamins that make up the B complex. Supplements offer a safe and sure method of doing so for many people.


text:
Q: Adding custom classes / methods I have created a task in Symfony 1.4 that loads in some CSV files into a table - very simple ->
protected function execute($arguments = array(), $options = array())
{
    $databaseManager = new sfDatabaseManager($this->configuration);
    $connection = $databaseManager->getDatabase($options['connection'])->getConnection();

    ......

    $query = "LOAD DATA INFILE '" . $cdrfile . "'
       INTO TABLE ....

    etc

    $connection->execute($query);
}

But i want to reuse this section of code else where - So i create a new PHP Class and created a new static method called loadDataFromCSV.
I put all of the code into that method and then called class::loadDataFromCSV ...
This gave me some problems - first the $this keyword in the method is not valid as the class it not an object (ie not instantiated) - so I could instantiate the class and then call the method class->loadDataFromCSV - the next problem is the $this->configuration on the first line - do I have to pass in the configuration to the method to get it working ?
Whats the simplest way to create a simple method to run a simple piece of code - without having to pass lots of variables around.

A: Short answer: Use DI Container.
Long answer: You basically ask how to set object dependencies as your class depends on configuration object. There are two ways to do this. Hardcode dependency in your class. e.g. Registry::getInstance()->get('config'); and to use dependency injection. Dependency injection is better solution as far as you can pass any config instance. Existing Object, new object, mock object for unit testing, or other config implementation. There are two types of dependency injection. inject dependency via constructor (e.g. new Object(new Dependency())) or via setter.
$o = new Object();
$o->setDependency($dependency);

If your object has many dependencies the code may become little unreadable in both ways. The solution is to use Dependency Injection Container which inject automatically all the dependencies for you. Your client code is still one simple line: DIContainer::create('object');. Create method creates an instance of class, inject all the dependencies and returns the object.

A: For using your approach with static method you should:

*

*Replace all this-> keywords on self::

*Move all config settings in one file and load them in for example Config class which will implement pattern Singleton.

*Call will look like Config::getInstance()->getSection('your_section');

Regarding DB initialization:

*

*Create Registry class with 2 static methods set/get

*Create a DB object in bootstrap file.

*Use $connection = Registry::get('db')->getConnection();

redpajama_set_name: RedPajamaStackExchange


Ruckus has a very simple way to collect most-needed troubleshooting information from an AP. Log into the AP, then see the screenshot below.
This information should be collected and provided any time you need troubleshooting assistance.


text:
Road test: 2011 Ford Fiesta
A returnee to the Canadian small car battlefield, the Ford Fiesta was forced to retreat to Europe for a number of years but is back with a vengeance. It plunges back into our market wielding a base price of just $12,999 and sleek ultra-modern new styling lines that are the envy of its competitors. The main reason behind this new small car offensive by Ford is that this market segment is expected to see sizable sales growth in the coming years.
drivingwheel2013
Aug 11, 2010 • October 13, 2013 • 5 minute read
2011 Ford Fiesta.
A returnee to the Canadian small car battlefield, the Ford Fiesta was forced to retreat to Europe for a number of years but is back with a vengeance.
It plunges back into our market wielding a base price of just $12,999 and sleek ultra-modern new styling lines that are the envy of its competitors.
Road test: 2011 Ford Fiesta Back to video
The main reason behind this new small car offensive by Ford is that this market segment is expected to see sizable sales growth in the coming years. More than just a car launch, if all goes to plan, Fiesta will re-establish Ford in the small car market and phase two will see this platform spawn a whole range of other new small Ford vehicles.
Boasting best-in-class highway fuel economy, Fiesta also claims to set new benchmarks in small car safety and electronic media connectivity. Our North American edition of Fiesta is made in Mexico and in addition to the five-door hatchback body style, sold in Europe, it's also sold here as a four-door sedan.
The Fiesta sedan comes in S, SE and SEL trim levels. That Canadian base price of $12,999 for the S trim level sedan is actually $2,000 below the US base price — now there's a refreshing change! What's more, other than the absence of air conditioning they are identical.
The five-door hatchback body style doesn't come in an 'S' trim and its price starts at $16,799 for an SE trim, which is $700 more than the SE sedan. The top-line SES (hatchback) and SEL (sedan) series offer optional leather upholstery ($1,200) with contrasting colour piping. There's also another ($500) upgrade package that includes push button start is also available.
Power comes from a Ti-VCT 1.6-litre 4-cylinder engine with twin variable camshaft timing that can provide up to 120 horsepower and peak torque is 112 ft-lb at 5000 rpm. Fuel consumption with the automatic is 6.9 L/100 km in the city and 5.1 L/100 km on the highway (which is about 56 mpg).
My bright green (called Lime Squeeze) test Fiesta came with the 5-speed manual transmission but another nice surprise for buyers will be the performance of the optional PowerShift six-speed automatic transmission. Basically, it's two manual transmissions in one that shift electronically, similar to Audi's superb high-tech DSG transmission.
Called "Kinetic" design language, introduced with the Iosis concept vehicle, the Fiesta brings a fresh and compelling aesthetic that's been lacking in our small car market. A sweeping design with oversized multi-element headlights and big wheel arches give it an athletic shape.
The hatchback Fiesta retains the Euro grille opening, while the sedan has Ford's signature three-bar look. A standard rear spoiler sits on the top of the hatchback's rear liftgate. On the sedan, a spoiler is optional and it fits on the trailing edge of the trunk lid.
THE INSIDE
A cell phone (think Razor) was the inspiration for the design of the centre dash switch assembly, which houses audio and HVAC controls. The idea being that it would be a
familiar interface that would appeal to a younger buyer (who probably now owns an iPhone).
My test Fiesta SES came with the optional Push Button Start and the Ford SYNC hands-free communications and entertainment system. It's a voice-activated system that can connect to your cellphone and offers services like 911 Assist, Vehicle Health Report and turn-by-turn navigational assistance.
Included in the SES and SEL trim levels are steering wheel-mounted audio controls and a four-inch multi-function screen that gives information. The ambient lighting system allows drivers to choose between seven interior accent lighting colours.
Second-row seating features a 60/40-split folding seat with adjustable head restraints, but leg room is quite limited and the large outboard head restraints restrict the driver's rear vision. Cargo space is not managed as cleverly in the Honda Fit, which has the multi-folding seat system. While there's a decent amount of cargo space with the rear seatbacks up, they simply flop forward on top of the seat cushion and you'll probably have to remove and then store the head restraints.
Fiesta comes with seven standard airbags, which includes an extra driver's knee airbag.
It's also one more airbag than you can get, even as an option, in a Fit, Yaris or Versa. The knee airbag helps prevent leg injuries and better positions the driver to survive a serious frontal impact.
More than 50 per cent of the welded body structure of Fiesta is made from high-strength steel and Boron steel (which has four times the strength of regular steel) is used in critical areas, such as roof pillars and side intrusion beams. Fiesta is also constructed to meet European pedestrian (impact) safety requirements.
The Sync system is also an indirect safety feature in that it allows drivers hands-free operation of a cellphone, car stereo and other technology without taking their eyes off the road or hands off the wheel.
Electronic stability control and anti-lock brakes are standard on all trim levels.
THE DRIVE
In addition to outstanding highway fuel economy the Fiesta rides surprisingly well on the highway, for a small car. Some extra reserve power would be nice at highway speeds, but it certainly has no problem getting to high cruising speeds. Fiesta is quick off its mark from a standing start and its mid-range power is also impressive.
Its electric-assist steering has a nice light feel at low vehicle speeds and gets progressively firmer as speed increases; it's a more natural feel than earlier electric-assist systems. Called EPAS (Electric Power Assist Steering), it has 'pull-drift compensation' to help the car track straighter in side wind conditions and another feature called 'active nibble control,' which dampens the transfer of for minor wheel/road vibrations to the steering wheel.
A tilt and telescopic steering wheel is standard on all versions of Fiesta. It certainly makes it a much easier task to find a comfortable driving position. And time spent behind the wheel is when owners will really appreciate the best attributes of Fiesta.
Its nimble handling characteristics are a terrific bonus and at the top of its class.
When you eventually do have to pull into a gas station in a Fiesta, you'll discover another pleasant surprise, a self-sealing fuel filler system that eliminates the need for a gas cap.
Cool looking and competitively priced, the new Ford Fiesta is a well engineered little car that's a hoot to drive and a fuel-miser supreme.
Trim levels: S, SE, SEL & SES
Sticker Price: $12,999 to $18,899
Power: 1.6-litre, 4-cylinder, 120-hp
Transmission: 5-sp man/6-sp auto
Fuel consumption (man): 7.1/5.3 L/100 km (city/highway)
Basic Warranty: 3 yrs / 60,000 km
Powertrain Warranty: 5 yrs / 100,000 km
Rust Warranty: 5 yrs / unlimited km
Chevrolet Aveo: $13,950 -$16,850
Hyundai Accent: $13,588 -$18,999
Honda Fit: $14,480 -$18,780
Kia Rio: $13,695 -$15,795
Nissan Versa: $12,698 -$20,598
Suzuki Swift: $14,715 -$17,055
Toyota Yaris: $13,905 -$20,555
Share this Story: Road test: 2011 Ford Fiesta

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: Помогите, пожалуйста, написать кнопку удаления элементов списка и документа word Суть проблемы:
У меня есть список в классе ButtonEventManager, в котором хранятся данные с текстовых полей.
Программа работает по принципу вывода этих данных в word.docx при нажатии кнопки send.
Мне нужно написать кнопку удаления элемента из списка и из документа.
Но я не могу обратиться к списку из других методов.
Подскажите решение проблемы
Main
public class Main {
    public static void main(String[] args) throws IOException {
        contactForm form = new contactForm();
        form.setVisible(true);
        File wrdd = new File("Anketa.docx");
    }
}

Форма
public class contactForm extends JFrame {

    JTextField name_field, number_field;

    public contactForm() {

        super("Анкета");
        super.setBounds(250, 250, 600, 200);
        super.setDefaultCloseOperation(EXIT_ON_CLOSE);

        Container container = super.getContentPane();
        container.setLayout(new GridLayout(5, 2, 2, 10));

        JLabel name = new JLabel("ФИО");
        name_field = new JTextField("");
        JLabel number = new JLabel("Номер телефона: ");
        number_field = new JTextField("+");

        container.add(name);
        container.add(name_field);
        container.add(number);
        container.add(number_field);

