Watch the March 31, 2017 segment HERE and the June 23, 2016 segment HERE!
GOOD DAY PA hosted by Amy Kehm is an ABC27 daily lifestyle program bringing their viewers the latest news and happenings of many PA area non-profit organizations, local businesses, authors, chefs, events and much more. The show airs daily on ABC27 starting at 12:30 PM.
Bridge of Hope Harrisburg Area is grateful to the Joy Daniel's Real Estate Group for their kind generosity to the families we serve through the House A Family program and holiday giving. The ownership and staff at Joy Daniel's Real Estate Group have shown generosity and care for the needs of our families and we are grateful for their support!
Tom has played a crucial role as Consultant for Bridge of Hope Harrisburg Area using his expertise to assist the organization in enhancing culture, developing benchmarking tools for accountability and succession in all levels of organizational leadership from the Board of Directors to staff.
Recruit 1,000 women to join the Dream Team by each making a gift of $1,000 which will be used to create a lasting endowment of $1 million to support women and girls now, and far into the future.
Bridge of Hope Harrisburg Area gratefully acknowledges The Foundation For Enhancing Communities, in particular, The Women's Fund grant awarded in 2015 in the amount of $1,250, in 2016 in the amount of $1,500 and in 2018 in the amount of $3,000 for rental assistance.
We gratefully acknowledge the Greater Harrisburg Foundation for the grant awarded through the "Our Challenge For Giving" opportunity in the amount of $7,500 as well as the Upstream grant awarded in the amount of $10,000. We are honored to receive these funds.
We thank The Foundations for Enhancing Communities and the Martin M. Sacks Memorial Fund for their contributions to the Bridge of Hope Harrisburg Area House A Family Program. The fund contributed $1000 in 2015, $500 in 2016 and $500 in 2018.
Bridge of Hope Harrisburg Area is grateful for the support of Justin McClure with Daflure Heating, Cooling & Solar. Justin has been a faithful & active member of the Board of Directors and was part of the team to approve the launch of the House A Family program. Justin, his family and Daflure Heating, Cooling & Solar are faithful supporters of Bridge of Hope Harrisburg Area and the House A Family program.


text:
Камерун в настоящее время разделён на 10 регионов (). Регионы образуют территории 58 департаментов (). Департаменты делятся на 327 коммун ().

Регионы

Департаменты

Коммуны

Списки:Камерун

redpajama_set_name: RedPajamaWikipedia


text:
Q: Is it true that mocks also fail or are unable to do TDD tests with database? In theory, it is difficult to perform tests on functional code bases that need interactions with database, but I think we can use mocks. In real life applications, do you have failed cases when applying mocks to perform TDD tests with databases ? Could you shared some thoughts to explain this to me?

A: In tdd i use mocks to replace the physical database access with a fake (mock).
For databaseaccess i am always using a The Repository Pattern as api which can be easily mocked.
To Answer your question:
> do you have failed cases when applying mocks
> to perform TDD tests with databases ?

No as long all database-operations are encapsulated in the repository.

redpajama_set_name: RedPajamaStackExchange


mining lease of m/s dev raj stone crusher, for collection of sand . M/s Dev Raj Stone Crusher intends to mine Sand, Stone and Bajri from lease area .
Leasing Stone Crusher 60 Ton Mack Trucks The Mack® Pinnacle™ represents the best in highway truck engineering. The Pinnacle delivers outstanding fuel efficiency, productivity, durability and reliability.
mining lease of m/s dev raj stone crusher, for collection of sand granted mining lease for mining sand, stone and bajri vide letter Nos.. M/s Dev Raj Stone Crusher intends to mine Sand, Stone and Bajri from lease area.
Leasing Stone Crusher Jakarta Acceptable Words to Query by on Twitter Plotter A List of Currently Acceptable Words to Query By: the. i. for. been. brown. fragrance. wind: peppermint. reed. badd. immune. pai. senators. classified. as needed.


Keeping up with bitcoin news and getting hungry to claim your own stake in bitcoins? If you have researched cryptocurrency and how bitcoins are acquired, you realize that this is no easy task.
There's more attention on Bitcoin mining than ever before.
Cryptocurrency mining generates new bitcoins via solving a series of complex mathematical equations which requires a considerable amount of computing power. Since the birth of Bitcoin in 2009, mining has been the only way for people to make new coins. In spite of the increased interest in Bitcoin mining, it doesn't make it easier to acquire… or has it?
One company wants to make Bitcoin mining more accessible for more people.
The Next Web talks about how Bitcoin's price exploded in 2017 and topped $20,000. While the pricing is still very volatile, the interest in this cryptocurrency and the act of claiming it has not subsided one bit. Oasis Mining is a company which has created a way for people to get on board with the bitcoin mining mania in a more affordable way. They make this possible through the pooling of different hardware resources which allows users to mine and generate new bitcoin to include its competitor cryptocurrencies such as Ethereum and Bitcoin Cash.
How much power does cryptocurrency mining use up?
Recent studies have shown that the global network of bitcoin miners consume 30.14 terrawatt hours of electricity each year. To put that into perspective, this is more power than countries like Ireland would use in an entire year. Every single bitcoin transaction consumes around 300KWh of power. Environmental impact concerns and sustainability questions aside, this is a resource hungry venture. It is indeed a race to mine these bitcoins as there are about 21 million bitcoins in existence, which makes companies like Oasis Mining such an attractive option.
What is the real cost of cryptocurrency mining?
To understand why this act is so far out of reach of every day people, just look at China's Bitmain, a massive bitcoin mining operation, which runs a sprawl of mining farms in warehouses. Even if you were to try to set something up in the basement of your home, mining takes very specific chips and computer rigs. Specific graphic cards are necessary to meet the demands of the miners and have pushed companies like AMD and Nvidia to ramp up their production of their GPUs.
Larger companies see the interest from a variety of people wanting to get into Bitcoin mining as well.
The solution is pooled mining. One form of pooled mining is cloud mining where companies rent out their capabilities via the cloud to other companies or individuals. Pooled mining, which is what Oasis Mining does, is a way for individuals to become a part of the cryptocurrency mining race now with less costs. The appeal for users is that less overhead means potentially bigger profits from your mining efforts.
On 1 April 2018, Oasis Mining will have a Bitcoin mining marathon where users can participate in a campaign of cryptocurrency mining.
The users will be allotted a certain amount of time to mine and they will earn coins daily dependent on the hash rate that they use. Cryptocurrencies can also be traded on Oasis Mining in return for enhanced mining capabilities. Oasis Mining provides each user with a dashboard to track the amount of bitcoin or ether they have mined.
The possibilities for Bitcoin mining are limitless.
There are exchanges which charge fees on transactions. These fees vary based on the transaction type and the location or bank of the user. Oasis Mining claims that using its mining pool is more cost effective since there aren't the same transaction fees associated.
The user must decide what to do with their cryptocurrency. It can be used for personal purchases and payments, which was Bitcoin's original intended use. Or the bitcoins can be reused in the mining process to mine for more bitcoins. It can also be held in hopes of bitcoin's value soaring again like it did in 2017. Regardless of what a users choose to do with their keep, there are more readily available ways to mine for this finite resource and play a key role in this mining gold rush race.
Next articleWhat Can a Blockchain do?


text:
Q: Video camera crashes after latest(4.4.2) Samsung/OS update I am using custom camera in my application this works fine in jelly bean. Now after this Samsung Galaxy Tab OS update the custom camera is broken. I got this report from one of my friend i didn't saw that tablet. And i got crash report form Carshylytics.
My log report:
java.lang.RuntimeException: Unable to instantiate activity ComponentInfo{com.x.y/com.x.y.tools.EnregistrementVideoStackActivity}: java.lang.RuntimeException: Unable to initialize media recorder
       at android.app.ActivityThread.performLaunchActivity(ActivityThread.java:2053)
       at android.app.ActivityThread.handleLaunchActivity(ActivityThread.java:2154)
       at android.app.ActivityThread.access$700(ActivityThread.java:146)
       at android.app.ActivityThread$H.handleMessage(ActivityThread.java:1260)
       at android.os.Handler.dispatchMessage(Handler.java:99)
       at android.os.Looper.loop(Looper.java:137)
       at android.app.ActivityThread.main(ActivityThread.java:4949)
       at java.lang.reflect.Method.invokeNative(Method.java)
       at java.lang.reflect.Method.invoke(Method.java:511)
       at com.android.internal.os.ZygoteInit$MethodAndArgsCaller.run(ZygoteInit.java:1043)
       at com.android.internal.os.ZygoteInit.main(ZygoteInit.java:810)
       at dalvik.system.NativeStart.main(NativeStart.java)
Caused by: java.lang.RuntimeException: Unable to initialize media recorder
       at android.media.MediaRecorder.native_setup(MediaRecorder.java)
       at android.media.MediaRecorder.<init>(MediaRecorder.java:121)
       at com.x.y.tools.EnregistrementVideoStackActivity.<init>(EnregistrementVideoStackActivity.java:38)
       at java.lang.Class.newInstanceImpl(Class.java)
       at java.lang.Class.newInstance(Class.java:1319)
       at android.app.Instrumentation.newActivity(Instrumentation.java:1068)
       at android.app.ActivityThread.performLaunchActivity(ActivityThread.java:2044)
       at android.app.ActivityThread.handleLaunchActivity(ActivityThread.java:2154)
       at android.app.ActivityThread.access$700(ActivityThread.java:146)
       at android.app.ActivityThread$H.handleMessage(ActivityThread.java:1260)
       at android.os.Handler.dispatchMessage(Handler.java:99)
       at android.os.Looper.loop(Looper.java:137)
       at android.app.ActivityThread.main(ActivityThread.java:4949)
       at java.lang.reflect.Method.invokeNative(Method.java)
       at java.lang.reflect.Method.invoke(Method.java:511)
       at com.android.internal.os.ZygoteInit$MethodAndArgsCaller.run(ZygoteInit.java:1043)
       at com.android.internal.os.ZygoteInit.main(ZygoteInit.java:810)
       at dalvik.system.NativeStart.main(NativeStart.java)

And this error line is
public MediaRecorder mrec = new MediaRecorder();

