text:
Oliver's shares nosedive by 55pc after a "very disappointing" result
January 30, 2019 February 10, 2019 | Nick Sundich
Healthy fast food chain Oliver's has disappointed shareholders again, releasing yet another profit downgrade in spite of a change of leadership and strategy.
Investors responded accordingly, dumping the stock and sending it lower by 55 per cent to 4.3c, a fraction of its 20c IPO price exactly two years ago.
Full year revenue is now expected to be 12-15 per cent lower than forecast in November at $34-$38 million, while EBITDA (earnings before interest, tax, depreciation, amortisation) has swung from a forecast $3m-4m profit to a $1m-4m loss.
Oliver's blamed the downgrade on a rage of factors, from roadworks outside flagship stores to new pricing and products not having the expected effect, similar reasons as the profit downgrade in May last year.
The company is still walking off the strategy from prior management of opening stores in marginal areas.
Oliver's chairman Mark Richardson admitted to investors he was "very disappointed" but was confident shareholders would soon start to see improvement from changes being implemented.
"We must allow time to realise the benefits of the changes over the coming months and for these to flow through to performance and profitability," he said as he asked investors for patience.
Oliver's has issued full year profit downgrades in both years it's been listed and showed the founder to the door in June.
Oliver's shares over the last 12 months.
The quarterly figures were also disappointing.
While Oliver's received $8.9 million in cash receipts over the December quarter, which was slightly higher than the prior period, it didn't reflect the fact that Christmas and holiday trading should have been an historically stronger time of year for the retailer.
CEO Greg Madigan was optimistic about the company's future in spite of its poor run of results.
"The Oliver's brand is young and still offers incredible potential. If we continue our consolidation, improving the current portfolio and resolving sales and profitability challenges in subdued trading conditions, we will be in an incredibly strong position to move forward and expand, realising the potential we all know the brand possesses," he said.
Oliver's has announced $1m of cost savings including the closure of its Dubbo store, and from renegotiating supply deals.
It says further store closures and redundancies may occur in the future.
The Company has made significant capital expenditure in recent months such as for new ovens and migration to a new accounting system, but these have not yet borne fruit.
Although the company undertook a capital raising in November, it only raised $4.1m of the $7.4 it wanted and the company admitted the remaining stock is unlikely to be placed within the three-month shortfall deadline.
Stockhead has contacted Oliver's for comment.
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"Sir G: Wharton ...who writ the yearely Almanac, during his Majesties troubles:"
Palmieri begins: "The satiric and parodic almanac Poor Robin was published annually from the mid-1660s through the early nineteenth century. When nine or twelve almanacs for the same year were bound together (as they often were), Poor Robin usually concluded the collection, like a satyr play following a tragic trilogy in Athens, mocking and inverting the conventions of the more serious genre. But Poor Robin not only emptied out the serious almanac; it also accommodated the form it parodied. After the first year of its appearance, the parodic almanac was published by the same Stationers' Company that energetically protected its monopoly on the publishing of all the other almanacs in England. This essay will concern itself with four episodes in the