        JButton send = new JButton("Добавить контакт");
        JButton remove = new JButton("Удалить контакт");

        container.add(send);
        container.add(remove);

        send.addActionListener(new ButtonEventManager());
        remove.addActionListener(new ButtonEventManager());
    }

    class ButtonEventManager implements ActionListener {

        @Override
        public void actionPerformed(ActionEvent e) {
            String[] nmbArray = {};
            ArrayList<String> numberandnames = new ArrayList<>((Arrays.asList(nmbArray)));
            numberandnames.add(name_field.getText());
            numberandnames.add(number_field.getText());

            try {
                File file = new File("C:\\Users\\Admin\\Desktop\\Anketa.docx");
                file.createNewFile();
                Path link = Paths.get("C:\\Users\\Admin\\Desktop\\Anketa.docx");
                if (Files.exists(link)) {
                    FileInputStream fis = new FileInputStream(file.getAbsolutePath());
                    XWPFDocument docxModel = new XWPFDocument(fis);
                    docxModel.createParagraph();
                    String documentLine = docxModel.getDocument().toString();
                    CTSectPr ctSectPr = docxModel.getDocument().getBody().addNewSectPr();
                    XWPFParagraph bodyParagraph = docxModel.createParagraph();
                    bodyParagraph.setAlignment(ParagraphAlignment.LEFT);
                    XWPFRun paragraphConfig = bodyParagraph.createRun();
                    XWPFParagraph paragraph = docxModel.createParagraph();
                    paragraphConfig.setItalic(true);
                    paragraphConfig.setFontSize(20);
                    paragraphConfig.setColor("170101");
                    paragraphConfig.setFontSize(12);
                    List<XWPFParagraph> paragraphs = docxModel.getParagraphs();
                    for (XWPFParagraph para : paragraphs) {
                        paragraphConfig.setText(numberandnames.toString());
                        break;
                    }
                    fis.close();
                    try{
                        FileOutputStream outputStream = new FileOutputStream("C:\\Users\\Admin\\Desktop\\Anketa.docx");
                        docxModel.write(outputStream);
                        outputStream.close();
                    } catch (Exception ex) {
                        throw new RuntimeException(ex);
                    }
                }
            } catch (IOException ex) {
                throw new RuntimeException(ex);
            }
            contactForm.Word wrd = new contactForm.Word();
            wrd.setVisible(true);
        }
    }

    static class Word extends JFrame {
        public Word() {
            super("Анкета");
            // Выход из программы при закрытии
            setDefaultCloseOperation(EXIT_ON_CLOSE);
            // Кнопки для создания диалоговых окон
            JButton docx = new JButton(".docx");
            docx.addActionListener(new ActionListener() {
                public void actionPerformed(ActionEvent e) {
                    Desktop desktop = null;
                    if (Desktop.isDesktopSupported()) {
                        desktop = Desktop.getDesktop();
                        try {
                            desktop.open(new File("C:\\Users\\Admin\\Desktop\\Anketa.docx"));
                        } catch (IOException ioe) {
                            ioe.printStackTrace();
                        }
                    }
                    dispose();

                }

            });

            // Создание панели содержимого с размещением кнопок
            JPanel contents = new JPanel();
            contents.add(docx);
            setContentPane(contents);
            // Определение размера и открытие окна
            setSize(350, 100);
        }

        private JDialog createDialog(String title, boolean modal) {
            final JDialog dialog = new JDialog(this, title, modal);
            dialog.setDefaultCloseOperation(EXIT_ON_CLOSE);
            dialog.setSize(180, 90);
            return dialog;
        }
    }
}


This authentic GLOV makeup remover wipe is pure magic; it allows you to quickly remove your makeup using nothing but water. Ingenious fiber technology allows the soft microfibers of this cloth to gently remove all makeup, even waterproof mascara, when dampened with water. No makeup remover is required when using this hypoallergenic wipe, meaning you won't expose your skin to harsh chemicals and alcohol that can cause dryness and irritation. With everyday use, you can reuse the GLOV Original On-The-Go washcloth for up to 3 months.


question about the times listed on the my points page.
Whenever you complete a survey or get 5 points for getting disqualified it lists the survey number and time on the my points page. I've noticed that the time listed on the my points page is based on the eastern time zone in the US even though I don't live in the eastern time zone. Although it really doesn't matter I'm just wondering if it is this way for everyone?
Yes,I think that the time is set to the location of Univox and yes,everytime it shows the time when I started the survey. Btw,for me is 2 hour difference.
that would mean it goes by Central time for her.
I went by info for location given on Survey Police, as I could not find it readily here on Univox.
Seen another site that said VA, but it looked like it hadn't been updated in years so I'll trust survey police that it is SC.
Ok so it is the same for everyone.
Good to know because in the past sometimes when I had a issue with a survey univox would ask what time I attempted the survey at.
The time and date was always shown there (my points).
Never really noticed, but I'm on the east coast so it probably wouldn't stand out.
I agree it doesn't matter I was just wondering if it was that way for everyone or just for my time zone.
Most boards will give the time zone from where the board comes from. I'm in AZ so get use to seeing eastern or pacific time. Some board will actually list your time zone but not many.
Answer the below question & win 20 points !!
How many points does a premium user need in order to redeem? answer & win 20 points !!
What's new on 'My Account' page and win 20 points for the correct answer.


Polident denture cleaner is proven to kill 99.9% of odor causing bacteria and more of the other micro-organisms than regular toothpaste. It can also effectively remove plaque and tough stains to prevent buildup. The product is available in four different favors and available at most drug stores. Visit mypolicare.com for info on Polident. During your visit at our office, we will clean and disinfect your dentures as a service for you!!


Buyse M. Clinical trial methodology. Invited lecture at the International Collaboration for Research Development in Oncology (CReDO) Workshop.
The objective of this workshop is to train researchers in oncology in various aspects of clinical trial design and to help them to develop a research idea into a structured protocol. Participation is open to researchers with training in surgical, medical or radiation oncology or any branch related to oncology.


Digital Desktop Clock - is an amazing time widget for windows. Bring more attraction and productivity to your desktop!
Digital Desktop Clock 1.0 Desktop Tools software developed by FlashTECH. The license of this desktop tools software is shareware$, the price is 4.99, you can free download and get a free trial before you buy a registration or license. Do not use illegal warez version, crack, serial numbers, registration codes, pirate key for this desktop tools software Digital Desktop Clock. If you want to get a full and unlimited version of Digital Desktop Clock, you should buy from original publisher FlashTECH.
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SL Digital Alarm Clock FREE DOWNLOAD Description: Minimize this great Digital Alarm Clock on your Desktop. Multiple Font and Background Settings. Stores your previous Alarm Settings.
Digital Table Clock for Windows 8 is a handy and reliable application designed to show the current date and time from a modern interface. The title panel can be hidden, which launches the application in full screen, so you can see the time in the dark on your portable tablet.


IST is committed to making your transition to campus as smooth as possible.
Announcement - Rutgers-UMDNJ Integration: UMDNJ will be transferred to Rutgers, effective July 1, 2013. As a result of this integration, you will see changes to this website. To learn more about how IT services are changing related to the integration, visit the OIT Rutgers-UMDNJ Integration site.
To provide EMERGENCY off hours assistance in the evaluation and resolution of an information technology issue.
A situation where either Patient Care or the Public Safety of the University is in jeopardy, or a major system outage affecting an entire floor, building or campus.
Monday thru Friday 5 p.m. to 7:30 a.m.
Please call the IST Service Center at 732-743-3200 and select the option to report an emergent issue impacting an entire department, building, or campus.


Carolina Value Pet care has a dynamic team inspired by our mission to provide affordable preventative care for pet owners.
Our team members must have the skill set to work well as a team player. We have a fast paced and high- energy work environment that requires our team to be adaptable and flexible for our clients and their furry family members. Team members must have compassion for people and pets, great communication skills, and the drive to learn and serve. We have high standards for a positive work environment and try to have fun on the job. Dr. Bob and Catherine are not just employers but are also inspirational leaders. Our team members come from a variety of backgrounds and have varied skill sets that they bring to Carolina Value Pet Care. If you have the qualities and the passion to be part of our team, please send us your resume or fill out the application. We are happy to keep your information on file. Please indicate the position(s) you are interested in applying for. NOTE: There will be a trial/shadowing period at one to two clinics.
Discusses options and services with clients. Fills in client forms with services requested. Must be willing to learn about products and be able to advise and inform clients. As an Intake Rep, you will learn to look at pet records and mark the forms appropriately.
Assist the client and doctor by lifting and lowering pets, restraining for vaccines, cleaning the exam table between clients, and other miscellaneous though very important duties. Must be able to lift 50 lbs and stand for long periods of time.
Fills out paperwork for recording visit, totals invoices, dispenses and documents medication sold. Must be customer oriented, patient and calm, able to focus under pressure.
Our Greeter is the first person from our team the client encounters. Must be Friendly and welcoming to all our clients and their pets. Greeters will hand out clipboards and forms to clients prior to seeing the DVM or RVT.
Carolina Value Pet care has a dynamic team inspired by our mission to provide affordable preventative care for pet owners. Thank you for your interest!


343 Industries currently unsure if Halo: Reach's "flight" will be on Xbox One or PC first.
343 Industries community director Brian Jarrard has some good news for Halo fans waiting for Halo: The Master Chief Collection on PC. "Flights", or beta tests as they're referred to, could begin later this month. Jarrard further confirmed that this is indeed "no joke".
The first flight for Halo: Reach could also begin this month, but Jarrard is still unsure whether the beta test will begin first for Xbox One or PC. Halo: The Master Chief Collection consists of four titles currently, with each releasing as betas for PC. Halo: Reach will be the first, and all titles should be on PC before the year ends.
Halo: Combat Evolved, Halo 2, Halo 3, and Halo 4 will also receive their respective flights. This will ensure that each is properly tested for issues before becoming publicly available. Each title can be purchased standalone on PC, but if you registered with Halo Insider, you could gain access to the flights at no cost. Stay tuned for more information on Halo: The Master Chief Collection, which will be available for both Windows 7 and Windows 10 users, through the Microsoft Store and Steam.