Why it is happen have any idea? How can i solve this issue. I hope the camera code is not needed. But anyone want to see the code i can post here.
EDIT:
My EnregistrementVideoStackActivity class:
 public class EnregistrementVideoStackActivity extends Activity implements
        SurfaceHolder.Callback {
    private SurfaceHolder surfaceHolder;
    private SurfaceView surfaceView;
    public MediaRecorder mrec = new MediaRecorder();
    private Button startRecording = null;
    private Button stopRecording = null;
    File video;
    private Camera mCamera;
    private String output_path;

    boolean isActivityRestarting = false;

    Chronometer myChronometer;
    Boolean recording = false;

    public boolean onKeyDown(int keyCode, KeyEvent event) {
        if (keyCode == KeyEvent.KEYCODE_BACK) {
            if (recording == false) {
                finish();
            } else {
                stopRecording();
            }
            return true;
        }
        return super.onKeyDown(keyCode, event);
    }

    @Override
    protected void onDestroy() {
        super.onDestroy();
    }

    @Override
    public void onRestart() {
        super.onRestart();
        isActivityRestarting = true;
        finish();
    }

    @Override
    public void onCreate(Bundle savedInstanceState) {
        if (isActivityRestarting) {
            return;
        }

        super.onCreate(savedInstanceState);
        this.requestWindowFeature(Window.FEATURE_NO_TITLE);

        getWindow().setFlags(WindowManager.LayoutParams.FLAG_FULLSCREEN,
                WindowManager.LayoutParams.FLAG_FULLSCREEN);
        /*getWindow().setFlags(WindowManager.LayoutParams.FLAG_KEEP_SCREEN_ON,
                WindowManager.LayoutParams.FLAG_KEEP_SCREEN_ON);*/

        setContentView(R.layout.camera_surface);
        Intent intent = getIntent();

        output_path = intent.getStringExtra("path");

        startRecording = (Button) findViewById(R.id.buttonstart);
        stopRecording = (Button) findViewById(R.id.buttonstop);
        try {
            // This case can actually happen if the user opens and closes the
            // camera too frequently.
            // The problem is that we cannot really prevent this from happening
            // as the user can easily
            // get into a chain of activites and tries to escape using the back
            // button.
            // The most sensible solution would be to quit the entire EPostcard
            // flow once the picture is sent.
            mCamera = Camera.open();
        } catch (Exception e) {
            Toast.makeText(getApplicationContext(),
                    "Please restart device, camera error", Toast.LENGTH_LONG)
                    .show();
            finish();
            return;
        }
        surfaceView = (SurfaceView) findViewById(R.id.surface_camera);
        surfaceHolder = surfaceView.getHolder();
        surfaceHolder.addCallback(this);
        surfaceHolder.setType(SurfaceHolder.SURFACE_TYPE_PUSH_BUFFERS);
        myChronometer = (Chronometer) findViewById(R.id.chronometer1);

        startRecording.setOnClickListener(new OnClickListener() {

            public void onClick(View arg0) {
                try {
                    startRecording();
                    myChronometer.setBase(SystemClock.elapsedRealtime());
                    myChronometer.start();

                    startRecording.setClickable(false);
                } catch (Exception e) {
                    e.getMessage();
                    e.printStackTrace();
                    mrec.release();
                }

            }
        });
        stopRecording.setOnClickListener(new OnClickListener() {

            public void onClick(View arg0) {
                try {
                    stopRecording();
                    myChronometer.stop();
                    Intent intent = getIntent();
                    intent.putExtra("gallery", "viewed");
                    setResult(RESULT_OK, intent);
                } catch (Exception e) {
                    e.getMessage();
                }

            }
        });

        myChronometer
                .setOnChronometerTickListener(new Chronometer.OnChronometerTickListener() {

                    public void onChronometerTick(Chronometer chronometer) {
                        long myElapsedMillis = SystemClock.elapsedRealtime()
                                - myChronometer.getBase();
                        if (myElapsedMillis >= 120000) {
                            Toast.makeText(getApplicationContext(),
                                    "Maximum Video limit reached",
                                    Toast.LENGTH_LONG).show();
                            stopRecording();
                        }
                    }
                });
    }

    @Override
    public boolean onCreateOptionsMenu(Menu menu) {
        menu.add(0, 0, 0, "StartRecording");
        menu.add(0, 1, 0, "StopRecording");
        return super.onCreateOptionsMenu(menu);
    }

    @Override
    public boolean onOptionsItemSelected(MenuItem item) {
        switch (item.getItemId()) {
        case 0:
            try {
                startRecording();
            } catch (Exception e) {
                String message = e.getMessage();
                Log.e(null, "Problem Start" + message);
                mrec.release();
            }
            break;

        case 1: // GoToAllNotes
            mrec.stop();
            mrec.release();
            mrec = null;
            break;

        default:
            break;
        }
        return super.onOptionsItemSelected(item);
    }

    protected void startRecording() throws IOException {
        recording = true;
        mrec = new MediaRecorder(); // Works well
        mCamera.unlock();
        mrec.setCamera(mCamera);
        mrec.setVideoSource(MediaRecorder.VideoSource.CAMERA);
        mrec.setAudioSource(MediaRecorder.AudioSource.MIC);

        mrec.setOutputFormat(MediaRecorder.OutputFormat.MPEG_4);

        mrec.setVideoEncoder(MediaRecorder.VideoEncoder.H264);
        mrec.setAudioEncoder(MediaRecorder.AudioEncoder.AAC);
        int width = 320;
        int height = 240;
        try {
            // Check what resolutions are supported by your camera
            List<Size> sizes = params.getSupportedPictureSizes();

            for (Size size : sizes) {

                Log.e("TAG", "Available resolution: " + size.width + " "
                        + size.height);
                width = size.width;
                height = size.height;
            }
        } catch (Exception e) {
            e.printStackTrace();
        }

        mrec.setVideoFrameRate(30);
        mrec.setVideoSize(width, height);
        mrec.setVideoEncodingBitRate(1700000);
        mrec.setPreviewDisplay(surfaceHolder.getSurface());
        mrec.setOutputFile(output_path);
        mrec.prepare();
        mrec.start();
    }

    protected void stopRecording() {
        try {
            Log.e("stop recording", "Stop recording");
            recording = false;
            mrec.stop();
            mrec.release();
            mCamera.release();
            // go out

            Toast.makeText(getApplicationContext(),
                    "New Video Observation Saved", Toast.LENGTH_LONG).show();
        } catch (Exception npe) {
            npe.printStackTrace();
        }
        Intent intent = getIntent();
        setResult(RESULT_OK, intent);
        finish();

    }

    public void surfaceChanged(SurfaceHolder holder, int format, int width,
            int height) {
        //
    }

    Parameters params;

    public void surfaceCreated(SurfaceHolder holder) {
        if (!isActivityRestarting) {
            if (mCamera != null) {
                params = mCamera.getParameters();
                mCamera.setParameters(params);
            } else {
                Toast.makeText(getApplicationContext(),
                        "Camera not available!", Toast.LENGTH_LONG).show();
                finish();
            }
        }
    }

    public void surfaceDestroyed(SurfaceHolder holder) {
        try {
            if (mCamera != null) {
                mCamera.stopPreview();
                mCamera.release();
                mCamera.setPreviewCallback(null);
                mCamera = null;
            }
        } catch (Exception e) {
            e.printStackTrace();
        }
    }

    @Override
    protected void onPause() {
        super.onPause();

        if (recording == false) {
            finish();
        } else {
            stopRecording();
        }
    }
}

A: I got the error Because of Video sizes are not set. I solve this
int width = 320;
            int height = 240;
            try {
                //get the available sizes of the video
                List<Size> tmpList = getSupportedVideoSizes();

                final List<Size> sizeList = new Vector<Size>();

                // compare the apsect ratio of the candidate sizes against the
                // real ratio
                Double aspectRatio = (Double.valueOf(getWindowManager()
                        .getDefaultDisplay().getHeight()) / getWindowManager()
                        .getDefaultDisplay().getWidth());
                for (int i = tmpList.size() - 1; i > 0; i--) {
                    Double tmpRatio = Double.valueOf(tmpList.get(i).height)
                            / tmpList.get(i).width;

                    if (Math.abs(aspectRatio - tmpRatio) < .15) {
                        width = tmpList.get(i).width;
                        height = tmpList.get(i).height;
                        sizeList.add(tmpList.get(i));
                    }
                }
                if (EnableLog.LOG_TAG) {
                    Log.e("tmpList", tmpList + "*");
                }
            } catch (Exception e) {
                e.printStackTrace();
            }

mrec.setVideoSize(width, height);

public List<Size> getSupportedVideoSizes() {
        if (params.getSupportedVideoSizes() != null) {
            return params.getSupportedVideoSizes();
        } else {
            // Video sizes may be null, which indicates that all the supported
            // preview sizes are supported for video recording.
            return params.getSupportedPreviewSizes();
        }
    }