history of the parodic and satiric almanac. Originating with Rabelais and others in the early sixteenth century, the satiric almanac becomes increasingly partisan in England from the 1590s to the 1650s. Early in the Restoration, Poor Robin begins annual publication, and the following four decades see it at its most innovative and suggestive. Swift refers to Poor Robin and builds on the tradition of the satiric almanac when he writes the predictions of Isaac Bickerstaff for 1708, which begin by foretelling the death of John Partridge, another almanac-maker. The Poor Richard almanacs, written by Benjamin Franklin from 1732 to 1758, take Poor Robin and Swift's predictions as two of their models; in form they parallel but in political perspective they diverge dramatically from almanacs on the other side of the Atlantic."
"Mr. Povy, whose vanity, prodigality, neglect of his business, and committing it to unfit hands..."
Hmm. Wasn't one of those hands Pepys himself?
Could someone help explain exactly what has "undone" Povy? Thanks.
William Prynne has gotten the reputation of a crank, whom nobody takes seriously any more. A very hard thing to overturn, once established.
"he told me many fine things"
Pepys never loses an opportunity to tap any likely source for news of who's in, who's out, who's up, who's down. All potentially useful information to the rising man.
"Yesterday Dr. Whistler, at Sir W. Pen's, told me that Alexander Broome, a the great song-maker, is lately dead"
L&M Brome (Lawyer, versifier and dramatist) had died on 29 June.
"Could someone help explain exactly what has "undone" Povy?"
I gather Pepys is being told that Povey's undone as he can't repay a debt to the Duke of York that's been suddenly declared due ("revived"). His prosperity has long been quite dependent on the Duke's fiduciary trust in him. He'd been Treasurer to the Tangier Committee -- which the Duke chaired --, and is still Treasurer to the Duke himself. L&M note he will be replaced in this role by Sir Allen Apsley this coming September.
",Mr. Vaughan, whom he reports as a man of excellent judgement and learning, but most passionate and 'opiniastre'"
L&M: John Vaughan was M.P. for Cardiganshire and a leading member of the country party . To Clarendon (whose impeachment Vaughan was to support in 1667) he was 'proud and insolent... magisterial and supercilious': Life, i. 37. He was made Chief Justice of Common Pleas and knighted in 1668.
"[Mr. Finch] told me Mr. Prin's character; that he is a man of mighty labour and reading and memory, but the worst judge of matters, or layer together of what he hath read, in the world; which I do not, however, believe him in;"
L&M: The consensus of opinion is with Finch not Pepys: William Prynne's method of writing a book was to discharge his materials pell-mell on to the page and into the margins.
"[Mr. Vaughan] believes [Mr. Prynne] had always very true to the King in his heart, but can never be reconciled to episcopacy; that the House do not lay much weight upon him, or any thing he says."
L&M: Prynne had always supported monarchy, but had opposed jure divino episcopacy. In the Commons he had been reprimanded in 1661 for a pamphlet addressed to the Lords against the Corporation Bill (CJ , viii. 301-2). The Corporation Act of 1661 was an Act of the Parliament of England (13 Cha. II. St. 2 c. 1). It belonged to the general category of test acts, designed for the express purpose of restricting public offices in England to members of the Church of England.
https://www.pepysdiary.com/diary/1664/05/13/#c1... He was too bookish and long-winded -- too fond of perambulating among his precedents -- to be a good oarliamentarian: Cf. The Moderate, 12 December 1648: John Price. Mystery of...Resttauration (1680), p. 131; Milward, p. 130.