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Despite controversy surrounding the Oscar nominations the final local ratings for the awards telecast on ABC appear to be a wash.
The final local rating for the show on WISN-TV (Channel 12) is expected to be 24.7.
That was slightly better than last year's rating of 24.3, but 1.4 points lower than the originally reported preliminary overnight rating.
It is higher the national overnight rating of 23.1.
A local rating point is the equivalent of 8,822 television homes.
According to Deadline Hollywood the national figure represents an 8-year low, down 6% from last year's telecast which was the third worst since 2005 when Chris Rock last hosted the show.
Former Milwaukee Brewer John Axford – now with the Oakland Athletics – predicts a big night for Leonardo DiCaprio and "The Revenant" picking both to pick up Oscars in ceremonies Sunday night on ABC.
He picks that film's director Alejandro Gonzalez Inarritu to win the Oscar as well.
Axford started out making his picks on Twitter and then last year with the Players Tribune, an online magazine for and by athletes.
This year he made them as part of a team for ABC News.
It is a fish out of water tale about a New York lawyer defending a poetry professor played by John Lithgow accused of murdering his wife in a small Southern town.
By my count there are seven (7) Wisconsin connections in this Sunday's Oscar awards ceremony.
Six are film related and one of them is corporate. To recap.
Kenosha native and University of Wisconsin – Milwaukee film department Caroline Kastelic oversaw puppet fabrication for the film by Charlie Kaufman and Duke Johnson.
Below find the radio ratings for the Milwaukee market during January.
WRIT-FM lost 5.7 share points from the so-called holiday book during which it played all Christmas music. But it still held a comfortable 2.1 point lead over second place WTMJ-AM.
Third ranked conservative talker WISN-AM seemed to benefit from the noisy Republican presidential contest, climbing 1.2 points.
Ratings dropped for only five stations – WMYX, WKLH, WJMR, WSSP and WOKY.
The survey was conducted between Dec. 31 and Jan. 27.
At their best Holocaust films can never adequately capture the horror of concentration camps.
At their worst they fetishize a culture of death.
Then there's "Son of Saul," which is like an episode of "The Office" set in Hell.
It's about a slaughterhouse where people are murdered in assembly line fashion. Management wears uniforms but slave labor does the dirty work.
Prisoners themselves, called Sonderkommando, herd Jews off trains like cattle and into changing rooms where wary but hopeful people undress with promise of soup and showers, the latter of course a euphemism for the Final Solution.
The essence of "The Witch" is below the surface, just like the fears and anxieties that rattle around our subconscious despite rational evidence to the contrary.
It is not a routine don't-go-in-the-basement or -woods-style horror tale, its perhaps misleading title aside. Rather the Sundance Film Festival award winner finds its escalating tension in the unknowable.
This portrait of how superstition and conspiracy is used explain away anything people don't understand is set at a time when not much was understood.
In the documentary "Where To Invade Next" Michael Moore channels at least three of this election cycle's presidential candidates with his Trump-style bluster, Sanders-type slogans and Christie-like girth.
The last, size, matters only because the veteran liberal provocateur has been the face of his films from the very first and now at the risk of judging a book by its cover looks frail and unhealthy.
That said the globetrotting Moore gamely takes a European vacation and cooks up a revealing and entertaining recipe for ways to make America great again.
WDJT-TV (Channel 58) meteorologist Lance Hill is on a medical leave of absence from the station.
Sources said he is reportedly recovering from a stroke.
Hill, 45, who joined the station in 2011 has been off the air since November. He was meteorologist on WDJT's morning newscast.
Until recently his replacements said they were "filling in" for Lance.
Hill's absence has been noticed and commented on by viewers and members of the local broadcast community.
Overnight ratings for Sunday's telecast of Super Bowl on CBS earned a 50.6 average for WDJT-TV (Channel 58). That was higher than the national overnight rating of 49.
Local ratings grew throughout the course of the game peaking at 55.4 in the closing moments.
Overnight ratings are preliminary. In Sunday's game the Denver Broncos upset the Carolina Panthers, 24 to 10. A local rating point is the equivalent of 8,822 television homes.
The national overnight rating was the second highest ever for a Super Bowl game, beating last year's rating of 49.7 on NBC, according to MediaLife magazine.


Our January 2009 issue won't be out for a couple more weeks (unless you're a subscriber, in which case you probably already have it), but here's a little teaser of the DC Europe Tour for you. The entire DC team split up into two groups, one taking on Northern Europe and the other took to the South. Photogs Mike Blabac and Mike O'Meally kept up with them and delivered an amazing article. So to accompany that, check out these photos Mike Blabac sent us of sightseeing, relaxing, goofing off, and everything else that happens on tour that we just can't squeeze into the mag: Josh Kalis, Lindsey Robertson, Colin McKay, Wes Kremer, Greg Myers, PJ Ladd, Antony Lopez, Ruben Garcia, Jani Laitala, Jody Smith, all the fans, and more.


With the refreshed mental health strategy for Scotland being published today, it is timely that we report here on Positive Realities first conference held on Thursday 23 February 2017 – Care Well: Mental Health and Young Carers. We were keen to run this event to raise awareness of the mental health needs of young carers amongst practitioners, as many remain hidden carers and often do not get access to much needed support. We know from our work many young carers experience emotional difficulties, such as anxiety, depression and low confidence.
The event brought together some wonderful speakers and input from professionals who attended. Councillor Norman Work, Carers Champion helped us secure the Edinburgh City Chambers as our venue and welcomed everyone to the event. A big thank you to our Chairs on the day – Joan Fraser, Chair of the Children and Families Network, Edinburgh Voluntary Organisations Council and Hawys Kilday, Assistant Director of Children Services of Barnardo's Scotland. Also, thanks to Crescent Kitchen for providing a very tasty lunch!
Leading up to the event we had two 'Relax and Recharge' events for young carers at The Yard. The purpose of these events was predominantly to provide recreational and relaxation activities. A 'chill out' area with refreshments was also run, where we asked carers what issues they faced in life and what they wanted more support with. Interestingly, some young carers felt this was their favourite part of the event! They created an amazing vision board which was on display at the conference.
We were also grateful to welcome Marta Szpindor (a trustee of Positive Realities and a young adult carer), who took part in a question and answer session on her experience as a young carer. During the afternoon, we began thinking about how best to support young carers and what we should do moving forwards.
Edinburgh Young Carers gave a presentation on their services for young carers. Seamus Prior, Senior Lecturer, University of Edinburgh then introduced mental health first aid and how it can help young carers to look after themselves and the person they care for.
Our last presentation of the day was from Ella Edginton, Consultant, Blake Stevenson and Louise Morgan, Young Carers Development Manager, Carers Trust Scotland on the recent research by the Children and Young People's Commissioner Scotland into the impact of caring. The report is available here.
A more extended write up of the identified priorities for action noted by delegates and the presentations are available to download below*. We hope that organisations responsible for addressing the mental health of young people are more aware of the specific issues affecting young carers and ensure that actions to improve mental health consider how effectively these will address the needs of young carers, notably to reduce potential negative consequences of caring on emotional and mental health.


text:
What is an Arraignment Hearing?
As a part of a fair justice system, arraignment hearings play a very important role. In this hearing, the accused person is formally read the charges set against him/her. Let us now look at the various procedures that take place, and the importance of this hearing in a criminal trial.
Anuj Mudaliar
Preliminary vs. Arraignment Hearing
While an arraignment hearing determines whether probable cause exists to charge the defendant of the crime, a preliminary hearing determines whether enough evidence exists for a defendant to stand trial.
An arraignment hearing can be defined as 'A court hearing in a criminal case during which the charges are read out to the named accused, and he or she (unless insane or mute) must plead guilty or not guilty.' This hearing is mostly the first time that the defendant appears in front of a judge on criminal charges, after which he is read out the charges and is asked to enter a plea to the charges. It is also the first time the defendant meets the lawyer who will prosecute the case against him. During this hearing, it is also decided whether the defendant can be released on bail, pending trial.
It is important to note that arraignments are required in felony and misdemeanor cases, or basically any case in which the penalty can result in incarceration. If the accused has been kept in jail after an arrest, he must be brought before a judge for an arraignment hearing within 48 hours of being arrested, so that it can be determined whether the arrest was justified by a probable cause. Now that we have understood the meaning of an arraignment hearing, we shall study about what its actual purpose is.
Purpose of an Arraignment Hearing
An arraignment has to take place, as the defendant gets a hearing without much delay. Unreasonable delays are against the defendant's federal constitutional Sixth Amendment right to a speedy trial. If the arraignment is not scheduled for an unreasonably long period of time, despite an indictment being issued by the prosecutor's office, the defendant's lawyer can request the case to be dismissed. The judge then reviews the details to determine whether the delay is reasonable, and decide whether the case is to be dismissed.
What Happens at an Arraignment Hearing?
Formal Advisement of the Defendant's Rights: During an arraignment hearing, the court has to advise the defendant of their constitutional rights, such as their right to legal counsel, the right for a fair trial, and the right against self-incrimination. The defendant also has the right to have legal representation during the hearing. If such a desire is expressed, the court cannot hold an arraignment hearing without giving an opportunity for legal counsel, or the provision of a public defender.
Advisement About the Charges: After the rights are explained to the defendant, the court has to now inform the defendant about the charges that have been leveled against him. The judge may also have to read out the criminal complaint, indictment, and other informational documents related to the charges; for e.g. evidence related to the case. The defendant will also have to receive a copy of the charging document.
Entering of a Plea: After the defendant is advised about the charges, the judge will now ask the defendant how he pleads to the charges. The defendant can either plead guilty, not guilty, or no contest.
If the crime is a minor one, and the defendant pleads guilty, the judge can sentence the defendant at the arraignment itself. The defendant's lawyer and the prosecutor negotiate the guilty plea to set the sentence at this time. However, if the crime is a serious one, the judge will ask for a pre-sentence report, and set a separate date for the sentencing hearing.
If the defendant pleads not guilty, it means that he is making the state―represented by the prosecutor―prove the charges laid against him. Most defense attorneys recommend their clients to plead not guilty, as it forces the prosecutor to gather evidence against the defendant, and gives the defense attorney a chance to study the evidence and investigate the case to prove that the defendant did not commit the crime.
The defendant usually chooses the plea option of no contest when he acknowledges that the prosecutor has enough evidence to prove that he has committed the crime, but does not admit that he did it. When such a plea is entered, the court proceeds in the same way as a guilty plea. The difference between a guilty and no contest plea is that, a no contest plea is accepted by the court at the discretion of the judge, and it cannot be used in cases of death penalties. It is used by defendants, as this plea cannot be used by the prosecution to prove the person's guilt. It is also used to avoid going on a criminal trial in cases where the outcome is not certain, and where the defendant does not want details of the case to become public.
Setting Conditions for Release: The court also decides whether to release the defendant, pending the completion of the case. This decision is primarily based on the overall relation of the defendant with the community, and also if the community is put at risk by such a release, or if the defendant is likely to flee after being released. If the defendant has a small or no criminal record, and if the crime is a minor one, the court will release the accused on his word that he will attend all trials and proceedings on the case. In some cases, certain conditions are applied to a release. For example, the defendant may be asked to regularly report to a probation or supervising officer, keep away from witnesses, drugs, alcohol, and committing other crimes, etc. If these conditions are broken, the court can rescind the release order.
The court may also release the defendant on a monetary bond/bail. In such cases, the defendant has to give a refundable amount of money to the court as an assurance that he will attend the trial. If the defendant finds that he does not have the resources to pay the bond, a bail bondsman pays the bond to the court in return for a small amount of non-refundable money, usually 10% of the original bond amount, along with collateral, which can be claimed by the bondsman in case the defendant does not appear for the trial.
Arraignment Waivers
If the defendant has an attorney, he can also choose to waive off the arraignment hearing. In such cases, the defense attorney will communicate with the prosecutor and the court with a written application for the waiver. The attorney may also submit a document for the conditions of release along with the waiver application, or the court may allow the defendant to waive the arraignment, and set a separate date for the hearing on the conditions of release.
In all cases, it is recommended that the defendant contacts an attorney as soon as he receives the notice of arraignment, who will help throughout the process and discuss the various options available, reducing stress, and setting up favorable conditions of release.
Note: How courts exactly conduct arraignments and what occurs varies with each state's laws and its state constitution.
What Does a Frivolous Lawsuit Mean?
What is an Out of Court Settlement?
Are Lawsuit Settlements Deductible?