text:
South Dakota homeowners might soon face glut
by: Bob Mercer
Posted: Oct 29, 2019 / 08:12 PM CDT / Updated: Oct 29, 2019 / 08:12 PM CDT
PIERRE, S.D. (KELO) — Population changes in South Dakota during the next 10 years point toward more retirees looking to sell their homes but fewer younger people being able to buy them.
The director for the Black Hills Knowledge Network delivered that sobering message Tuesday at the South Dakota Housing Conference.
Jared McEntaffer has looked at trends and sees imbalance. People reaching retirement age will nearly double by 2030, he said, while adults younger than 65 will grow only six to nine percent.
At the same time, young people's pay levels during the past decade haven't kept up with their growing college debts, according to McEntaffer. He said they're tending to live alone or with roommates longer than before, and they're more likely to be in apartments rather than houses.
There's already a softening Midwest housing market.
"What we're seeing is the demand pulling back. And that's the big component, that's why nationwide, we're seeing home prices falling even though the interest rates are falling. And that's caused by buyers pulling back. That's caused by people being less confident in the future of the economy and sort of delaying those purchasing decisions," he said.
McEntaffer said trade uncertainty and weather have hurt South Dakota's economy. He said there's also a lot of political "angst" at the national level.
The South Dakota Housing Development Authority is hosting the annual conference through Wednesday. Executive director Mark Lauseng welcomed several hundred people and introduced Stockton Williams, who leads the National Council of State Housing Agencies.
"We'll probably produce as a country eight-hundred, nine-hundred-thousand new for-sale homes this year. That's still going to be several hundred thousand short of demand, and that's continuing a trend that's been playing out since the worst of the crash," Williams said.
The U.S. housing bubble that blew up in about 2006 led to more caution and the nation is now short about two million for-sale homes and one million to four million rental units, according to Williams.
He described the federal low-income tax credit as the most important and effective means for developers to produce affordable rental apartments. He said secondary lenders Fannie Mae and Freddie Mac came under federal-government control during the Great Recession but are now profitable again.
The federal tax cuts Congress passed in 2017 included provisions for housing opportunity zones that call for fewer capital-gains taxes to be paid if the money is re-invested in designated areas. But many members of Congress tend to still be focused on what happened a decade ago, according to Williams. He described it as fighting the last war.
"We don't necessarily want to forget those lessons, but we don't want to over-learn from them either. And sometimes I think policymakers from both parties are slower than those of you who are actually doing this everyday, to recognize that circumstances have changed. Companies and individuals have learned lessons from what not to do and now there really needs to be a commitment to sustainable home ownership," Williams said.
Meanwhile, in the nation's Capitol Tuesday, Republican U.S. Senator Mike Rounds of South Dakota introduced legislation with Democratic U.S. Senator Tina Smith of Minnesota to improve lending services at the federal Department of Housing and Urban Development for Native Americans.
Rounds said the department's loan-guarantee program since 1992 helped "countless" native peoples "realize their dreams of homeownership" He said the bill would remove regulatory hurdles that can delay loan processing.
More Capitol News Bureau Stories
After private meeting on choosing director, S.D. Legislature's Executive Board will meet again
by Bob Mercer / Jan 20, 2020
PIERRE, S.D. (KELO) -- The South Dakota Legislature's Executive Board had a lengthy discussion Monday night at the Capitol, talking behind closed doors about the next steps for picking a director.
After 75 minutes, lawmakers reopened the meeting and Senator Brock Greenfield said they would need to gather again because some things needed further discussion.
S.D. courthouses' employees could get concealed-carry too
PIERRE, S.D. (KELO) -- County employees might be next to get to carry handguns hidden from others in South Dakota courthouses.
Senator Lance Russell, a Hot Springs Republican, introduced SB 51. His lead House co-sponsor is Representative Tim Goodwin, a Rapid City Republican.
by Michael Geheren / Jan 20, 2020
PIERRE, S.D. (KELO) -- The South Dakota legislature has been in session for less than a week, but already has filed 121 bills.
KELOLAND News has a team of journalists tracking bills in the legislature, led by Capitol News Bureau Correspondent Bob Mercer.
Tweets by pierremercer

redpajama_set_name: RedPajamaCommonCrawl


My dream today is a little different.
I'm at this house with a man who married a witch that spreads diseases. They have a daughter, who is the sole reason I go house visit.
The dad is constantly laboring hard, fixing the house, attending to the sick animals, taking care of the wife and daughter. And he has no idea why the animals kept falling sick. The mum is normally in lumbur. The time when she's awake and walking about is when everything she touches fell ill. Strangely, I noted that her husband and daughter never gotten ill.
I have the fortune (or misfortune) to witness her being awake. She walks about in a daze, touching this and that, and of course one by one their conditions worsen. I realise that she didn't realize that she is the disease queen, and thought she is spreading love instead. My last memory of her is when she walks into a shed out at the garden, with the horses and cows braying pitifully at the background.


text:
Employers' Organizations
In Lebanon
Gender equality and non-discrimination
International Labour Standards
Workers' Organizations
Decent work in Arab States
Statements and speeches
Comment and Analysis
Factsheets and briefs
ILO Project Office for the State of Qatar
Study identifies effective mitigation strategies to keep workers safe from ...
Study identifies effective mitigation strategies to keep workers safe from heat stress
Largest ever study on the impact of heat stress reveals effectiveness of a number of existing approaches, and makes recommendations to better protect workers during summer months
Press release | 11 October 2019
DOHA (ILO News) – Outdoor workers in Qatar are able to perform their roles safely, despite the summer heat and humidity, if effective precautionary measures are in place. This is the key finding from a study commissioned by the International Labour Organization (ILO) and the Ministry of Administrative Development, Labour and Social Affairs, in collaboration with the Supreme Committee for Delivery & Legacy (SC).
Throughout the summer, the FAME Lab from the University of Thessaly, a leading institution in this field, collected data on workers' physiology and labour effort, covering more than 5,500 work hours. This is the largest ever study of its kind and the first in the region. The research examined a construction site with 4,000 workers (a World Cup stadium) with a comprehensive heat stress management plan, and a farm with fewer precautions in place. The research examined different strategies for mitigating heat strain, focusing on hydration, work-rest ratios and clothing.
The research found the amount of time that workers' core body temperature exceeded the safety threshold of 38 °C (proposed by the World Health Organization) was low. On the construction site, this averaged zero to three per cent of the workers' shift and on the farm eight per cent.
"One of the key reasons why workers on the World Cup site were at low risk to occupational heat strain, was because they were empowered to self-pace and take breaks," said Dr. Andreas Flouris, head of the FAME Laboratory. "This was a key element of the heat mitigation plan, and was how workers were able to cope with the heat and humidity."
Workers' labour effort was recorded on a second-by-second basis, and the labour intensity was low. On the World Cup site, workers were on breaks for 62 per cent of their work shift, and 32 per cent of their work was carried out at low intensity (0.1 to 1.4 W / m2). The farm workers were on breaks for 23 per cent of their shift, and carried out 67 per cent of their shift at low intensity.
The study found that many workers were dehydrated at the start of their shifts, underscoring the importance of effective hydration strategies. The research also tested different clothing options, including the dark-coloured overalls that are typically worn by construction workers, against white overalls, a cooling suit developed by the SC, and a cooling vest with embedded solar-powered fans. The study found that the SC suit and the white overalls can effectively reduce the heat strain experienced by workers.
Recommendations made by the study include adjusting the summertime working hours, mandatory heat stress mitigation plans for all companies across Qatar, annual health checkups for workers, as well as greater worker empowerment. There are also specific recommendations on clothing, access to drinking water and working in shaded areas.
"We are working with the Government to translate the recommendations of this study into improved legislation, and to promote the replication of the good practices that were identified," said Houtan Homayounpour, Head of the ILO Project Office in Doha. "We have a scientific basis on which to propose adjustments to the prohibited working hours during summer, and it is clear that heat stress mitigation plans must recognize the right and enhance the ability of workers to self-pace."
At the beginning of summer 2019, the Labour Inspection Department disseminated heat stress guidance for employers and workers, which had substantial reach on social media. Labour inspectors also shut down 310 work sites for violating the regulation on prohibited working hours between 15 June and 31 August.
The FAME Lab is part of the University of Thessaly's School of Exercise Science. Dr Andreas Flouris is the head of the Lab. He has been a member of Working Groups providing input for guidelines and policy pertaining to the health effects of different environmental factors for many international organizations (World Health Organisation, United Nations, European Commission, NASA, and others). He is an author of the global recommendations for work in hot environments to be jointly published in 2020 by the World Health Organization and the World Meteorological Association.
For more information, please contact Steve Needham, Communications Officer, ILO Project Office for the State of Qatar at Mob +97450069011 or at needham@ilo.org
Tags: employment, migrant workers, labour law, technical cooperation, workers rights, occupational safety and health
Regions and countries covered: Qatar
Assessment of occupational heat strain and mitigation strategies in Qatar [pdf 6553KB]
Home page of ILO in Qatar


text:
Drosera aberrans är en sileshårsväxtart som först beskrevs av Allen Lowrie och Sherwin Carlquist, och fick sitt nu gällande namn av Allen Lowrie och John Godfrey Conran. Drosera aberrans ingår i släktet sileshår, och familjen sileshårsväxter. Inga underarter finns listade i Catalogue of Life.

Bildgalleri

Källor

Externa länkar

Sileshår
aberrans


text:
\section{Introduction}
\label{sect_intro}

The Large Area Telescope (LAT) on board the \emph{Fermi $\gamma$-ray Space Telescope} (\emph{Fermi}: \citealt{atwood09}) has increased the number of observed solar flares with photon emission above 100 MeV by an order of magnitude compared to all previous instruments \citep{share17}. One prominent characteristic of these flares is the long-duration emission extending hours past the impulsive phase, long after other flare associated electromagnetic emissions at longer wavelengths have decayed (e.g., \citealt{ajello14}). High-energy $\gamma$-rays can be produced by electrons and ions (primarily protons), with somewhat larger energies than the photons, via relativistic electron bremsstrahlung or decay of pions (and their byproducts) produced by interactions of protons with the background ions. Both mechanisms require transport of the accelerated particles deep into the high-density solar photosphere (where the particles lose most of their energy) and  through column depths of about $2.5\times 10^{25}$ and $2.5\times 10^{26}$~cm$^{-2}$, respectively. Thus, the accelerated particles, wherever produced, must travel to the photosphere to produce the observed $\gamma$-rays. This transport is guided by the magnetic field lines connecting the acceleration site to the photosphere.

The impulsive phase (duration of $< 10^3$ s) radiations (from microwaves to GeV $\gamma$-rays) are produced by the interactions of the nonthermal electrons and protons with the flaring loop magnetic field and plasma (mainly at the loop footpoints). In a vast majority of flares, the impulsive emission is dominated by nonthermal electrons, rather than protons \citep{shih09}, in which particles are generally believed to be accelerated near the loop-top region (heights $> 10 ^9$ cm; e.g., \citealt{petrosian02, liu13}). This acceleration mechanism may be at work for some of the long-duration $\gamma$-ray flares observed by {\it Fermi}\  (e.g., \citealt{ajello14}). Examples include the 2011 March 7\,--\,8 \citep{ackermann14} and the 2017 September 10 \citep{omodei18} flares, during which the centroid of the $\gamma$-ray source coincided well with the active region (AR) where the flare was initiated. This is also the case for the initial phase of the stronger 2012 March 7 flare, which lasted for about 20 hours, later with a temporal drift of the centroid away from the AR \citep{ajello14}. In these events, the bulk of the hard X-rays (HXRs) and $\gamma$-rays may be explained in terms of thick-target emission from the footpoints of the flaring loops.