text:
Family Weekend Features Whole Host of Activities, North Country in the Fall
Parents and families coming to campus Sept. 20-22 will find a full slate of activities and programs as part of SUNY Plattsburgh's annual Family Weekend.
Organized by the Center for Student Involvement, the weekend begins Friday from 4 to 7 p.m. with registration in the Angell College Center. There, families can check in, pick up reserved tickets and a schedule of events and suggestions for things to do in the North Country.
Theater Friday Night
Friday night, families can attend the Black Box Theater production of "White Room of My Remembering," the story of two women who come to put a childhood home up for sale. One of the women begins a series of conversations with herself as a young girl and with the dead parents. Curtain is at 7:30 p.m. Friday and Saturday. Tickets are $8 general public, $5 faculty, staff, seniors and alumni, and $3 for SUNY Plattsburgh students and are available online at https://plattsburgh.university.tickets.com.
Later, join a game of Bingo in the Sundowner, Angell College Center, beginning at 9 p.m.
Registration picks back up Saturday in the ACC lobby at 9 a.m. Afterwards, join the Sorority Association for a free pancake breakfast in the Sundowner. Donations welcomed for St. Jude's Children Hospital.
If running is your family activity, the Center for Student Health and Psychological Services is sponsoring a three-mile fun run/walk beginning at 9:30 a.m. with sign-ups beginning at 9 in the lobby of the Student Health Center. Meet in the Student Health Center parking lot.
Cardinal Soccer
Sports fans can cheer on the Cardinal men's soccer team as they meet Clarkson University at 2 p.m. on the Field House soccer complex. Stick around the Field House and go ice skating at 3 p.m. in the Stafford Ice Arena.
After dinner at any of the area's restaurants — families can ask for suggestions at registration — or in Clinton Dinning Hall with their students, they can catch a musical comedy routine, "Dueling Pianos," beginning at 8 p.m. in the Warren Ballrooms, Angell College Center.
Family Weekend wraps up at 10 a.m. Sunday with the Presidents' Lakeside Breakfast Buffet at Valcour Inn and Boathouse, overlooking Lake Champlain and Valcour Island, the site of the first major naval engagement of the American Revolution. Breakfast is hosted by college administrators and Essence Hightower, president of the Student Association, with student musical accompaniment. Advance reservations and tickets are required. Space is limited.
'Perfect Time to Come to Campus'
"Family Weekend is the perfect time for families to come to campus," said Cori Jackson, assistant vice president for student life in in enrollment and student success and director of the Center for Student Involvement.
"Students have had a few weeks getting to know campus and getting settled in their routines so they can show their family members around, point out where their classes are, show them their residence hall, maybe eat in Clinton Dining Hall. The North Country is beautiful in the fall, so there are plenty of opportunities for families to explore the area, maybe go apple picking or take a drive up to Lake Placid. And it's a perfect break between the start of school and when most students return for the first time over Thanksgiving break," she said.
For a detailed schedule, suggestions for things to do in the area and where to stay, visit https://www.plattsburgh.edu/parents-families/family-weekend.html.
Submissions Open for Skopp Competition on Themes of Holocaust
On-Campus, On-Line Events Planned for Prospective SUNY Plattsburgh Students
Local Professor, Students Participate in National Exhibit on Incarceration
SUNY Plattsburgh Announces Fall 2019 Dean's List
Human Resource Management Certificate Can Lead to New Career Opportunities
Alumnus Features Retired President in Public Radio Program
View All NewsView All Events
Last Updated 9/6/19