3 cubes to add as an extension to the award winning Rorys Story Cubes games. Each Rorys Story Cubes MIX set contains 3 cubes with a particular theme. They are designed to extend the play of Rorys Story Cubes. One of the first three sets in the series is Rorys Story Cubes Enchanted. Simply mix up these three dice with other Rorys Story Cubes to conjure up fantastic fairytales.


text:
Aptoceras jutaiana är en insektsart som beskrevs av Marius Descamps 1981. Aptoceras jutaiana ingår i släktet Aptoceras och familjen gräshoppor. Inga underarter finns listade i Catalogue of Life.

Källor

Gräshoppor
jutaiana

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}

SU(2) Yang-Mills-Higgs (YMH) theory, with the Higgs field
in the adjoint representation,
possesses globally regular particle-like solutions,
such as the
't Hooft-Polyakov magnetic monopole \cite{thooft}
and the Julia-Zee dyon,
which carries both magnetic and electric charge \cite{jul}.

In SU(2) Einstein-Yang-Mills-Higgs (EYMH) theory,
for small gravitational constant
the gravitating fundamental monopole
\cite{old,ewein,bfm}
and the gravitating fundamental dyon \cite{bhk}
emerge smoothly
from the corresponding flat space solutions.
The mass of the gravitating fundamental monopole \cite{ewein,bfm}
and dyon \cite{bhk} solutions decreases
with increasing gravitational constant,
corresponding to increasing coupling constant $\alpha$,
which is proportional to the ratio of vector meson mass and Planck mass.
The regular solutions cease to exist beyond some maximal value
of $\alpha$, depending on the electric charge $Q$
\cite{ewein,bfm,bhk,ewein3}.

Besides these globally regular solutions, in SU(2) EYMH theory
magnetic
\cite{ewein,bfm,bfm2,aichel} and dyonic \cite{bhk}
non-abelian black hole solutions exist.
They emerge from the globally regular solutions,
when a finite regular event horizon $x_h$ is imposed.
Consequently,
they have been characterized as ``black holes within magnetic monopoles''
\cite{ewein} or ``black holes within dyons'' \cite{bhk}.
Distinct from the corresponding embedded Reissner-Nordstr\o m (RN)
black holes \cite{rn},
these non-abelian black hole solutions
represent counterexamples to the ``no-hair'' conjecture,
because they carry non-trivial non-Coulomb-like fields
outside their horizon.
In contrast, pure
SU(2) EYM theory possesses neither regular dyon solutions \cite{gal1},
nor dyonic black holes other than embedded RN solutions \cite{gal2,popp}.

The magnetic non-abelian black holes
exist only in a limited domain of the $\alpha-x_h$ plane
\cite{ewein,bfm,bfm2}.
The domain of existence consists of two regimes,
where for fixed coupling constant $\alpha$ and varying
horizon radius $x_h$,
the solutions approach limiting solutions in two distinct ways.
At the transition point between these two regimes, given by
the critical value $\hat \alpha$, the maximal horizon radius
is attained \cite{bfm,bfm2}.
Limiting our investigations to vanishing Higgs self-coupling,
we here determine the domain of existence
of the dyonic non-abelian black holes,
finding also two regimes for the coupling constant $\alpha$.

Besides the fundamental gravitating monopole and dyon solutions
there are radially excited solutions \cite{bfm,bfm2,bhk},
where the gauge field function possesses nodes.
Both the radially excited monopole and dyon solutions
are related to the globally regular
Einstein-Yang-Mills (EYM) solutions,
found by Bartnik and McKinnon \cite{bm},
and, like these solutions, have no flat space counterparts.
Besides the radially excited globally regular dyon solutions,
we here consider the radially excited dyonic non-abelian
black hole solutions and determine their domain of existence.

In section II we derive the EYMH equations of motion.
We present the equations both in Schwarzschild-like coordinates,
employed in the numerical calculations \cite{bhk},
and in isotropic coordinates, to extend the analytical calculations
\cite{bfm2} to the dyonic case.
In section III we briefly review the embedded RN solutions.
We discuss the globally regular dyon solutions in section IV.
In addition to vanishing Higgs self-coupling,
we consider the fundamental solutions also for finite Higgs self-coupling,
in order to demonstrate that, as in flat space \cite{bkt},
a maximally possible charge $Q_{\rm max}$ arises.
In section V we discuss the dyonic non-abelian black hole solutions.
In particular, we derive the critical value $\hat \alpha$
for the dyonic solutions analytically and confirm it numerically.
For vanishing Higgs self-coupling,
we determine the domain of existence for the fundamental
and the first radially excited dyonic non-abelian black hole solutions,
and we discuss the pattern how the black hole solutions
approach limiting solutions.
We conclude in section VI.
In Appendix A, finally we show the local existence of the non-abelian
regular dyon and dyonic black hole solutions
at the origin and at the horizon, respectively.

\section{Einstein-Yang-Mills-Higgs Equations of Motion}

We consider the SU(2) EYMH action
\begin{equation}
S=S_G+S_M=\int L_G \sqrt{-\rm g} d^4x + \int L_M \sqrt{-\rm g} d^4x
\ \label{action}   \end{equation}
with
\begin{equation}
L_G=\frac{1}{16\pi G}{\cal R}
\ , \end{equation}
and
\begin{equation}
L_M = - \frac{1}{4} F_{\mu\nu}^a F^{a\mu\nu}
      - \frac{1}{2} D_\mu \phi^a D^\mu \phi^a
      - \frac{\beta^2 g^2}{4} (\phi^a \phi^a - v^2)^2
\ , \end{equation}
where
\begin{equation}
F_{\mu\nu}^a = \partial_\mu A_\nu^a - \partial_\nu A_\mu^a
 + g \epsilon^{abc} A_\mu^b A_\nu^c
\ , \end{equation}
\begin{equation}
D_\mu \phi^a = \partial_\mu \phi^a + g \epsilon^{abc} A_\mu^b \phi^c
\ , \end{equation}
$g$ is the gauge coupling constant, $\beta$ is the dimensionless
Higgs coupling constant, proportional to the ratio of Higgs boson mass
and vector boson mass,
and $v$ is the Higgs field vacuum expectation value.
Variation of the action eq.~(\ref{action}) with respect to the metric
$g_{\mu\nu}$, the gauge field $A_\mu^a$ and the Higgs field $\phi^a$
leads to the Einstein equations and the matter field equations.

\subsection{Ansatz}

For static spherically symmetric globally regular
and black hole solutions the metric can be parametrized as \cite{bfm2,bck}
\begin{equation}
ds^2=g_{\mu\nu}dx^\mu dx^\nu=
  - e^{2 \nu (R)} dt^2 + e^{2 \lambda (R)} dR^2
  + r^2(R) (d\theta^2 + \sin^2\theta d\phi^2)
\ . \label{genmet} \end{equation}

For the gauge and Higgs field we employ the
spherically symmetric ansatz \cite{bhk}
\begin{equation}
\vec A_t = \vec e_r J(r) v
\ , \end{equation}
\begin{equation}
\vec A_r=0 \ , \ \ \
\vec A_\theta =  -\vec e_\phi \frac{1- K(r)}{g} \ , \ \ \
\vec A_\phi =   \vec e_\theta \frac{1- K(r)}{g} \sin \theta
\ , \end{equation}
and
\begin{equation}
\vec \phi = \vec e_r H(r) v
\ , \end{equation}
with the standard unit vectors $\vec e_r$, $\vec e_\theta$ and $\vec e_\phi$.
For $A_t^a=0$, the solutions carry only magnetic charge
\cite{ewein,bfm,aichel}.

With these ans\"atze we obtain the action
\begin{eqnarray}
{S} = \frac{1}{G} \int dt dR e^{\nu+\lambda} && \Biggl(
    {1\over 2} \left[1+e^{-2\lambda} \left((r')^2
  +\nu'(r^2)'\right)\right] \Biggr. \nonumber\\
 &&+4 \pi G \left[
      e^{-2(\lambda+\nu)} \frac{r^2}{2} (J')^2 v^2
    + e^{-2\nu} K^2J^2v^2 \right. \nonumber\\
 && \Biggl. \left.
    - e^{-2\lambda} \left( \frac{(K')^2}{g^2}
    + {r^2\over 2} (H')^2v^2) \right) - V_2 \right]
                         \Biggr)
\ , \label{ac1} \end{eqnarray}
where $\nu$, $\lambda$, $r$, $K$, $J$ and $H$ are functions of $R$,
the prime indicates the derivative with respect to $R$, and
\begin{equation}
V_2 = {(1-K^2)^2\over{2g^2r^2}} + K^2 H^2 v^2
+ {\beta^2 g^2 \over 4} r^2 (H^2-1)^2 v^4
\ . \label{v2} \end{equation}

\subsection{Schwarzschild-like coordinates}

We first employ Schwarz\-schild-like coordinates,
corresponding to the gauge $r(R)=R$. Renaming $R=r$,
the spherically symmetric metric reads
\begin{equation}
ds^2=
  -A^2N dt^2 + N^{-1} dr^2 + r^2 (d\theta^2 + \sin^2\theta d\phi^2)
\ , \end{equation}
with the metric functions
\begin{equation}
A(r)= e^{\lambda + \nu}
\ , \label{a} \end{equation}
\begin{equation}
N(r)=1-\frac{2m(r)}{r} = e^{-2 \lambda}
\ , \label{n} \end{equation}
and the mass function $m(r)$.