However, {\it Fermi}\  also detected $>$100~MeV photons from three other flares which, according to observations by the \emph{Solar TErrestrial RElations Observatory} (\emph{STEREO}), originated from ARs that were located 13$\arcdeg$\,--\,36$\arcdeg$ behind the solar limb seen from the Earth perspective \citep{pesce15, ackermann17}. These flares were also detected in HXRs by the \emph{Reuven Ramaty High Energy Solar Spectroscopic Imager}  (\emph{RHESSI}), \emph{Fermi}/Gamma-ray Burst Monitor (GBM), and \emph{Wind}/Konus with similar time profiles, in extreme ultraviolet (EUV) by \emph{Solar Dynamics Observatory} (\emph{SDO}) and \emph{STEREO}, and in microwave by the Radio Solar Telescope Network (RSTN). In addition, \emph{RHESSI} detected HXR emission located just over the limb which is consistent with the top of the (relatively tall) flaring loop rooted at the source AR behind the solar limb. \emph{An important question is whether or not the LAT $\gamma$-rays are coming from this loop-top source as well}. As described below, the LAT observations and some theoretical arguments lead us to consider a different location on the Sun for the $>$$100$~MeV $\gamma$-ray source and perhaps a different site and mechanism for acceleration of particles (either electrons or protons). This would be an important step toward resolving the puzzle of {\it Fermi}\  BTL flares and understanding $\gamma$-ray flares in general.

\citet{cliver93} first proposed that the BTL $\gamma$-ray events are caused by particles that are accelerated at the shock driven by the associated coronal mass ejection (CME) and then propagate back to the visible solar disk. The goal of this study is to explore this scenario by investigating the magnetic connectivity and evolution of the CME-driven shock, and their relationship, in both space and time, with the observed $\gamma$-ray emission during a BTL flare. Specifically, we will evaluate to what extent the CME and CME-driven shock are magnetically connected to $\gamma$-ray emitting areas of the visible disk away from the AR, and track several key shock parameters over those magnetically-connected areas of the shock surface.\footnote{A corollary of this scenario is that we would expect a similar spread of $\gamma$-ray emission over the solar disk for on-disk flares as well. In fact, the new PASS-8 analysis of the X5.4 flare on 2012 March 7 shows hints of migration of the emission centroid moving away from its host AR over time (Allafort et al., in preparation), although in general it is harder to distinguish between a point source (which was assumed in locating the centroids) and an extended one due to the relative low number of photons detected by \emph{Fermi}.} To this end, we performed high-fidelity, data-driven magnetohydrodnamic (MHD) simulations to reconstruct the global corona and solar wind environment for the CME eruption associated with the strongest of the three BTL flares: {\it SOL2014-09-01}. We note the pioneering work by \citet{plotnikov17} toward this direction that used a potential magnetic field and a \emph{static} MHD global corona solution. We believe that the inclusion of the dynamic evolution of the CME, as done in the present study, is an important step forward and can shed critical new light on the underlying physics of BLT $\gamma$-ray flares.

This article is organized as follows. In Section~\ref{sect_obs}, we present a summary of relevant observations of this event and theoretical arguments. In Section~\ref{sect_modeling}, we describe our numerical model and present the simulation results with a focus on the magnetic field connectivity and shock evolution, followed by discussions in Section~\ref{sect_discuss} and summary and conclusion in Section~\ref{sect_summary}.

\section{Review of Observations and Theoretical Arguments: the {\it SOL2014-09-01} Flare \& CME Event}
\label{sect_obs}

Here we briefly review the observations of the \emph{SOL2014-09-01} (hereafter Sept14) flare relevant to this work (We refer the reader to \citealt{ackermann17} for more details). Specifically, we give two empirical reasons why we favor the CME-shock origin, rather than the direct flare acceleration, of the particles responsible for the $\gamma$-rays detected by the LAT in this flare.

The first reason is the difficulty of producing strong $\gamma$-rays in the tenuous solar corona. According to \emph{STEREO-B} data, this flare originated from what was named NOAA AR~12158 later. It was located at N14E126, about $36^{\circ}$ behind the east solar limb. \emph{RHESSI} images show a HXR source with a size of about 40$\arcsec$ ($\sim 30$ Mm) just over the limb, which is consistent with (a part of) the loop-top source of a relatively large flaring loop with a height of $\gtrsim$130~Mm above the photosphere. Similar examples have been reported \citep{krucker07}. Since all other $<$100~MeV emissions, as seen by \emph{Fermi}/GBM and \emph{Wind}/Konus, have light curves very similar to the \emph{RHESSI} HXRs, it is reasonable to assume that they also come from the top of the flare loop through thin-target bremsstrahlung emission \citep{chen13, petrosian16, effenberger17}. Since only a small fraction of the particle energy is lost during the {\it thin-target} bremsstrahlung, coronal HXR/$\gamma$-ray emission in general requires a higher number (and energy) of accelerated particles than if we are dealing with a {\it thick-target} footpoint emission, where particles lose all their energy \citep{petrosian73}, and where most of the HXRs and $\gamma$-rays \citep[e.g.,][]{hurford03,hurford06} in on-disk flares originate from. This difference would also be the case for either electrons or protons if the \emph{Fermi}/LAT $\gamma$-rays were also coming from the thin-target loop-top source. However, assuming thick-target emission by protons in the photosphere, one requires a total energy in protons comparable to that calculated for disk flares. Therefore, if the Sept14 \emph{Fermi}/LAT emission were from the loop-top source, it would require a much higher energy of the accelerated protons than any of the other (even stronger) \emph{Fermi}/LAT flares \citep{petrosian18}. This difficulty is the first reason for considering a different source and possibly a different acceleration mechanism for the production of the $\gamma$-rays.

The second and more important reason is that the centroid of the \emph{Fermi}/LAT source is about $300\arcsec (\sim 200$ Mm) northwest of the \emph{RHESSI} source and the corresponding light curve is different than that of all the other emissions. Specifically, the LAT light curve decays very gradually with emission detected for almost two hours, while all other emissions last less than one hour before falling below background. Although the possibility of LAT emission being also produced (in part) by particles accelerated near the loop-top source cannot be completely ruled out, the above two reasons lead to a more plausible scenario that this emission is produced at the photosphere by particles (most likely protons) accelerated at the CME-driven shock and escaping from the downstream back to the Sun \citep{cliver93}. In the case of BTL flares, unlike in on-disk flares, these particles must be streaming down to the photosphere along field lines connected to the LAT centroid region located on the visible disk, tens of degrees away from the host AR.

This scenario is further supported by the facts that the Sept14 flare is also associated with: (i) a fast CME observed by both \emph{SOHO}/LASCO and \emph{STEREO-B}/COR1 with a speed $>$1900~km~s$^{-1}$; (ii) a Type II radio burst with an estimated velocity of 2079 km s$^{-1}$ \citep{pesce15}, and (iii) an SEP event with a quick onset and hard spectrum observed by \emph{STEREO} \citep{cohen16, zelina17}. The CME white-light images and height-time history are shown in Figures~\ref{fig:wl} and \ref{fig:htplot}, respectively, and will be further discussed in \S 3.1.

\section{Modeling the {\it SOL2014-09-01} Event}
\label{sect_modeling}

\subsection{Global Coronal \& CME Models}
\label{subsect_model-descr}

To reconstruct the global corona and solar wind environment during the {\it SOL2014-09-01} CME eruption, we used the University of Michigan Alfv\'{e}n Wave Solar Model (AWSoM; \citealt{sokolov13, bart14}) within the Space Weather Modeling Framework (SWMF; \citealt{toth12}). AWSoM is a data-driven global MHD model with the inner boundary specified by observed magnetic maps and the simulation domain extending from the upper chromosphere to the corona and heliosphere. Physical processes implemented in the model include multi-species thermodynamics, electron heat conduction (both collisional and collisionless formulations), optically thin radiative cooling, and Alfv\'{e}n-wave turbulence that energizes the solar wind plasma. The Alfv\'{e}n-wave description is physically self-consistent, including non-Wentzel-Kramers-Brillouin (WKB) reflection \citep{heinemann80, velli93, hollweg07} and physics-based apportioning of turbulence dissipative heating to both electrons and protons. AWSoM has demonstrated its capability of reproducing solar corona condition with high-fidelity \citep[e.g.,][]{sokolov13, bart14, oran13, oran15, jin16, jin17a}.

Based on the steady-state global corona and solar wind solution, we initiate the CME by using an analytical Gibson-Low (GL) flux-rope model \citep{gibson98}, which has been successfully used in numerous modeling studies of CMEs (e.g., \citealt{chip04a, chip04b, lugaz05, chip14, jin16, jin17a}). The GL flux rope is mainly controlled by five parameters: the stretching parameter $a$ determines its shape, the distance $r_{1}$ of the flux rope center from the center of the Sun determines its initial position before being stretched, the radius $r_{0}$ of the flux-rope torus determines its size, $a_1$ determines its magnetic field strength, and a helicity parameter determines its positive (dextral) or negative (sinistral) helicity. Analytical profiles of the GL flux rope are obtained by finding a solution to the magnetohydrostatic equation $(\nabla\times{\bf B})\times{\bf B}-\nabla p-\rho {\bf g}=0$ and the solenoidal condition $\nabla\cdot{\bf B}=0$. This solution is derived by applying a mathematical stretching transformation $r\rightarrow r-a$ to an axisymmetric, spherical ball of twisted magnetic flux with radius $r_0$ centered in the heliospheric coordinate system at $r=r_1$. The transformed flux rope appears as a tear-drop shape. At the same time, Lorentz forces are introduced, which lead to a density-depleted cavity in the upper portion and a dense core at the lower portion of the flux rope, corresponding to a coronal cavity and a dense prominenence, respectively. This configuration can thus readily reproduce the typical three-part structure of an observed CME \citep{llling85}. The GL flux rope and contained plasma are then superposed onto the steady-state AWSoM solution of the solar corona: i.e. $\rho=\rho_{0}+\rho_{\rm GL}$, ${\bf B = B_{0}+B_{\rm GL}}$, $p=p_{0}+p_{\rm GL}$. The temperature will be updated from the new density $\rho$ and pressure $p$. The resulting combined background-flux rope system is in a state of force imbalance, due to the insufficient background plasma pressure to counter the magnetic pressure of the flux rope, and thus erupts immediately when the numerical model advances in time.