redpajama_set_name: RedPajamaCommonCrawl


text:
package com.dbumama.market.model.base;

import com.jfinal.plugin.activerecord.Model;
import com.jfinal.plugin.activerecord.IBean;

/**
 * Generated by JFinal, do not modify this file.
 */
@SuppressWarnings("serial")
public abstract class BaseShipping<M extends BaseShipping<M>> extends Model<M> implements IBean {

	public void setId(java.lang.Long id) {
		set("id", id);
	}

	public java.lang.Long getId() {
		return get("id");
	}

	public void setOrderId(java.lang.Long orderId) {
		set("order_id", orderId);
	}

	public java.lang.Long getOrderId() {
		return get("order_id");
	}

	public void setExpKey(java.lang.String expKey) {
		set("exp_key", expKey);
	}

	public java.lang.String getExpKey() {
		return get("exp_key");
	}

	public void setBillNumber(java.lang.String billNumber) {
		set("bill_number", billNumber);
	}

	public java.lang.String getBillNumber() {
		return get("bill_number");
	}

	public void setActive(java.lang.Integer active) {
		set("active", active);
	}

	public java.lang.Integer getActive() {
		return get("active");
	}

	public void setCreated(java.util.Date created) {
		set("created", created);
	}

	public java.util.Date getCreated() {
		return get("created");
	}

	public void setUpdated(java.util.Date updated) {
		set("updated", updated);
	}

	public java.util.Date getUpdated() {
		return get("updated");
	}

}

redpajama_set_name: RedPajamaGithub


text:
Emma Raducanu: Former mentor says US Open champ will 'go through a lot of coaches'
By Georgia Goulding
Published: 20 Oct 2021, 15:19
After Emma Raducanu made history at the Arthur Ashe stadium by becoming the first qualifier to win a Grand Slam, she controversially split from coach Andrew Richardson.
Her US Open title has propelled her into the spotlight. Aside from scooping a handsome prize pot for her win at Flushing Meadows, she has signed ambassador deals with jeweller Tiffany & Co. and fashion house Dior.
Raducanu also rose from 150th in the world rankings to 24th and is now the new British number one, overtaking Johanna Konta.
The US Open was Raducanu's second ever Grand Slam tournament, having previously competed at Wimbledon back in June.
Less than two weeks after her win, she parted ways with Richardson, claiming she was looking for a mentor with more tour experience.
Finding a replacement seems to have been a more difficult task than anticipated for the Brit, as she is yet to tie down a new full-time coach.
She is currently trialing Konta's former mentor Esteban Carril after her brief spell with Jeremy Bates ended following her early exit from Indian Wells.
Mark Petchey, who coached Raducanu between July and December in 2020 and then returned for a brief one-month stint earlier this year, has commented on his former client's search for a new mentor.
"I think, to be honest, that Emma will go through a lot of coaches during her career," he said. "Because she will take what she needs from someone and she will find someone else who will be good for something else. She's very proactive about the way she wants to build her game.
"People need to understand that there will be a lot of collaborations during her career, rather than the 'hiring' and 'firing' of a coach. It feels so personal, and people need to stop getting hung up on hiring and firing."
Raducanu's first match following her US Open victory was a shock defeat to Belarusian Aliaksandra Sasnovich, who was ranked 100th in the world at the time.
The Brit has since withdrawn from the Kremlin Cup, which was scheduled to begin on October 18th in Moscow. Her next match will instead take place on the home soil of her father – the Transylvania Open in Cluj, Romania.
GMSw
News Now - Sport News
Tim Henman warns there will be 'bumps in the road' for Emma Raducanu
Multiple tennis stars could miss Australian Open due to vaccine regulations
Flavia Pennetta says Emma Raducanu would've 'never won a Slam' in her day
Georgia Goulding
Interested in: Football, Boxing, Formula 1, WWE
Reporting on all the badass women in sport. Liverpool supporter, motorsport fan, vinyl record collector and game show enthusiast by trade.
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text:
Home » IANS » McTominay pens down new long-term deal with Manchester United
McTominay pens down new long-term deal with Manchester United
Published on : Tue 23rd June 2020, 02:15 PM
London, June 23 (IANS) Midfielder Scott McTominay has signed a new contract with Manchester United which will keep him at the club until June 2025, with the option to extend for a further year.
"Whilst I understand that we all have so many other things to think about at the moment, I'm so happy to sign this contract and play a part in the future ahead for this team," McTominay said on Tuesday in a statement on the club's official website.
"All I have ever known is United and I hope that my passion for the club shows every time I go onto the pitch. I'll continue to give everything for this club whenever I pull on the shirt.
"I want to thank the manager for the faith he has shown in me and everyone at the club that has helped me to get where I am today. I'm looking forward to finishing this season on a high and hopefully achieving our aims," he added.
Scott, 23, has been at the club since 2012. He made his senior debut in 2017 against Arsenal and has gone on to make 75 appearances for the first team, scoring 6 goals. He is also a full Scotland international.
Ole Gunnar Solskjaer said: "Scott has done tremendously well since I joined and has been a vital part of our midfield. He brings determination, tenacity and skill to the game and we know that Scott's attributes will be a major asset to the squad over the coming years.
"I look forward to seeing his continued improvement in the years to come," he added.
aak/bbh/
Sushant's sister Priyanka remembers her 'brother, pride and alter ego'
Covid trigger for BSE Sensex's biggest bull run
Brisbane to lift indoor face mask mandate
Football Delhi announces scholarships for u-16 players
Biden's 1st foreign leader call to be with Trudeau


text:
package org.cocos2dx.lib;

import android.content.Context;
import android.graphics.Bitmap;
import android.graphics.Canvas;
import android.graphics.Color;
import android.graphics.Paint;
import android.graphics.Rect;
import android.graphics.Typeface;
import android.text.BoringLayout;
import android.text.Layout;
import android.text.StaticLayout;
import android.text.TextPaint;
import android.text.TextUtils;
import android.util.Log;

import java.nio.ByteBuffer;
import java.nio.ByteOrder;

public final class Cocos2dxBitmap {
    // ===========================================================
    // Constants
    // ===========================================================