We now introduce the dimensionless coordinate $x$
and the dimensionless mass function $\mu$,
\begin{equation}
x = g v r \ , \ \ \ \mu=g v m
\ , \label{xm} \end{equation}
as well as the dimensionless coupling constant $\alpha$
\begin{equation}
\alpha^2 = 4 \pi G v^2
\ . \end{equation}

The $tt$ and $rr$ components of the Einstein equations then yield
the equations for the metric functions,
\begin{eqnarray}
\mu'&=&\alpha^2 \Biggl( \frac{x^2 J'^2}{2 A^2}
   + \frac{J^2 K^2}{A^2 N}
   + N K'^2 + \frac{1}{2} N x^2 H'^2
\nonumber\\
 & &\phantom{ \alpha^2 \Biggl( }
   + \frac{(K^2-1)^2}{2 x^2} + H^2 K^2
   + \frac{\beta^2}{4} x^2 (H^2-1)^2 \Biggr)
\ , \label{eqmu} \end{eqnarray}
and
\begin{eqnarray}
 A'&=&\alpha^2 x \Biggl(
    \frac{2 J^2 K^2}{ A^2 N^2 x^2}
   + \frac{2 K'^2}{x^2} + H'^2 \Biggr) A
\ , \label{eqa} \end{eqnarray}
where the prime now indicates the derivative with respect to $x$.
For the matter functions we obtain the equations
\begin{eqnarray}
(A N K')' = A K \left( \frac{K^2-1}{x^2} + H^2 - \frac{J^2}{A^2 N}
 \right)
\ , \label{eqk} \end{eqnarray}
\begin{equation}
\left( \frac{x^2 J'}{A} \right)' = \frac{2 J K^2}{AN}
\ , \label{eqj} \end{equation}
and
\begin{eqnarray}
( x^2 A N H')' = A H \left( 2 K^2 + \beta^2 x^2 (H^2-1) \right)
\ . \label{eqh} \end{eqnarray}

Introducing the new function
\begin{equation}
 P = \frac{J}{A}
\label{p} \end{equation}
and using eq.~(\ref{eqa}), we see that
the metric function $A$ can be eliminated from the set of equations
(\ref{eqmu}), (\ref{eqk})-(\ref{eqh}).
These can then be solved separately, with the metric function $A$
being determined subsequently by (\ref{eqa}).

In the following we refer
to the above set of functions, variables and parameters,
also employed in \cite{bhk}, as notation I.

\subsection{Isotropic coordinates}

To make contact with the analytical results of \cite{bfm,bfm2}
and to extend them
to the case of gravitating dyons and dyonic black holes,
we now present the equations of motion in the notation of \cite{bfm2},
in the following referred to as notation II.
In the Schwarzschild gauge the following identifications hold
\begin{equation}
\begin{array}{ccccccccc}
\cite{bhk} : & x & A & N &
K & H & J & \alpha & \beta^2\\
\cite{bfm2} : & \alpha r & e^{\lambda+\nu} & e^{-2\lambda} &
W & \alpha H & J  & \alpha & \frac{\beta^2}{2}
\end{array}
\end{equation}

Along with \cite{bfm2}, we now employ
the gauge choice $e^{\lambda}={r(R)\over R}$, corresponding to
isotropic coordinates, and introduce the coordinate
\begin{equation}
\tau = \ln R
\ , \label{tau} \end{equation}
and the dot ( $\dot {} $ ) now indicates the derivative with respect to $\tau$.
To obtain a system of first order equations
we further employ for the first derivatives the new variables \cite{bfm2}
\begin{equation}
    N={\dot r\over r}\ , \ \ \kappa=\dot \nu + N \ ,
\ \ U={\dot W\over r}\ , \ \ V=\dot H
\ , \end{equation}
and we introduce
\begin{equation}
    B = e^{-\nu} J\ , \ \ C=\dot B
\ . \label{b} \end{equation}
(Note, that the symbol $N$ here
has a totally different meaning from eq.~(\ref{n}).)

Then the following system of
first order autonomous equations is obtained
\begin{eqnarray}
\label{autoi}
\dot r &=& Nr\\
\dot N &=& N(\kappa-N)-(2U^2+V^2) - 2\alpha^2B^2W^2\\
\dot \kappa &=& 1-\kappa^2+2U^2-{\beta^2r^2\over 2} (H^2-\alpha^2)^2-2W^2H^2 + 2\alpha^2
W^2B^2\\
\dot H &=& V\\
\dot V &=& {\beta^2r^2\over 2} (H^2-\alpha^2)H+2W^2H- \kappa V\\
\dot W &=& rU\\
\dot U &=& U(N-\kappa)+ {W(W^2-1)\over r} + Wr (H^2-\alpha^2B^2)\\
\dot B &=& C\\
\dot C &=& -\kappa C+B(2W^2-4U^2-V^2+\kappa^2-1 \nonumber \\
       &\ & +2W^2H^2+{\beta^2r^2\over 2} (H^2-\alpha^2)^2) - 4\alpha^2B^3W^2
\label{autof}
\end{eqnarray}
supplemented by the constraint
\begin{equation}
\label{contr}
  2\kappa N = 1+N^2+2U^2+V^2-2V_2
+ 2\alpha^2W^2B^2-\alpha^2(C+B(\kappa-N))^2
\end{equation}
compatible with the equations.

\section{Embedded Reissner-Nordstr\o m Solutions}

As noted long ago \cite{rn},
the Einstein-Yang-Mills-Higgs system admits embedded RN solutions.
In notation I, RN solutions
with mass $\mu_\infty$,
unit magnetic charge and arbitrary electric charge $Q$ are given by
\begin{equation}
\mu(x) = \mu_\infty - \frac{\alpha^2 (1 + Q^2)}{2x} , \ \ \ A(x)=1
\ , \end{equation}
\begin{equation}
K(x)=0 \ , \ \ \
J(x) =
  J_\infty
 - \frac{Q}{x} \ , \ \ \
H(x)=1
\ , \label{Q} \end{equation}
where $J_\infty$ is a priori arbitrary, but here chosen as
$J_\infty = Q/x_h$ (see eq.~(\ref{Jhor})).
At the regular horizon $x_h$ the metric function
\begin{equation}
  N(x) = {x^2 - 2x \mu_{\infty} + \alpha^2(1 + Q^2) \over x^2}
\end{equation}
vanishes, $N(x_h)=0$, yielding
\begin{equation}
      x_h = \mu_{\infty} + \sqrt{\mu_{\infty}^2 - \alpha^2 (1+Q^2)}
\end{equation}
or equivalently
\begin{equation}
     \mu_{\infty} = {x_h^2 + \alpha^2 (1+Q^2) \over 2 x_h}
\ . \end{equation}
For fixed values of $\alpha$ and $Q$, RN
solutions exist for
$x_h \geq \alpha \sqrt{1+Q^2}$,
independent of $\beta$.

In the extremal case
\begin{equation}
 x_h =  \mu_{\infty} = \alpha \sqrt{1+Q^2}
\ , \label{exh} \end{equation}
extremal RN solutions are obtained.
Extremal RN solutions
are characterized by $Q$ and $\alpha$.
In particular, for extremal RN solutions
the function $B(x)$ defined in (\ref{b}) becomes constant
\begin{equation}
     B = {J \over A \sqrt{N}} = {Q \over \alpha \sqrt{1+Q^2}}
\ . \label{brn} \end{equation}

\section{Dyon Solutions}

Let us first consider the globally regular particle-like solutions
of the SU(2) EYMH system.

In the Prasad-Sommerfield limit, $\beta=0$,
the dyon solutions in flat space are known analytically \cite{jul},
whereas for finite $\beta$ they are obtained only numerically
\cite{bkt}.
In the presence of gravity, the corresponding gravitating
monopole and dyon solutions are obtained only numerically as well.
The gravitating dyon solutions have many features in common
with the gravitating monopole solutions \cite{bhk}.

After presenting the boundary conditions for the asymptotically
flat globally regular solutions, we here briefly discuss
the fundamental dyon solutions
both in the Prasad-Sommerfield limit and for finite $\beta$.
Then we turn to the excited dyon solutions.

\subsection{Boundary conditions}

Requiring asymptotically flat solutions implies in notation I
that the metric functions $A$ and $\mu$ both
approach a constant at infinity.
We here adopt
\begin{equation}
A(\infty)=1
\ , \end{equation}
and $\mu(\infty)=\mu_\infty$ represents the dimensionless mass
of the solutions.
The matter functions also approach constants asymptotically,
\begin{equation}
K(\infty)=0 \ , \ \ \ J(\infty)= J_\infty \ , \ \ \ H(\infty) = 1
\ , \end{equation}
where for magnetic monopole solutions $J_\infty = 0$.
The asymptotic fall-off of the function $J(x)$ determines the dimensionless
electric charge $Q$ (see eq.~(\ref{Q})).

Regularity of the solutions at the origin requires
\begin{equation}
\mu(0)=0
\ , \end{equation}
and \cite{jul}
\begin{equation}
 K(0)=1 \ ,  \ \ \ J(0) = 0 \ , \ \ \ H(0)=0
\ . \label{bc0} \end{equation}
The local existence of a family of analytic solutions
obeying these conditions is shown in
Appendix A.1.

\subsection{Fundamental dyons}

\boldmath
\indent {\bf $\beta=0$}
\unboldmath

Like the gravitating monopole solutions, the gravitating dyon
solutions exist up to
a maximal value of the coupling constant $\alpha$.
Beyond this value no dyon solutions exist.
The fundamental dyon branch
does not end at the maximal value $\alpha_{\rm max}$,
but bends backwards and extends
up to the critical value $\alpha_c$.
Since $\alpha^2=4\pi G v^2$, variation of the coupling constant
along the fundamental dyon branch can be considered
as first increasing $G$ with $v$ fixed
up to the maximal value $\alpha_{\rm max}$,
and then decreasing $v$ with $G$ fixed
up to the critical value $\alpha_c$.

Completely analogously to the fundamental monopole branch \cite{bfm},
the fundamental dyon branch reaches a limiting solution
at the critical value $\alpha_c$,
where it bifurcates with the branch of extremal RN solutions of
unit magnetic charge and electric charge $Q$ \cite{bhk}.
The critical value $\alpha_c(Q)$ depends only slightly on the charge $Q$
\cite{bhk}.