To specify the inner boundary condition of the magnetic field, we utilize a global magnetic map sampled from an evolving photospheric flux transport model \citep{schrijver03}, which assimilates new observations within 60$^{\circ}$ from disk center obtained by the \emph{SDO} Helioseismic and Magnetic Imager \citep[HMI;][]{schou12}. The assimilated magnetogram is updated every 6 hours. The Sept14 flare occurred behind the east limb where no direct observation of the magnetic field is available. This means that the magnetic field around the flare site at the time of the event contains the most aged observation obtained from about a half solar rotation earlier when the region was on the western side of the visible solar disk. Therefore, a large amount of magnetic flux could potentially be missing. From the magnetogram closer in time shown in Figure \ref{fig:magnetogram}a, we find that the flare source region AR~12158 is indeed completely missing. To alleviate this problem, we choose the assimilated magnetogram on 2014 September 8 00:04:00 UT (Figure  \ref{fig:magnetogram}b), about a week after the event on September 1, when the magnetic field around the source region was first assimilated into the flux transport model. The missing flare source region AR~12158 and another large AR~12157 to the south of it are now properly included. The rest of the old and new magnetic maps are qualitatively very similar. As such, the 2014 September 8 magnetogram is a reasonable representation of the photospheric magnetic field at the time of the Sept14 flare and is thus used to specify the inner boundary condition of our global magnetic field model.

To configure a proper GL flux rope for initiating the Sept14 CME, we utilize a newly developed tool called the Eruptive Event Generator using Gibson-Low configuration (EEGGL; \citealt{jin17b}), which is designed to determine the GL flux-rope, including its location, orientation, and five key controlling parameters, using the observed magnetogram and CME speed near the Sun. The left panel of Figure~\ref{fig:initiation}a shows a zoom-in view of AR 12158 with weighted centers of positive/negative polarities and the polarity inversion line (PIL) determined by EEGGL. The green asterisk marks the central location to insert the GL flux rope, whose calculated key parameters are also listed. The right panel shows the 3D configuration of the global coronal magnetic field, with the inserted GL flux rope shown in red. The white field lines represent the large-scale helmet streamer structures. The selected field lines from surrounding active regions and open field are marked in green. The GL flux rope erupts due to the force imbalance upon insertion into the active region. The simulation is then evolved forward in time and the MHD equations are solved in conservative forms to guarantee the energy conservation across the CME-driven shock \citep{bart10, chip12, jin13}. To better resolve the shock structure, two more levels of refinement along the CME path are performed, which make the cell size $\sim$0.02 R$_\odot$ at 2 R$_\odot$ and $\sim$0.06 R$_\odot$ at 5 R$_\odot$. We run the simulation for 1 hour after the initiation, until the CME reaches $\sim$10 R$_\odot$.

Since the CME propagation near the Sun is mainly observed by coronagraphs, we generate synthesized white-light images (Thomson-scattered white-light brightness) and compare them with observations. The top panel of Figure~\ref{fig:wl} shows the observations from \emph{SOHO}/LASCO C2 and \emph{STEREO-B}/COR1. The bottom panel shows the synthesized white-light images. The color scale shows the relative total brightness changes with respect to the pre-event level. At the time of the Sept14 event, \emph{STEREO-B} and \emph{SOHO} were separated by $\sim$161$^{\circ}$ therefore observing the Sun from nearly opposite directions. By comparing the observation and simulation from two different viewpoints, we find that the observed CME is adequately simulated in terms of the direction of propagation and the width. Note that the absolute brightness comparison between the observation and simulation requires advanced calibration of the observational data as well as the inclusion of the contribution from the F corona (light scattered by interplanetary dust) in the simulation data, which are beyond the scope of this study. The reader is referred to previous studies for such model validation \citep[e.g.,][]{chip08, jin17a}. Also, there is a distinct feature (marked in Figure~\ref{fig:wl}) around the CME leading edge in the LASCO C2 image, which might imply that the corresponding shock front can deviate from a typically circular or dome shape. We speculate that this feature might be related to the complex and dynamically changing
background solar wind environment (e.g., affected by previous CMEs or coronal disturbances), which is not captured by the current simulation. We further compare the observed and simulated CME speeds by tracking the height-time (HT) history of the CME leading edge, as shown in Figure~\ref{fig:htplot}. The black dots show measurements from \emph{SOHO}/LASCO C2/3 (left panel) and \emph{STEREO-B} COR1/2 (right panel), while the red asterisks show corresponding measurements from the synthesized white-light images. We use the moment when the observed and simulated CMEs are around the same height as a guidance to calibrate the start time of the simulation in terms of the real observation. With this assumption, the first appearance of CME in the LASCO C2 field of view (11:12:05 UT) corresponds to $t = 10$~minutes in the simulation. In general, the CME HT history is well reproduced in the simulation, with the simulated CME being slightly slower by about 10-14\%.

\subsection{Field Connectivity Evolution}
\label{subsect_connect}

In the course of the eruption, the flux rope interacts and reconnects with the magnetic fields of the source AR as well as the global coronal field. As a result, the magnetic field configuration and connectivity can change dramatically, which could significantly influence the transport of the accelerated particles. With this global MHD simulation of the Sept14 event, we now investigate the field connectivity evolution in detail during the first hour of CME evolution.

Figures~\ref{fig:3d_evo}a-d show the 3D magnetic field configurations at selected times (5, 10, 20, and 30 minutes). Magnetic reconnection between the erupting flux rope (red) and the surrounding field lines (green and white) is evident, especially after the first 10 minutes. The interaction between the flux rope and the large-scale helmet streamers significantly changes the global corona configuration around the CME source region. The helmet streamers are opened up by reconnection or stretched by the CME expansion. Specifically, we further examine the field line connectivity around the \emph{Fermi} $\gamma$-ray emission region at $t = 30$~minutes (shown in Figure~\ref{fig:3d_evo}e). The derived \emph{Fermi} $\gamma$-ray emission centroid and 68\% uncertainty circle (adapted from \citealt{ackermann17}) are overlaid on the simulation data. The green field lines are the pre-existing open field connected to the CME-driven shock after $t \sim 6$~minutes. The red field lines are the closed field connected to the flaring AR. These field lines were not present before, but started to develop $\sim$5~minutes after the eruption through magnetic reconnection between the flux-rope magnetic field and the global coronal field.

To investigate the details of these two types of field lines, we further mark their photospheric footpoints on the magnetic field map in the top panel of Figure \ref{fig:open_close}. The closed field line regions (red) are relatively compact, compared with the elongated open field line region (green) to the south. The bottom panel of Figure \ref{fig:open_close} shows the 3D configuration of these two types of field lines. As evident in this plot, the open field lines change directions abruptly due to the rapid expansion the CME and CME-driven shock. For the closed field lines, the configuration is more complex with twisted large-scale loops. It appears that some of these field lines result from reconnection between the erupting flux rope and the nearby helmet streamers.

\subsection{CME-driven Shock Evolution}
\label{subsect_shock}

After the eruption, the flux rope drives a shock in the corona that propagates freely into the heliosphere. CME-driven shocks are believed to be responsible for acceleration of particles through the diffusive shock acceleration (DSA) mechanism (e.g., \citealt{axford77}) that produces the so-called gradual solar energetic particle (SEP) events \citep{reames99}. Due to the nonuniform background environment, the CME-driven shock evolution is highly spatially dependent. For example, a shock that is propagating into the fast solar wind could acquire a higher shock speed therefore leading to a higher stand-off distance from the flux rope driver \citep{jin17a}. Also, the shock parameters could vary significantly over the shock front, which can significantly affect the acceleration process \citep{chip05, li12}. Based on the white-light observations from SOHO and STEREO, several methods have been developed to derive the shock parameters directly from the data (e.g., \citealt{rouillard16, lario17, kwon18}). In this study, with the data-driven MHD simulation of the Sept14 event, we can track the shock location and key parameters (e.g., the compression ratio, shock Alfv\'{e}n Mach number, shock speed, and shock obliquity angle $\theta_{Bn}$) during the CME evolution. The shock obliquity angle $\theta_{Bn}$ refers to the angle between the shock normal (see equation~[\ref{eq_shock}]) and the upstream magnetic field. As shown below, such analysis can provide a more comprehensive picture of the shock as to its configuration and properties over the area linking back to the visible side of the Sun, where LAT $\gamma$-rays were detected.

We first determine the shock location at each time step by using the proton temperature gradient criteria \citep{jin13}. At each shock location, the shock normal is determined by using the magnetic coplanarity ${\bf (B_{d}-B_{u})}\cdot {\bf n}=0$ \citep{abraham72, lepping71}:

\begin{equation}
{\bf n}=\pm\frac{({\bf B_{d}}\times{\bf B_{u}})\times({\bf B_{d}}-{\bf B_{u}})}{|({\bf B_{d}}\times{\bf B_{u}})\times({\bf B_{d}}-{\bf B_{u}})|}
\label{eq_shock}
\end{equation}
where $\bf B_{d}$ and $\bf B_{u}$ represent downstream and upstream magnetic field respectively. Note that this method fails for $\theta_{Bn} = 0^{\circ}$ or $90^{\circ}$, which we found to be very rare in the actual simulations. The $\pm$ sign is determined by assuming a forward moving shock in the heliocentric coordinate. We then determine the upstream/downstream plasma parameters, from which the shock parameters (e.g., the compression ratio, shock speed, shock Alfv\'{e}n Mach number, and shock obliquity angle) can be calculated accordingly.