    /* The values are the same as cocos2dx/platform/CCImage.h. */
    private static final int HORIZONTAL_ALIGN_LEFT = 1;
    private static final int HORIZONTAL_ALIGN_RIGHT = 2;
    private static final int HORIZONTAL_ALIGN_CENTER = 3;
    private static final int VERTICAL_ALIGN_TOP = 1;
    private static final int VERTICAL_ALIGN_BOTTOM = 2;
    private static final int VERTICAL_ALIGN_CENTER = 3;

    // ===========================================================
    // Fields
    // ===========================================================

    private static Context sContext;

    // ===========================================================
    // Getter & Setter
    // ===========================================================

    public static void setContext(final Context context) {
        Cocos2dxBitmap.sContext = context;
    }

    // ===========================================================
    // Methods for/from SuperClass/Interfaces
    // ===========================================================

    // ===========================================================
    // Methods
    // ===========================================================

    private static native void nativeInitBitmapDC(final int width,
            final int height, final byte[] pixels);

    //http://egoco.de/post/19077604048/calculating-the-height-of-text-in-android
    public static int getTextHeight(String text, int maxWidth, float textSize, Typeface typeface) {
        TextPaint paint = new TextPaint(Paint.ANTI_ALIAS_FLAG | Paint.SUBPIXEL_TEXT_FLAG);
        paint.setTextSize(textSize);
        paint.setTypeface(typeface);

        int lineCount = 0;

        int index = 0;
        int length = text.length();

        while(index < length) {
            int numOfChars = paint.breakText(text, index, length, true, maxWidth, null);
            index += numOfChars;
            lineCount++;
            //in andriod 4.4.2, the breakText will return 0, which would lead to infinite loop
            if (numOfChars == 0) {
                break;
            }
        }

        float actualHeight = (Math.abs(paint.ascent()) + Math.abs(paint.descent()));

        return (int)Math.floor(lineCount * actualHeight);
    }

    public static Typeface calculateShrinkTypeFace(String text, int width, int height, Layout.Alignment hAlignment, float textSize, TextPaint paint, boolean enableWrap)
    {
        if (width == 0 || height == 0) {
            return  paint.getTypeface();
        }
        float actualWidth = width + 1;
        float actualHeight = height + 1;
        float fontSize = textSize + 1;

        if (!enableWrap) {
            while (actualWidth > width || actualHeight > height) {
                fontSize = fontSize - 1;

                actualWidth = (int)Math.ceil( StaticLayout.getDesiredWidth(text, paint));
                actualHeight = getTextHeight(text, (int)actualWidth, fontSize, paint.getTypeface());

                paint.setTextSize(fontSize);
                if (fontSize <= 0) {
                    paint.setTextSize(textSize);
                    break;
                }
            }
        } else {
            while (actualHeight > height || actualWidth > width) {
                fontSize = fontSize - 1;

                Layout layout = new StaticLayout(text, paint, (int) width, hAlignment,1.0f,0.0f,false);
                actualWidth = layout.getWidth();
                actualHeight = layout.getLineTop(layout.getLineCount());

                paint.setTextSize(fontSize);

                if (fontSize <= 0) {
                    paint.setTextSize(textSize);
                    break;
                }
            }

        }
        return paint.getTypeface();
    }

    public static boolean createTextBitmapShadowStroke(final String string,  final String fontName, int fontSize,
                                                       int fontTintR, int fontTintG, int fontTintB, int fontTintA,
                                                       int alignment, int width, int height,
                                                       boolean stroke, int strokeR, int strokeG, int strokeB, int strokeA, float strokeSize,
                                                       boolean enableWrap,
                                                       int overflow,
                                                       boolean enableBold) {

        Layout.Alignment hAlignment = Layout.Alignment.ALIGN_NORMAL;
        int horizontalAlignment = alignment & 0x0F;
        switch (horizontalAlignment) {
            case HORIZONTAL_ALIGN_CENTER:
                hAlignment = Layout.Alignment.ALIGN_CENTER;
                break;
            case HORIZONTAL_ALIGN_RIGHT:
                hAlignment = Layout.Alignment.ALIGN_OPPOSITE;
                break;
            case HORIZONTAL_ALIGN_LEFT:
                break;
            default:
                break;
        }