For $\alpha \rightarrow \alpha_c$
the minimum of the metric function $N(x)$ of the dyon solutions
decreases monotonically, approaching zero
at $x_c = \alpha_c \sqrt{1+Q^2}$.
For $x \ge x_c$,
the metric function $N(x)$ of the limiting solution
corresponds to the metric function
of the extremal RN black hole with horizon
$x_h = x_c = \alpha_c \sqrt{1+Q^2}$,
unit magnetic charge and electric charge $Q$.
Likewise, for $x \ge x_c$,
the other functions of the limiting solution
correspond to those of this extremal RN black hole \cite{bhk}.
Consequently, also the mass of the limiting solution
coincides with the mass of this extremal RN black hole.

On the interval $0 \le x \le x_c$
the functions $N(x)$, $K(x)$ and $H(x)$ of the limiting solution
vary smoothly from their respective boundary values at $x=0$
to those of the extremal RN solution at $x_c$,
whereas the function $J(x)$ is identically zero.
The metric function $A(x)$ is identically zero, as well,
on the interval $0 \le x < x_c$,
but discontinuous at $x_c$.
Consequently, in the limiting spacetime
the inner and outer parts are not analytically connected
\cite{ewein,bfm}.

\boldmath
\indent {\bf $\beta>0$}
\unboldmath

Let us briefly consider the dyon solutions for
finite Higgs self-coupling, $\beta > 0$,
because we here encounter a phenomenon,
also present for the black hole solutions at
vanishing Higgs self-coupling, $\beta=0$.

In flat space dyon solutions of arbitrarily large charge exist
only for $\beta = 0$.
In contrast, for finite values of $\beta$ dyon solutions exist only up to
a maximal value of the charge, $Q_{\rm max}(\beta)$ \cite{bkt}.
As the maximal value of the charge is approached,
the function $J(x)$ approaches asymptotically the limiting value
\begin{equation}
\lim_{Q \rightarrow Q_{\rm max}} J_\infty = 1
\ . \label{Jlim} \end{equation}
At this point the solutions change character and become oscillating
instead of asymptotically decaying \cite{bkt}.

As illustrated in Figs.~1-2,
this phenomenon persists in curved space.
In Fig.~1 we show the mass
of the flat space dyon (solid line) and of the
gravitating dyon (dashed line, corresponding to $\alpha = 0.5$)
as a function of the charge $Q$
for $\beta^2=0$ and $\beta^2=0.5$.
In Fig.~2 the corresponding asymptotic values of the function
$J(x)$ are presented.
We note, that for finite $\beta$
also gravitating dyon solutions exist only up to
a maximal value of the charge,
where $J_\infty \rightarrow 1$.

\subsection{Radially excited dyons}

Besides the branch of fundamental dyon solutions
there are branches of radially excited dyon solutions,
where the gauge field function $K(x)$
of the $n$-th radially excited dyon solution has $n$ nodes.

These solutions have no flat space counterparts, and
the variation of $\alpha$ along a branch of excited solutions
must be interpreted as a variation of $v$ with $G$ fixed.
In the limit $\alpha \rightarrow 0$ the Higgs field vacuum
expectation value therefore vanishes, while $G$ remains finite.
Because of the particular choice of dimensionless variables (\ref{xm}),
in this limit the solutions shrink to zero size
and their mass $\mu$ diverges.
As for the radially excited monopole solutions \cite{bfm},
the coordinate transformation $\tilde x = x/\alpha$
leads to finite limiting solutions in the limit $\alpha \rightarrow 0$,
which are the Bartnik-McKinnon solutions \cite{bhk}.

In Fig.~3 we show the normalized mass $\mu_\infty/\alpha$
as a function of $\alpha$
for the first excited dyon branch
with electric charge $Q=1$ and $\beta=0$.
For comparison also the
first excited monopole branch is shown.

Like the radially excited monopole solutions,
the radially excited dyon solutions
exist only below a critical value
of the coupling constant $\alpha$.
For the radially excited monopole solutions this critical value is
$\alpha_c = \sqrt{3}/2$ \cite{bfm,bfm2}.
For the radially excited dyon solutions the critical value is larger
and will be discussed in the context of the dyonic black hole solutions.

\section{Black Hole Solutions}

We now turn to the dyonic black hole solutions of the
SU(2) EYMH system, choosing $\beta=0$.
Again, the SU(2) EYMH dyonic black holes
have many features in common with the
magnetic non-abelian black holes \cite{bhk}.
In particular,
dyonic non-abelian black hole solutions exist in a limited domain of the
$\alpha$-$x_h$ plane, which depends on the charge $Q$,
and, in the limit $x_h \rightarrow 0$,
the corresponding globally regular solutions are obtained.
But a new phenomenon occurs for small values of $\alpha$,
where the non-abelian solutions no longer bifurcate with
non-extremal RN solutions.

In the following, we briefly present the boundary conditions.
We generalize the considerations of \cite{bfm2} to dyonic solutions
and derive analytically the critical value
of the coupling constant, $\hat \alpha$.
We then present our numerical calculations for the
fundamental dyonic black hole solutions and their radial excitations.

\subsection{Boundary conditions}

Imposing the condition of asymptotic flatness,
the black hole solutions satisfy the same
boundary conditions at infinity
as the regular solutions.
The existence of a regular event horizon at $x_h$
leads in notation I to the conditions for the metric functions
\begin{equation}
\mu(x_h)= \frac{x_h}{2}
\ , \end{equation}
and $A(x_h) < \infty $,
and for the matter functions
\begin{eqnarray}
 {N' K' }|_{x_h} =  \left. K \left( \frac{K^2-1}{x^2} + H^2
 \right) \right|_{x_h}
\ , \end{eqnarray}
\begin{equation}
 J |_{x_h} =0
\ , \label{Jhor} \end{equation}
and
\begin{eqnarray}
 {x^2  N' H' }|_{x_h} =  \left.
   H \left( 2 K^2 + \beta^2 x^2 (H^2-1) \right)
  \right|_{x_h}
\ . \end{eqnarray}
The local existence of a family of solutions
obeying these conditions at the horizon is
demonstrated in Appendix A.2.

\boldmath
\subsection{Critical value of $\alpha$}
\unboldmath

For magnetic black holes, there are two
regimes of the coupling constant $\alpha$,
corresponding to two distinct patterns of reaching
a limiting solution as a function of the horizon radius $x_h$.
For larger values of $\alpha$, the solutions bifurcate with
an extremal RN black hole solution,
when the horizon radius appoaches its critical value $x_h^{\rm cr}$.
Here the solutions tend towards the corresponding extremal RN solution
with horizon radius $x_h^{\rm RN} = \alpha$
only on the interval $x \ge x_h^{\rm RN}$,
whereas they tend to a generic non-abelian limiting solution
on the interval $x_h^{\rm cr} \le x \le x_h^{\rm RN}$ \cite{bhk}.
In contrast for smaller values of $\alpha$ the solutions
bifurcate with a non-extremal RN solution on the full interval
$x \ge x_h^{\rm cr}$ \cite{bfm,bfm2}.
The transition point between these two regimes corresponds
to the critical value $\hat \alpha$,
where the non-abelian black hole solutions tend towards the extremal RN
solution with horizon radius $x_h^{\rm RN} = \hat \alpha$
on the full interval $x \ge x_h^{\rm cr} = x_h^{\rm RN}$,
i.e.~$x_h^{\rm cr}$ and $x_h^{\rm RN}$ coincide.
For the magnetic non-abelian black holes
this critical value is given by
$\hat \alpha = \sqrt{3}/2$ \cite{bfm,bfm2}.

Analogously, for dyonic non-abelian black holes there are
also two regimes of the coupling constant $\alpha$,
with $\hat \alpha$ marking
the transition point between these two regimes.
We now derive this critical value $\hat \alpha$
for the dyonic non-abelian black hole solutions, following closely
the reasoning of \cite{bfm2}.

Let us then consider the fixed points
of the system (\ref{autoi})-(\ref{autof}).
Employing notation II, the relevant fixed point is given by
the configuration
\begin{equation}
\label{fixp}
H_h = \alpha \ , \ \  W_h = 0 \ , \ \ \kappa_h=1 \ , \ \
r_h = {1\over  \sqrt{1- \alpha^2 B_h^2}}
\ , \end{equation}
where $N_h = V_h = U_h = C_h = 0$,
while $B_h$ is such that
$0 \leq B_h \leq 1/ \alpha$.

Linearization of the equations about this fixed point leads to the
following eigenvalues of the matrix defining the linear part
(adopting the order $N$, $W$, $U$, $H$, $V$, $P$, $Q$, $\kappa$)
\begin{eqnarray}
\label{eig0}
\gamma_0 &=& 1\\
\gamma_{1,2} &=& -{1\over 2} \pm i \sqrt{   {3\over 4}-  \alpha^2
 {{1 -B^2_h} \over {1 - \alpha^2 B_h^2}}   }
\label{eig12}\\
\gamma_{3,4} &=& -{1\over 2} \pm \sqrt{{1\over 4} + \alpha^2\beta^2r_h^2}\\
\gamma_5 &=& 0\\
\gamma_6 &=& -1\\
\gamma_7 &=& -2
\label{eig7}
\end{eqnarray}
In particular,
we see that the eigenvalues $\gamma_{1,2}$,
which are related to the function $W$
and determine the critical value $\hat \alpha$ for the magnetic
black holes \cite{bfm2},
now depend on $B_h$. The zero mode $\gamma_5$ is related to the
occurrence of this free parameter.

For $Q=0$, the critical value of $\alpha$ corresponds to the
transition of the eigenvalue $\gamma_{1,2}$ (eq.~(\ref{eig12}) for $Q=0$)
from complex to real value \cite{bfm2}.
Repeating this reasoning for dyonic black holes,
we conclude, that the corresponding critical value of the coupling constant
for the dyonic non-abelian black holes is given by
\begin{equation}
\hat \alpha^2 = {3\over{4-B^2_h}}
\ . \label{acrit} \end{equation}

Here the relation of the critical value $\hat \alpha$ to
the charge $Q$ seems only indirect, since the value of the function
$B(x)$ at the horizon enters in eq.~(\ref{acrit}).
However, for the dyonic non-abelian black holes
$\hat \alpha$ also represents the special point,
where the non-abelian black hole solutions tend towards the
corresponding extremal RN
solution with horizon radius $x_h^{\rm RN} = \hat \alpha \sqrt{1+Q^2}$
on the full interval $x \ge x_h^{\rm cr} = x_h^{\rm RN}$.
This implies for the function $B(x)$
according to eq.~(\ref{brn})
\begin{equation}
\label{valp}
    \lim_{\alpha \rightarrow \hat \alpha} B(x) =
{Q \over \hat \alpha \sqrt{1+Q^2} }  \ ,  \ \   \forall x > x_h^{\rm RN}
\ . \end{equation}
Consequently, we may insert for $B_h$ in eq.~(\ref{acrit})
the constant RN value, eq.~(\ref{brn}),
and obtain for the critical coupling constant the expression
\begin{equation}
    \hat \alpha(Q) =  \sqrt{{3 + 4 Q^2 \over 4(1+Q^2)}}
\ , \label{ahat} \end{equation}
which now depends on the electric charge $Q$.