Figure \ref{fig:shock_evo} shows the shock geometry evolution during the first hour of the simulation. The color scales on the shock surface represent the four shock parameters (from top to bottom): the compression ratio, shock speed, shock Alfv\'{e}n Mach number, and shock $\theta_{Bn}$. The yellow field lines represent the open field near the \emph{Fermi} emission region (shown in Figures \ref{fig:3d_evo} and \ref{fig:open_close}). Based on the simulation, we found that the CME-driven shock started to intersect the open field lines around $t = 6$~minutes, when the fastest part of the shock reached $\sim$3 R$_{\odot}$. This finding is consistent with the estimation of the CME located at $\sim$2.5 R$_{\odot}$ at the onset of the \emph{Fermi}-LAT emission \citep{ackermann17}. However, we should note that the part of the shock intersecting the open field is closer to the Sun at $\sim$1.6 R$_{\odot}$. At $t = 20$~minutes, the CME-driven shock covered the entire open-field region around $\sim$3 R$_{\odot}$ linking to the front side of the Sun. Furthermore, the derived $\theta_{Bn}$ suggests that this part of the shock is a quasi-perpendicular shock with a mean $\theta_{Bn}\sim73^{\circ}$. Another observational fact worth mentioning is the EUV wave observed in this event. The EUV wave from the source region arrived at the open field region (connecting to the CME-driven shock) by 11:20 UT as shown in online movies (http://aia.lmsal.com/AIA\_Waves), an extension of the \citet{nitta13} study. There is a possibility that this EUV wave may trace the low-corona flank of the shock, as see in several other eruptive events (e.g., \citealt{carley13}), including the recent X8.2 flare on 2017 September 10 \citep{gopal18a, liu18, morosan18}, which was the first (and the only one so far) long-duration \emph{Fermi} flare associated with a ground level enhancement event \citep{omodei18}.

At $t = 30$~minutes, the shock surface starts to deviate from its initial spherical shape due to the non-uniform background solar wind condition. In particular, one part of the shock (as marked by a white arrow in Figure \ref{fig:shock_evo}), with open field lines crossing it, propagates into a fast wind region originating from an on-disk coronal hole and acquires a higher speed. This process may also lead to a ``shock-shock" interaction at the boundary between the two shock surfaces that causes an elevated shock compression ratio and Alfv\'{e}n Mach number at $t = 60$~minutes (marked with a white circle in the upper-right panel of Figure \ref{fig:shock_evo}). Note that the open field lines connected to this shock interaction region are closer to the \emph{Fermi} $\gamma$-ray emission region. Since the compression ratio, shock Alfv\'{e}n Mach number, and shock geometry are key parameters for DSA of SEPs, this part of the shock can be favorable for accelerating particles to higher energies \citep{chip05, sokolov06, li12, zhao14, hu17, hu18}.

We obtain the shock parameters averaged over the portion of the shock surface that is connected back to the visible side of the Sun. The temporal evolution of the resulting four key shock parameters as well as the average upstream local plasma density is shown in Figure \ref{fig:shock_profile} and described as follows:

\begin{enumerate}

\item
The shock compression ratio (Figure \ref{fig:shock_profile}a) increases rapidly from $\sim$1.8 at $t \sim$10~minutes to $\sim$4.6 at $t \sim 20$~minutes\footnote{The maximum compression ratio is slightly larger than 4 (strong shock limit) due to the non-ideal processes (e.g., heat conduction, other compression effects) or merged background density gradient in the simulation.}, and then gradually decreases to $\sim$3.7 at $t = 60$~minutes. This evolution trend closely follows that of the \emph{Fermi}/LAT $\gamma$-ray flux profile (red curve), with a similar $\sim$10~minute duration of the rapid rise phase.

\item
The average local plasma density at the shock front (Figure \ref{fig:shock_profile}b) is another important parameter, which is related to the seed population and the number of particles available for shock acceleration. We also plot an empirical quantity $CR\cdot\rho^{1/3}$ (blue curve), a product of the shock compression ratio (CR) and the ambient density to a $1/3$ power (heuristically selected to match the temporal trend of the Fermi $\gamma$-ray flux). The density generally decreases with time as the CME travels away from the Sun, which causes this empirical quantity to decrease after its initial increase during the first ~20 minutes. This could potentially explain the simultaneous decrease in the Fermi $\gamma$-ray flux, even though the shock compression ratio and Mach number remain high.

\item
The shock speed (Figure \ref{fig:shock_profile}c) shows a gradual increase from $\sim$400~km~s$^{-1}$ at $t \sim$10~minutes to $\sim$1000~km~s$^{-1}$ at $t \sim$35~minutes and then remains roughly constant.

\item
Likewise, the shock Alfv\'{e}n Mach number (Figure \ref{fig:shock_profile}d) gradually increases from $\sim$1 to $\sim$3 during the $t \sim$10-35~minutes interval and then grows even more slowly to $\sim$4 at $t \sim$60~minutes.

\item
The shock obliquity angle analysis (Figure \ref{fig:shock_profile}e) shows that the shock is originally a quasi-perpendicular shock before $t \sim$30~minutes (with $\theta_{Bn} \sim 75 ^\circ$ at $t \sim$10~minutes) and evolves into a quasi-parallel shock (with $\theta_{Bn} \sim 30 ^\circ$ at $t = 60$~minutes). The most rapid decrease in $\theta_{Bn}$ occurs during $t \sim$22-35~minutes, the onset of which coincides with the peak time ($t=22$~minutes) of the compression ratio and \emph{Fermi} $\gamma$-ray flux shown in Figure \ref{fig:shock_profile}a. Note that the same trend of shock obliquity angle variation during CME evolution was also found by \citet{chip05}.

\end{enumerate}

\section{Discussions}
\label{sect_discuss}

\subsection{Magnetic Connectivity: CME-Shock vs. Flare Site}
\label{subsect_magconnect}
As noted earlier in Section~\ref{subsect_connect}, the \emph{Fermi} $\gamma$-ray emission centroid is closer to the footpoints of the closed field lines connecting the source AR than those of the open field lines connecting the CME shock. It is possible that the particles accelerated at the flaring site or the areas passed by the coronal shock \citep{hudson18} can be trapped in the closed field through some mechanisms (e.g., \citealt{sheeley04}), re-accelerated, and then transported to the front side of the Sun through the connectivity established by the interaction between the erupting flux rope and global corona field. However, we would like to emphasize that, based on the present simulation result, it is difficult to unambiguously distinguish the potential contributions from the two groups of field lines to the observed LAT emission for four reasons. (i) The northern portion of the open-field footpoints is adjacent \emph{in space} to both the closed-field footpoints and the LAT centroid; (ii) The appearances of the closed field ($t \sim 5$~minutes) and open field ($t \sim 6$~minutes) are very close \emph{in time};	(iii) The current localization of the LAT centroid is based on an assumption of a point source for the $\gamma$-ray emission and can change if the actual source shape deviates from this assumption; (iv) Because of the proximity between the open and closed field lines, cross-field diffusion (e.g., \citealt{zhang03}) can allow shock-accelerated energetic particles to access the closed field lines as well.

\subsection{The CME-shock and $\gamma$-ray Connection}
\label{subsect_shockconnect}

However, our simulation result of the Sept14 event together with our initial inspection of other {\it Fermi}\  BTL flares, does reveal some unique and attractive features about the CME-driven shock linked to the observed $\gamma$-rays:

\begin{enumerate}

\item
Since the shock compression ratio is one of the key parameters in the DSA mechanism that determines the energetic particle production at the shock (e.g., the particle spectral index), the temporal correlation noted in Item~1 (Section~\ref{subsect_shock}) above indicates an intimate relation between the $\gamma$-ray flux and the shock particle production. This provides clear evidence supporting the mechanism that (at least some of) the $\gamma$-ray producing particles are accelerated by the CME-driven shock.

\item
The open field is connected to a quasi-perpendicular shock early on (Item~4 in Section~\ref{subsect_shock}), which is generally believed to be an efficient particle accelerator if the upstream coronal or heliospheric magnetic field is sufficiently turbulent (e.g.,\citealt{giacalone05, tylka05}). Furthermore, a recent \emph{in-situ} observation of Saturn's bow shock from the Cassini spacecraft \citep{masters17} shows that energetic electrons were only detected \emph{downstream} of the quasi-perpendicular shock, which suggests the potential importance of a quasi-perpendicular shock in accelerating particles that could escape the \emph{downstream} and propagate \emph{back to the Sun} to produce $\gamma$-rays.

\item
Another piece of supporting evidence for shock acceleration is that in all three identified \emph{Fermi} BTL events (Sept14, {\it SOL2013-10-11}, and {\it SOL2014-01-06}; \citealt{pesce15, ackermann17}), there are pre-existing open field lines (e.g., in on-disk coronal holes) near the $\gamma$-ray emission region, which could be potentially connected to the CME-driven shock.

\end{enumerate}

By using a 3D triangulation technique, \citet{plotnikov17} reconstructed the CME-driven shock structure from white-light observations of the Sept14 event. With the density and magnetic field information obtained from a \emph{static} solar corona constructed with the Magnetohydrodynamic Algorithm outside a Sphere (MAS) model \citep{lionello09}, the time-dependent distribution of the shock Mach number and obliquity angle were approximately derived. They found that the Mach number shows a rapid increase to supercritical values after the type-II burst onset and the shock has a quasi-perpendicular geometry during the $\gamma$-ray emission, which are in general agreement with our results. However, an important distinction between their and our studies is that, instead of using a \emph{static} coronal model, we self-consistently simulated the \emph{dynamic} evolution of the CME and the CME-driven shock. This allows us to track the detailed temporal evolution of the shock and derive the shock compression ratio, which is of critical importance to particle acceleration by shocks. In addition, we found that the shock geometry evolves and changes from quasi-perpendicular to quasi-parallel, instead of remaining quasi-perpendicular all the time.

We also briefly discuss the shock Alfv\'{e}n Mach number evolution derived from the simulation. Note that when this number is around unity (see Item~3 in Section~\ref{subsect_shock}), stochastic acceleration of particles by plasma turbulence (e.g., in the downstream of the shock) is more efficient than DSA \citep{petrosian16}. Stochastically accelerated particles could also serve as the seed population to be further accelerated by the shock. This could be the case early on, when the shock compression ratio is also relatively low, and could be related to the rapid rise in the detected LAT $\gamma$-ray flux. Later on, when the shock Alfv\'{e}n Mach number and compression ratio are sufficiently large, shock acceleration would be more important and can account for the gradual, long-duration $\gamma$-ray emission. Therefore, it is likely that, in addition to DSA, stochastic acceleration could also play a role in the Sept14 event, especially in the early stage. On the other hand, as mentioned in \S 3.1, the simulated CME speed is 10-14\% slower than the observed one. Considering the higher shock speed in the simulation, the Alfv\'{e}n Mach number will also be higher. The critical Alfv\'{e}n Mach number is estimated between 1 and 1.7 for the solar wind plasma with $\gamma = \frac{5}{3}$ and $\beta = 1.0$ \citep{edmiston84}. Therefore, it is also possible that the shock in the simulation already becomes supercritical in the early stage. In summary, we believe multiple acceleration mechanisms could be important in the beginning but DSA might be the dominant one after 20 minutes.

\subsection{Effect of Magnetic Mirroring}
\label{subsect_magmirror}

Finally, we discuss the possibility of particle transport back to the Sun from the CME-driven shock. This may appear difficult because of strong magnetic mirroring due to the high degree of convergence of magnetic field lines  toward the Sun (with a mirror ratio of $\eta=B_{\odot}/B _{\rm CME}\gg 1$) and thus extremely small loss cones (e.g., a few degress; \citealt{klein18}, see their Section 8.4.4). In an ideal \emph{scattering-free} environment, this could potentially prevent particles from reaching the photosphere to produce $\gamma$-rays. In reality, however, the CME environment in general, and the shock downstream region in particular, are most likely \emph{highly turbulent}, rendering a sufficiently short scattering mean free path which can continuously scatter particles into the loss cone, thus precipitating to the Sun. How fast and what fraction of the particles can reach the photosphere depend on the relative values of the duration $\Delta T$ of the emission and the escape time from the trap, $T_{\rm esc}$. The latter depends on the mirror ratio $\eta$, the scattering time $\tau_{\rm sc}$, and the crossing time from the shock back to the Sun, $\tau_{\rm cross}\sim L/v_p$, where $v_p\sim c$ is the velocity of GeV protons responsible for $\gamma$-rays and $L=v_{\rm CME}\Delta T$ is the distance between the CME and the Sun. With some analytical and numerical treatments, \citet{malyshkin01} gave an approximate relationship between the escape time and the three variables $\eta$, $\tau_{\rm sc}$, and $\tau_{\rm cross}$ (see Figure 2, Petrosian 2016):
\begin{equation}
T_{\rm esc}=\tau_{\rm cross}\left(2\eta+\frac{\tau_{\rm cross}}{\tau_{\rm sc}}+\ln\eta\frac{\tau_{\rm sc}}{\tau_{\rm cross}}\right).
\end{equation}
Recent numerical simulations by \citet{effenberger18} have confirmed this relation. The upshot of this result is that for an \emph{isotropic} pitch-angle distribution, $T_{\rm esc}\sim 2\eta \tau_{\rm cross}$ for $\tau_{\rm sc}\sim \tau_{\rm cross}$ and $\eta \gg 1$, which means that $T_{\rm esc}/\Delta T\sim 2\eta v_{\rm CME}/c \sim \eta/100$ for a CME speed of $v_{\rm CME}=1,500$ km/s. Therefore, for $\eta\lesssim 100$, we have $T_{\rm esc} \lesssim \Delta T$; i.e., a large fraction of the downstream GeV protons can reach the photosphere within the emission duration $\Delta T$. We have tracked the history of the magnetic field strength along the field lines connecting the shock to the solar surface in our simulation and found that the median value of the mirror ratio $\eta$ increases from $\sim 10$ to $\sim 100$ during the first hour (Figure \ref{fig:shock_profile}f). Thus, for the first few hours, which is the duration of most Fermi events, the difficulty of particle transport back to the Sun due to magnetic mirroring can be overcome with a scattering mean free path of order of a solar radius or a scattering time of $\tau_{\rm sc}\sim 2$ s. For protons with gyro-frequency of $\Omega_p\sim15\cdot\left[\frac{B}{mG}\right]$  Hz, and magnetic field of $\sim$100 mG (the typical average value on the shock surface in the first hour of simulation), this would require a fractional turbulence energy ($\delta B/B)^2\sim 1/(\Omega_p \tau_{\rm sc})\sim 3\times10^{-4}$. According to \citet{effenberger18}, the situation is similar for a \emph{pancake} pitch-angle distribution. But for a distribution \emph{beamed} along the field lines, the escape time will be shorter and thus facilitate particle precipitation back to the Sun.

\section{Summary \& Conclusion}
\label{sect_summary}

In this study, we simulated the CME associated with a well-known \emph{Fermi} BTL flare on September 1, 2014 by using a data-driven global MHD model AWSoM within SWMF. We tracked the dynamic evolution of the global magnetic field and the CME-driven shock and investigated the magnetic connectivity between the shock and the region around the centroid of the \emph{Fermi}-LAT $\gamma$-ray source. We found supporting evidence for the hypothesis that the observed $\gamma$-ray emission is produced by particles that are accelerated in the CME environment and escape the shock downstream region along magnetic field lines connected to regions on the Sun far away from the hosting AR of the flare. Our specific findings are summarized as follows:

\begin{enumerate}

\item
To enable the high-energy particle precipitation and thus $\gamma$-ray emission on the front side of the Sun, certain \emph{magnetic connectivity} must be established between the emission region and the flare source AR or the CME-driven shock. In our simulation, both types of connections are present and appear close in space and time within the first few minutes of the event, as a result of the interaction between the erupting flux-rope magnetic field and the global solar corona. The CME-driven shock is connected to the front side of the Sun by open magnetic field lines that originate from an on-disk coronal hole. This part of the shock surface is away from the flux-rope driver and the shock nose that are propagating in a different direction. Such open-field configurations represent a favorable condition for connecting the CME-driven shock back to the solar surface, and have been identified in all three \emph{Fermi} BTL events reported so far.

\item
Within the shock surface connected to the front side of the Sun, the \emph{shock properties} vary significantly with time and space. The temporal evolution of the compression ratio and thus the rate of particle acceleration by the shock are closely correlated with the {\it Fermi}\  $\gamma$-ray flux, suggestive of a causal relationship. In addition, this part of the shock is initially a quasi-perpendicular shock and later evolves to a quasi-parallel shock, the former of which is believed to be an effective particle acclerator.

\item
These findings provide strong support for the aforementioned hypothesis and indicate that the \emph{CME-driven shock} can play an important role in accelerating particles that then travel back to the Sun to produce observed $\gamma$-rays. In addition to DSA, \emph{stochastic acceleration} by plasma turbulence may play a role as well, especially in the shock downstream region and during the early stage of the event.

\end{enumerate}

The present study is among the first attempts to solve the puzzle of {\it Fermi}\  BTL $\gamma$-ray flares. The identified mechanisms, in general, could be at work in on-disk \emph{Fermi} flares as well and can potentially solve another puzzle, i.e., long-duration $\gamma$-ray flares. BTL and long-duration $\gamma$-ray flares could be viewed as two faces of the same puzzle, with the $\gamma$-ray emission being \emph{spatially separated} in the former and \emph{temporally delayed} in the latter from the main flare emission commonly observed at longer wavelengths. In fact, recent statistical studies show that long-duration $\gamma$-ray flares observed by \emph{Fermi}/LAT always associated with wide, fast CMEs \citep{winter18} and Type II radio bursts \citep{gopal18b}. These results strongly support that long-duration $\gamma$-rays are produced by shock-accelerated protons precipitating back to the Sun.

Ultimately, one needs to self-consistently couple MHD simulations with particle acceleration, escape, and transport models (e.g., Borovikov et al. 2017, \citealt{hu18}). Furthermore, a comparative study is needed among not only the BTL events but also the on-disk events, by combining observational and simulation efforts, which we plan to pursue in future studies.

\begin{acknowledgements}
We are very grateful to the referee for invaluable comments that helped improve the paper. M.J. and W.L. were supported by NASA's {\it SDO}/AIA contract NNG04EA00C to LMSAL. W.L. by NASA HGI grants NNX15AR15G and NNX16AF78G and LWS grant NNX14AJ49G. N.V.N by NSF grant AGS-1259549. F.E. by NASA grant NNX17AK25G. G.L. by NASA grants NNX17AI17G and NNX17AK25G. W.M. by NASA grant NNX16AL12G and NSF AGS 1322543. We are thankful for the use of the NASA Supercomputer Pleiades at Ames and to its supporting staff for making it possible to perform the simulations presented in this paper.

The \emph{Fermi} LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \'{a} l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucl\'{e}aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. {\it SDO} is the first mission of the NASA's Living With a Star (LWS) Program.
\end{acknowledgements}

\newpage

redpajama_set_name: RedPajamaArXiv


text:
Phillip Phillips' "Home" Now in No. 1 on Rock Digital Songs, No. 8 in the Hot 100 Songs on Billboard
December 1, 2012 by jio-admin
American Idol winner Phillip Phillips' "Home" is now No. 1 on Rock Digital Songs, and No. 8 on the Hot 100 Songs on Billboard.com as of December 1, 2012. "Home" is also No. 3 on Rock Songs, No. 12 on Radio Songs, and No. 12 on Pop Songs.
Phillip Phillips has earned phenomenal success with his coronation song "Home." The single is already a certified double platinum selling over 2 million copies. "Home" is the only song from American Idol 2012 that made it to Top 10 on the Hot 100 Songs on Billboard.
Phillip Phillips, American Idol winner
The Top 10 songs in the Hot 100 are:
"Diamonds" by Rihanna
"Die Young" by Ke$ha
"One More Night" by Maroon 5
"Locked Out of Heaven" by Bruno Mars
"Gangnam Style" by PSY
"Some Nights" by fun
"Ho Hey" by The Lumineers
"Home" by Phillip Phillips
"I Cry" by Florida
"Let Me Love You (Until You Learn to Love Yourself)" by Ne Yo
Categories Entertainment, News Tags "Die Young" by Ke$ha, "Home", "Home" No. 1 Rock Digital Songs, american idol season 11, Billboard, Hot 100 Songs, No. 8 Hot 100 Songs, phillip phillips, Phillip Phillips' "Home" No. 1 Rock Digital Songs, Phillip Phillips' "Home" No. 8 Hot 100 Songs Billboard Leave a comment Post navigation
World AIDS Day: Decrease of AIDS Cases Difficult in Third World Countries, NIH Talks about Antiretroviral Drugs for HIV Prevention
X Factor USA is Inviting Fans to Select Songs and Wardrobes for Their Favorite Top 6 Contestants for the Pepsi Challenge Week