\subsection{Fundamental dyonic black holes}

Let us now define some quantities helpful in the analysis
of the numerical results.
Denoting the set of functions of the extremal RN solution
with horizon radius $x_h^{\rm RN} = \alpha \sqrt{1+Q^2}$
by $(N_{\rm RN},K_{\rm RN},H_{\rm RN},P_{\rm RN})$,
and denoting the set of functions of the non-abelian black hole solution
with horizon radius $x_h$ (with $x_h < x_h^{\rm RN}$)
by $(N,K,H,P)$, we define
\begin{equation}
     D N  = {\rm max}_{x \in [x_h^{\rm RN}, \infty]}
  \vert N_{\rm RN}(x) - N(x) \vert
\ , \label{dn} \end{equation}
and analogously we define the quantities $D K$, $D P$ and $D H$.
Clearly the quantities $DN$, $DK$, $DP$ and $DH$
must vanish, when the non-abelian black hole solutions
bifurcate with the corresponding extremal RN solution.
Therefore these quantities help
to determine the critical values with good accuracy
in the regime $\alpha \ge \hat \alpha$.

\boldmath
{\rm $Q=0$}
\unboldmath

Our numerical evaluation of the domain of existence
of the magnetic non-abelian black holes
in the $\alpha$-$x_h$ plane
is in agreement with the results of \cite{bfm,bfm2},
and in particular we confirm $\hat \alpha = \sqrt{3}/2$.
Considering the quantities $DN$, $DK$ and $DH$ (eq.~(\ref{dn}))
as functions of the horizon radius $x_h$,
we observe that for $\alpha \ge \hat \alpha$
the three functions approach zero at a common
value $x_h^{\rm cr}(\alpha) \le \hat \alpha$.
As $\alpha - \hat \alpha$ changes sign,
in particular the quantity $DK$ changes drastically,
becoming a convex function
when the critical horizon radius $x_h^{\rm cr}$
is approached.

\boldmath
{\rm $Q \ne 0$}
\unboldmath

We have numerically determined the domain of existence
of the fundamental dyonic non-abelian black hole solutions
in the $\alpha$-$x_h$ plane,
which is shown in Fig.~4 for $Q=1$.
The straight line indicates the extremal RN solutions, dividing the
domain of existence into a lower region with non-abelian
black holes only and an upper region with both non-abelian and
non-extremal abelian black holes, completely analogously
to the case of magnetic black holes.

To start the detailed discussion of the diagram,
we choose a small fixed value of the horizon radius $x_h$
and vary $\alpha$.
Then the dyonic black hole solutions
exist only up to some maximal value $\alpha_{\rm max}(x_h)$.
>From $\alpha_{\rm max}(x_h)$
a second branch extends backwards until a critical
value $\alpha_c(x_h)$ is reached.
With increasing $x_h$ the second branch becomes increasingly smaller,
and finally disappears.
The critical values $\alpha_{\rm max}(x_h)$ and
$\alpha_c(x_h)$ are both shown in Fig.~4.

The presence of the two branches is illustrated in Fig.~5
for $Q=1$ and $x_h = 0.8$,
where the quantities $DN$, $DK$, $DP$ and $DH$
are shown as functions of the parameter $\alpha$.
Here the second branch of solutions only exists
in the small interval $1.1986 \le \alpha \le 1.2002$.

For fixed $x_h$ and varying $\alpha$,
the functions of the black holes solutions evolve
completely analogously to those of the regular dyon solutions.
Consequently, the limiting solution reached
at the critical value $\alpha_c(x_h)$
consists of two parts, the outer part
corresponding to the exterior of the extremal RN black hole with horizon
$x_h^{\rm RN} = \alpha_c \sqrt{1+Q^2}$,
unit magnetic charge and electric charge $Q$
and the inner part representing a genuine non-abelian solution.

Similarly for fixed $\alpha > \hat \alpha$ and varying $x_h$,
the limiting solution reached
consists of two parts, the outer part
corresponding to the exterior of the extremal RN black hole with horizon
$x_h^{\rm RN} = \alpha \sqrt{1+Q^2}$,
unit magnetic charge and electric charge $Q$,
as demonstrated in Figs.~6-7 for the black hole solutions
with horizon $x_h=1$, 1.1 and 1.153,
charge $Q=1$ and $\alpha=1$ for the functions
$N$ and $P$ and the functions $K$ and $H$, respectively.

According to eq.~(\ref{ahat}), for $Q=1$
the critical value $\hat \alpha$ is given by
$\hat \alpha = \sqrt{7/8} \approx 0.935$.
Here the transition
between the two regimes with different bifurcation patterns
is supposed to occur.
Indeed, our numerical calculations confirm this critical value,
as demonstrated in Figs.~8-9, where
the four quantities $DN$, $DK$, $DP$ and $DH$
are shown as functions of the horizon radius $x_h$
for $\alpha=0.94$ and $\alpha=0.93$, respectively.

For $\alpha=0.94$, which is slightly above $\hat \alpha$,
the curves in Fig.~8 clearly approach zero
at $x_h^{\rm cr} \approx 1.235$. This value is well below
the horizon value of the corresponding extremal RN solution,
$x_h^{\rm RN}= \alpha \sqrt{1+Q^2} \approx 1.329$.
Moreover, in this limit
$x_h \rightarrow x_h^{\rm cr}$,
the corresponding values of $K(x_h)$ and $H(x_h)$
do not tend to their RN values of zero and one, respectively,
but they converge to generic numbers in the interval $[0,1]$.

In contrast, for $\alpha=0.93$, which is slightly below $\hat \alpha$,
the function $DK$ becomes a convex function
when the critical horizon radius $x_h^{\rm cr}
\approx 0.93 \sqrt{2} \approx 1.315$ is approached.
Furthermore, the quantities $K(x_h)$ and $H(x_h)$
tend to their RN values zero and one, respectively,
for $x_h \rightarrow x_h^{\rm cr}$.
Thus for $\alpha = 0.93$ the limiting solution
represents a RN solution on the full interval
$x \ge x_h^{\rm cr}$.

Clearly, the transition point $\hat \alpha$
occurs inbetween these two values.
Approaching $\hat \alpha$ further from both sides, the value
$\hat \alpha = \sqrt{7/8} \approx 0.935$ is confirmed.
The gap in Fig.~4 on the rhs of $\hat \alpha$
represents a tiny region, numerically not accessible
with sufficient accuracy \cite{foot}.
We have confirmed the validity of eq.~(\ref{ahat})
also for other values of the charge $Q$.

In the regime $\alpha < \hat \alpha$, we observe that
the maximal value of the horizon radius $x_h$ decreases
with decreasing $\alpha$,
completely analogously to the magnetic case.
Continuing our detailed discussion of the approach to the limiting
solution in this regime, however, we observe differences to
the magnetic case for smaller values of $\alpha$ and larger values of $Q$.

For fixed $\alpha$ close to $\hat \alpha$ and increasing $x_h$,
the dyonic black hole solutions bifurcate with a RN solution
when the maximal value of the horizon is reached.
The limiting solution corresponds to the exterior of the RN solution
on the full interval $x \ge x_h^{\rm cr}$.
For smaller values of $Q$ and
somewhat smaller fixed $\alpha$, with increasing $x_h$
the solutions do not yet bifurcate with a non-extremal RN solution,
when the maximal value of the horizon is reached.
Instead a second branch of solutions emerges,
extending backwards to lower values of the horizon radius,
until it bifurcates with a non-extremal RN solution
at the critical value of the horizon $x_h^{\rm cr}$ \cite{bfm,bfm2,bhk}.
Moving along both branches,
the values of $K(x_h)$ and $H(x_h)$ change monotonically,
reaching their respective RN values of zero and one as the critical
horizon is reached.

For the magnetic black holes as well as
for the dyonic black holes with smaller values of $Q$
this latter bifurcation pattern persists
with decreasing $\alpha$ \cite{bfm,bfm2}.
In contrast,
for the dyonic non-abelian black holes with larger values of $Q$
new phenomena occur.

We exhibit these new phenomena in Fig.~10,
where the critical region of the $\alpha$-$x_h$ plane
shown in Fig.~4 for $Q=1$ is enlarged and more details are given.
First, we observe the occurrence of bifurcations,
which lead to the small triangular region $ABC$,
where three solutions exist.
Thus below $\hat \alpha$
we find four distinct regions in the $\alpha$-$x_h$ plane.
With decreasing $\alpha$ and
increasing $x_h$ there are
i) for $0.605 < \alpha$
first one, then zero solutions,
ii) for $0.575 < \alpha < 0.605$
first one, then three, then one, then zero solutions,
iii) for $0.535 < \alpha < 0.575$
first one, then three, then two, then zero solutions
and iv) for $\alpha < 0.535$
first one, then two, then zero solutions.

Second, with decreasing $\alpha$,
the value $J_\infty$ of the limiting solution increases.
When it reaches its maximal value of one,
the function $K(x)$ ceases to decay exponentially.
The limiting solution then no longer represents
a non-extremal RN solution,
instead an oscillating solution is reached as the limiting solution.
The corresponding critical point,
where the transition from the limiting non-extremal RN solutions
to the oscillating solutions occurs, is labelled $D$ in Fig.~10.
Along the curve $BD$
the maximal value of the horizon radius is reached
when the limiting value $J_\infty=1$ is attained,
whereas along the curves $AB$ and $A'A$
an intermediate extremal value of the horizon radius is reached
when the limiting value $J_\infty=1$ is attained.

Figs.~11-13 illustrate both phenomena,
representing the values $K(x_h)$, $H(x_h)$ and $J_\infty$
as functions of the horizon radius
for $\alpha=0.7$, 0.55 and 0.2, respectively.
As seen in Fig.~11, for $\alpha=0.7$
only one branch of solutions exists.
Here, with increasing $x_h$
$K(x_h)$ decreases monotonically to zero,
$H(x_h)$ increases monotonically to one,
while $J_\infty$ increases monotonically to a limiting value
smaller that one.
Decreasing $\alpha$, the critical point $C$ of Fig.~10 is reached,
below which three branches of solutions exist.
Moving along the three branches,
$K(x_h)$ decreases monotonically, $H(x_h)$ increases monotonically
and $J_\infty$ increases monotonically until it reaches one,
as seen in Fig.~12 for $\alpha = 0.55$.
For still smaller values of $\alpha$,
at the critical value $A$, the third branch
disappears, leaving two branches which end
when $J_\infty$ reaches one.
This is seen in Fig.~13 for $\alpha = 0.2$.
The maximal horizon radius in this case is approximately 0.917.
For small values of $\alpha$ (i.e.~below the critical point $A$)
the lower curve in Fig.~4
represents the critical value of the horizon,
where the asymptotically exponentially decaying solutions cease to exist.