text:
20 Questions With Arielle Miralles
Arielle Miralles. Photo by Karolina Kuras.
A graduate of the RBC Apprentice Programme, Arielle Miralles joined The National Ballet of Canada in the 2022/23 season as a full member of the Corps de Ballet. Get to know this promising artist through our "20 Questions" series!
What inspired you to join The National Ballet of Canada?
I first saw the National Ballet perform Giselle in 2011 when I was a student at Canada's National Ballet School. I was enamored and totally captured by the tragedy, power and love of former Principal Dancer Sonia Rodriguez, who was dancing the role of Giselle. I was so enthralled by her storytelling and the beauty of her dancing that I forgot where I was. It was in that moment that I knew I wanted the opportunity to dance with National Ballet. I continued attending all their performances as a student and even began to fangirl over all the dancers – and yes, it felt like all the dancers I grew up watching were these celebrities who then became my wildly talented colleagues and friends!
What would you have done as a career if you hadn't pursued ballet?
I would probably be a baker or a chef. I'm a huge foodie and I'm always bringing baked goods into work to cheer people up!
Have you ever had an embarrassing moment on stage?
Many. Falling, slipping, tripping, even forgetting choreography! Although it feels mortifying, the best any dancer can do is shake it off and not let it get to you. Keep calm and carry on.
What is your work philosophy?
1% better every day.
How do you handle criticism?
I really welcome feedback, positive or negative. I try to view criticism as a tool to guide me in new directions and explore different perspectives. I know that every constructive comment may come with a bias, so I'll often try it out and see if it works for me. If it's something that I can use to enhance my work, I'll apply it in order to expand myself as a dancer and as a person.
Arielle Miralles backstage at Swan Lake. Photo by Karolina Kuras.
What's your definition of a successful ballet dancer?
"People will forget what you said, people will forget what you did, but people will never forget how you made them feel." – Maya Angelou
My mom told me this as a kid growing up and it's exactly what I experienced while watching that performance of Giselle in 2011. Like watching a movie or reading a book, people use these forms of entertainment as an escape from their own reality and to be immersed in the art. I see a successful dancer as someone capable of making an audience feel the emotion, visualize the movement and understand the story they are expressing onstage, making them forget about everything else that's happened outside the theatre. That is the most powerful kind of dancer.
What's the best thing about being a dancer?
Getting to do what you love every day! It's still surreal.
What's the worst?
The blisters.
What music are you listening to right now?
I love a lot of different genres of music. I got this trait from my dad.
I love spending quality time and sharing meals with my friends or family. I really enjoy something as simple as going on a walk with coffee or cooking together.
What are three things most people don't know about you?
I faint every time I go for a blood test.
My version of vintage shopping is going through my parents' closet.
I've rewatched Gilmore Girls far too many times.
What cheers you up on an off day?
Calling my parents. They're my best friends.
Do you have any bad habits that you're working on breaking?
Overthinking.
Arielle Miralles in Rehearsal for The Collective Agreement. Photo by Karolina Kuras.
What is your favorite onstage memory?
Our first performance back after the pandemic. We performed George Balanchine's Serenade, and it was one of those shows where you trusted yourself enough to let go and let the combination of the choreography meet the incredible music to take you to what felt like another planet. It was a milestone moment for me where I learnt the power of self-confidence.
Do you have any performance rituals or superstitions?
My ballet teacher from school, and former National Ballet dancer, Lise-Marie Jourdain passed on the tradition of eating a banana before every show.
What's the biggest risk you've taken, either personally or in your career?
Trusting myself. It's easy to get wrapped up in the outcomes of situations and lose your sense of being grounded. Learning to trust the process has been one of the hardest things but has changed my outlook and perspective.
Could you name someone who has mentored or inspired you?
My mom. And Second Soloist Selene Guererro-Trujillo. I aspire to one day be as strong, resilient and kind as these women. They teach and inspire me daily.
Where would you like to travel, but haven't yet?
The South of France. I want to wake up and eat a freshly baked croissant, dip my toes in the Mediterranean Sea and explore the beautiful and historical architecture.
What is your perfect meal?
A charcuterie board. I enjoy pretending to be Ratatouille and putting together different combinations of food.
What's the top item on your bucket list?
Humanitarian work. I feel so lucky that I'm able to live the life I do, so I enjoy giving back and helping others who are less fortunate. When I have the time I go to my local Food Bank to volunteer, but I'd love to travel abroad and do some work with children one day.
Artists of the Ballet in Serenade. Photo by Karolina Kuras.
Learn more about Arielle
Read More Dancer Q&As
Ross Allen
Isabelle Bratt
Emerson Dayton
Josh Hall
Sophie Lee
Keaton Leier
Emma Ouellet
McKhalya Pettingill
Anima Animus: A Company Premiere by David Dawson
Cinderella Synopsis
Arielle Miralles
Hope Muir on 2022-23


Website ISS Facility Services, Inc.
A new part-time role CUSTODIAN – PT – Night – $10.00 is available in Yankton, SD 57078. Highly motivated candidates are encouraged to apply. Please check full job details offered by ISS Facility Services, Inc. below.
Company: ISS Facility Services, Inc.
Oversees the day-to-day duties of all janitors while performing routine cleaning of offices and public areas and maintenance of tile and carpeted floors in buildings; solves minor cleaning problems. Assists in assigning work schedules and in coordinating special cleaning jobs with management.
Determines type of chemicals and equipment necessary for specific cleaning tasks.
Identifies cleaning problems and determines appropriate remedies.
Makes rounds to check for crew coverage of designated work areas, assigns needed coverage, gives special cleaning instructions and/or assignments, and ascertains compliance with directives.
Oversee the work task of janitors in Supervisors' absence. Responsibilities include assigning and directing work; addressing complaints and recommending solutions; reporting any disciplinary concerns to supervisor/manager.
1+ experience or training. Completed all safety and task training certification provided.
Knowledge of occupational hazards and safety rules and regulations.
Ability to work in a demanding, fast paced, high volume environment.
Must be a team player and committed to working in a quality environment.
Demonstrates exceptional customer service skills.
Bilingual in Spanish is a plus.
While performing the duties of this job, the employee is occasionally exposed to normal weather conditions for the area. While performing the duties of this job, may be working around semi-trucks and trailers, dumpsters, and vans. This may include construction areas and the hazards associated with such. The noise level in the work environment is usually moderate. Hearing Protection not required, but may be worn for comfort.
The above statements are intended to describe the general nature and level of work performed by people assigned to this classification. They are not intended to be construed as an exhaustive list of all responsibilities, duties and skills required of personnel so classified. Management retains the discretion to add to or change the duties of the position at any time.
ISS Facility Services is an Affirmative Action and Equal Opportunity Employer that promotes a diverse workplace.


Are you energetic, enthusiastic, love to work with children and want to give back to your community?
We are looking for responsible volunteers that are passionate about camp! If you are a team player, demonstrate leadership capabilities, have strengths in group environments and delivery in a wide range of specialized programming areas, such as Outdoor activities, Orthodox faith, Arts, Drama, Dance, Hiking and sports, etc, then Camp Met is for you!
Counselors hold the most important job at camp as they are the role models for our campers! You are the campers' caregiver, instructor, leader, positive role model, and best friend. Counselors enjoy meals with their campers, assist in activity programs, participate with them during evening programs, theme days, fun with other cabins and much, much more! All Counselors help to facilitate friendships, cabin identity, mutual support, and help build unforgettable memories. They ensure that campers have a safe and healthy camp experience.
Previous camper or camp related experience is required.
A current Police Record Check/Vulnerable Sector Check is required immediately after an offer has been made and a copy must be emailed prior to Camp Met Start Date.
A Current Standard First Aid & CPR-C Qualification is preferred for all successful applicants but is not mandatory.
It is the applicants responsibility to attend the Volunteer Counselor Orientation that is provided at the date disclosed to successful applicants.
It is the applicants responsibility to cover the cost of the Police Record/Vulnerable Sector check.
It is the applicants responsibility to attend an interview on a date in which we will specify**All successful applicants must attend all the dates provided for Interview, Orientation and Meetings in order to attend Camp Metamorphosis Ontario 2019.


He's so young, so talented, and so cheap that the Marlins are telling teams that, in order to deal their ace, they would need a return that makes them better not just in the future but also today. According to Clark Spencer of the Miami Herald , Miami President of Baseball Operations Michael Hill said Fernandez was not available. However, for a pitcher as skilled as Fernandez, all names should be on the table.
CARDINALS 27, RAMS 3 (at St. Louis) - The Cardinals' Larry Fitzgerald made his 1,000th reception and topped 1,000 yards for the seventh time. Against the Philadelphia Eagles, the Patriots receivers were absolutely terrible with many dropped passes, a lot coming from Brandon LaFell.
Plenty more can be expected from baseball's Winter Meetings! Details of Soria's agreement were provided by a person familiar with the negotiations who spoke on condition of anonymity because it had not yet been announced. Chris Young figures to provide key rotation depth as a guy that wears down over the long term in the rotation, but can dominate for short spurts.
That 4.10 ERA was exactly league average for a starter before you even account for Miley's home park, and that performance, combined with his low pay, is precisely why the Sox cannot just give him away. The latter includes a $500,000 club buyout. Regardless of whether he gets the pay bump (not likely), that doesn't necessarily mesh with Dipoto's vision to build around the Mariners current core rather than make a pricy acquisition.
Former USC head coach Steve Sarkisian is claiming that his former employer kicked him "to the curb" as he was fighting his addiction issues when he was head coach earlier this season.


Torturing terrorists for national security imperatives: Mediated violence on "24"
This study analyzed mediated violent content as seen on the FOX television program 24. The study covered a seven year period, or six seasons, of 24 , with a sample set of 43 episodes and 445 individual acts ofviolence. Three research questions guided this study. The first research question sought to determine if a relation exists between heroic characters inflicting torturous violence and justifying the act with a national security imperative. The second research question examined the prevailing mode of violence and the use of nonlethal and lethal weapons. The third research question examined the portrayed efficiency of violence on24. Findings suggest that while torture is rarely the intent and rarely justified with a national security imperative, 24 is nonetheless very violent, generally portraying violence as physical, involving the use of lethal weapons, intentionally gratuitous, and most often efficient.
Sears, Michael D., "Torturing terrorists for national security imperatives: Mediated violence on "24"" (2009). UNLV Theses, Dissertations, Professional Papers, and Capstones. 1183.


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