Considering the $Q$-dependence of the new phenomena, we observe that
the bifurcations leading to three branches arise only for $Q \ge 0.8$,
and the limiting value $J_\infty = 1$ is reached
only for $Q \ge 0.75$.
The latter is seen in Fig.~14, where
the critical value $D$ is shown, which marks the transition from
the limiting non-extremal RN solutions
to the oscillating solutions.
Also shown in Fig.~14 is the critical value $\hat \alpha$.
We note, that
with increasing $Q$ the two curves get increasingly closer.

\subsection{Excited dyonic black holes}

Besides the fundamental magnetic black hole solutions
there exist radially excited black hole solutions,
for which the gauge function $K(x)$ possesses $n$ nodes \cite{bfm,bfm2}.
These radially excited solutions
exist only for $\alpha \le \hat \alpha = \sqrt{3}/2$ \cite{bfm,bfm2}.

Our numerical analysis of the radially excited dyonic black hole solutions
strongly indicates that,
at least for $n=1$, the excited dyonic black hole solutions penetrate
into a small domain of the $\alpha > \hat \alpha$ regime,
as can already be anticipated from Fig.~3, where the
first excited regular dyon solution is shown for charge $Q=1$.
Indeed, we observe that the maximal value of $\alpha$,
where the radially excited black hole solutions
cease to exist, increases more strongly with $Q$
than the critical value $\hat \alpha$.

Let us now consider the domain of existence of the black hole
solutions in the $\alpha-x_h$ plane in more detail.
In the regime $\alpha > \hat \alpha$,
for fixed $x_h$ and increasing $\alpha$
the solutions again reach a limiting solution
at the critical value $\alpha_c(x_h)$,
which consists of two parts, the outer part
corresponding to the exterior of the extremal RN black hole with horizon
$x_h^{\rm RN} = \alpha_c \sqrt{1+Q^2}$,
unit magnetic charge and electric charge $Q$.

For $\alpha \rightarrow \alpha_c(x_h)$
the function $N(x)$ develops a progressively decreasing minimum,
$N_{\rm min}$,
reaching zero at $x_h^{\rm RN}= \alpha_c(x_h) \sqrt{1+Q^2}$.
This is illustrated in Fig.~15, where the value of
$N_{\rm min}$ is shown as a function of $\alpha$ for the horizon radii
$x_h=0.01$, 0.4 and 0.8 and charge $Q=1$.
With increasing $x_h$ the value of $\alpha_c(x_h)$ decreases,
though it remains greater than $\hat \alpha$
even for $x_h=0.8$, as inspection of
the four quantities $DN$, $DK$, $DP$ and $DH$ reveals.

In Fig.~16 we show the functions $N(x)$, $K(x)$, $H(x)$ and $P(x)$
of the first radially excited black hole solution
for charge $Q=1$, horizon radius $x_h=0.4$ and
$\alpha=0.938 > \hat \alpha$.
The minimum of the function $N(x)$,
which here occurs close to $x_h^{\rm RN}= \alpha_c(x_h) \sqrt{1+Q^2}$,
remains well separated from the horizon $x_h$
for $\alpha \rightarrow \alpha_c(x_h)$.

Considering finally the first excited black hole solutions
for small fixed $\alpha$ and increasing $x_h$, we observe that
as for the fundamental black hole solutions,
the quantity $J_\infty$ here plays a major role.
With increasing $x_h$, $J_\infty$ approaches its maximal value one,
where the asymptotically exponentially decaying solutions cease to exist.
For $\alpha = 0.2$, for instance, this happens at $x_h \approx 0.28$.

\section{Conclusions}

In analogy to gravitating monopoles \cite{ewein,bfm,ewein3}
also gravitating dyons \cite{bhk} exist.
When a regular horizon $x_h$ is imposed,
from these solutions ``black holes within monopoles'' \cite{ewein,bfm}
and ``black holes within dyons'' \cite{bhk} emerge.
Besides the fundamental regular and black hole solutions
also radially excited solutions exist \cite{bfm,bfm2,bhk},
related to the corresponding EYM solutions \cite{bm,su2}.
The static spherically symmetric ``black holes within monopoles''
and ``black holes within dyons''
provide counterexamples to the ``no-hair conjecture''.

The domain of existence of the fundamental dyonic non-abelian black hole
solutions in the $\alpha-x_h$ plane is similar to the one of the
fundamental magnetic non-abelian black hole
solutions.
There are two regimes of the coupling constant $\alpha$.
For $\alpha < \hat \alpha$,
the maximal horizon radius increases with increasing $\alpha$,
whereas for $\alpha > \hat \alpha$ it decreases.
The transition point between these two regimes, $\hat \alpha$,
depends on the charge $Q$ of the solutions,
$\hat \alpha =  \sqrt{(3 + 4 Q^2)/(4(1+Q^2))}$.

For fixed $\alpha$ and varying horizon radius,
a limiting solution is approached.
For $\alpha > \hat \alpha$ the limiting solution
consists of two distinct parts. The outer part
corresponds to the exterior of an extremal RN black hole solution
with horizon radius $x_h^{\rm RN} = \alpha \sqrt{1+Q^2}$,
unit magnetic charge and electric charge $Q$,
whereas on the interval $x_h \le x < x_h^{\rm RN}$
the limiting solution has the features of generic non-abelian solutions.
At the transition point $\alpha = \hat \alpha$ the limiting solution
corresponds precisely to the exterior of the extremal RN black hole solution
with horizon radius $x_h^{\rm RN} = \hat \alpha \sqrt{1+Q^2}$,
on the full interval $x \ge  x_h$.
In contrast, for $\alpha < \hat \alpha$
the limiting solution
represents the exterior of a non-extremal RN solution
for the larger values of $\alpha$, while for the smaller values of
$\alpha$ the dyonic non-abelian black hole solutions
encounter a critical point, where the solutions
no longer are exponentially decaying but become oscillating.

The domain of existence of the
radially excited dyonic non-abelian black hole
solutions in the $\alpha-x_h$ plane is similar to the one of the
fundamental solutions.
Again, there are two regimes of the coupling constant $\alpha$
with the transition point $\hat \alpha$.
This is in contrast to the
radially excited magnetic non-abelian black hole solutions,
which exist only up to $\hat \alpha$ \cite{bfm,bfm2}.

In a large part of their domain of existence,
the magnetic non-abelian black hole solutions are classically stable
\cite{ewein,bfm,bfm2,holl}.
In contrast,
dyonic non-abelian black hole solutions should be classically unstable.
As for the classical dyon solutions in flat space,
their mass should be lowered continuously,
by lowering the electric charge,
as long as there is no charge quantization
\cite{jul}.

redpajama_set_name: RedPajamaArXiv


Anyone with a valid NetID has access to the university's Google G Suite subscription. One of the features of the G Suite is access to Google's Team Drives. Team Drives allow for easy cloud file storage and collaboration, as you can specify users who can access all files in a given drive. You can also give access to Google users outside of the university.
1. To set up a Google Team Drive, you must first log in to your UW G Suite account. You can do this by navigating to https://apps.google.wisc.edu or by logging in to Google using [your_netID]@wisc.edu, which will redirect you to the NetID login page.
2. From there, click on Team Drives, and then New, to create a new team drive.
4. You can search for other UW members by name or email, or enter the email address of members outside of the university.


Making their first trip to Hugoton since 2000, Liberal won 57-43. The Redskins were able to get points in transition in the second half to pull away for the road win over the third ranked team in 3A.
The Redskins led 9-8 after one quarter and 21-20 at the half. LHS bolted to a 40-30 lead after three. The Skins led 45-31 with 4:59 to play. They struggled making free throws and layups down the stretch but won. Hugoton's Zack Leininger, who averages 14 points and eight rebounds per game, was injured in the first half and did not play in the second half.
Both teams struggled at the foul line as LHS was 14-26 at the foul line. They shot 48 percent from the field and were 3-10 from three point range. Hugoton was 9-19 at the foul line and 3-17 from three.
Liberal got 16 from Markalyn Eatmon and 15 from Kylan Thomas. Cade Hinkle scored 12. Deladris Green had seven points and 14 rebounds before fouling out.
The Redskins are 11-2 and the Eagles are 11-2. The Redskins bring the 2-1 WAC record back to conference play at Great Bend Friday night at about 7:45 on 1270 and kscbnews.net. The Eagles have a GWAC showdown with Holcomb Tuesday night in Hugoton.


text:
logo_moneymuseum
Speaking coins
Picture Tours of coins
Publications on the history of money
Bisopric of Lausanne, Aimon de Cossonay, Denier
The denier was the succession coin of the denarius that Charlemagne had introduced as standard coin of his empire toward the end of the 8th century. Since then, 240 Carolingian denarii were struck from one pound of silver (of about 408 grams). In German lands, the denarius developed into the pfennig, while in France it was called denier, and in Italy denaro.
The territories of modern Switzerland belonged to the realm of Charlemagne too. The little town of Lausanne, where this denier was struck, already had a mint at that time. Some 550 years after the coinage reform of Charlemagne, Lausanne still minted deniers geared to the Carolingian example. The issuer of this piece was Bishop Aimon de Cossonay, who presided over the Bishopric of Lausanne from 1355 (until 1375). The obverse depicts a church with five pillars, the reverse a cross.
Era/Origin/Country
Europe, Switzerland
ca. 1370 n. Chr.


Gary Groeneveld loves to be outdoors photographing sports, landscapes and wildlife with his DSLR and variety of lenses. For him it is a great way to get away from the stress of the city and observe nature in its true form. As a teacher with CBE for over 36 years, he continues to hold photography classes on variety of subjects. He is a graduate of Michigan State with two BSc. Degrees and two Journeyman Certificates.


THE BAY The Series Press: SOAPS.COM: Ex-General Hospital's John Reilly Joins The Bay.
SOAPS.COM: Ex-General Hospital's John Reilly Joins The Bay.
Sean Donely's friends could probably use him right now in Port Charles, but, for now, his portrayer John Reilly is joining the webseries "The Bay." Per Soaps In Depth, Reilly will play the Garret family butler who serves as their voice of reason.
I was hoping to see him at the GH reunion.