        TextPaint paint = Cocos2dxBitmap.newPaint(fontName, fontSize, enableBold);

        if (stroke) {
            paint.setStyle(TextPaint.Style.STROKE);
            paint.setStrokeWidth(strokeSize);
        }

        int maxWidth = width;

        if (maxWidth <= 0) {
            maxWidth = (int)Math.ceil( StaticLayout.getDesiredWidth(string, paint));
        }

        Layout layout = null;
        int layoutWidth = 0;
        int layoutHeight = 0;

        if (overflow == 1 && !enableWrap){
            int widthBoundary = (int)Math.ceil( StaticLayout.getDesiredWidth(string, paint));
            layout = new StaticLayout(string, paint, widthBoundary , hAlignment,1.0f,0.0f,false);
        }else {
            if (overflow == 2) {
                calculateShrinkTypeFace(string, width, height, hAlignment, fontSize, paint, enableWrap);
            }
            layout = new StaticLayout(string, paint, maxWidth , hAlignment,1.0f,0.0f,false);
        }

        layoutWidth = layout.getWidth();
        layoutHeight = layout.getLineTop(layout.getLineCount());

        int bitmapWidth = Math.max(layoutWidth, width);
        int bitmapHeight = layoutHeight;
        if (height > 0) {
            bitmapHeight = height;
        }

        if (overflow == 1 && !enableWrap) {
            if (width > 0) {
                bitmapWidth = width;
            }
        }

        if (bitmapWidth == 0 || bitmapHeight == 0) {
            return false;
        }

        int offsetX = 0;
        if (horizontalAlignment == HORIZONTAL_ALIGN_CENTER) {
            offsetX = (bitmapWidth - layoutWidth) / 2;
        }
        else if (horizontalAlignment == HORIZONTAL_ALIGN_RIGHT) {
            offsetX = bitmapWidth - layoutWidth;
        }

        int offsetY = 0;
        int verticalAlignment   = (alignment >> 4) & 0x0F;
        switch (verticalAlignment)
        {
            case VERTICAL_ALIGN_CENTER:
                offsetY = (bitmapHeight - layoutHeight) / 2;
                break;
            case VERTICAL_ALIGN_BOTTOM:
                offsetY = bitmapHeight - layoutHeight;
                break;
        }

        Bitmap bitmap = Bitmap.createBitmap(bitmapWidth, bitmapHeight, Bitmap.Config.ARGB_8888);
        Canvas canvas = new Canvas(bitmap);
        canvas.translate(offsetX, offsetY);
        if ( stroke )
        {
            paint.setARGB(strokeA, strokeR, strokeG, strokeB);
            layout.draw(canvas);
        }
        paint.setStyle(TextPaint.Style.FILL);
        paint.setARGB(fontTintA, fontTintR, fontTintG, fontTintB);
        layout.draw(canvas);

        Cocos2dxBitmap.initNativeObject(bitmap);
        return true;
    }

    private static TextPaint newPaint(final String fontName, final int fontSize, final boolean enableBold) {
        final TextPaint paint = new TextPaint();
        paint.setTextSize(fontSize);
        paint.setAntiAlias(true);

        // Set type face for paint, now it support .ttf file.
        if (fontName.endsWith(".ttf")) {
            try {
                final Typeface typeFace = Cocos2dxTypefaces.get(
                        Cocos2dxBitmap.sContext, fontName);
                paint.setTypeface(typeFace);
            } catch (final Exception e) {
                Log.e("Cocos2dxBitmap", "error to create ttf type face: "
                        + fontName);

                // The file may not find, use system font.
                paint.setTypeface(Typeface.create(fontName, Typeface.NORMAL));
            }
        } else {
            if(enableBold) {
                paint.setTypeface(Typeface.create(fontName, Typeface.BOLD));
            } else {
                paint.setTypeface(Typeface.create(fontName, Typeface.NORMAL));
            }
        }

        return paint;
    }

    private static void initNativeObject(final Bitmap bitmap) {
        final byte[] pixels = Cocos2dxBitmap.getPixels(bitmap);
        if (pixels == null) {
            return;
        }

        Cocos2dxBitmap.nativeInitBitmapDC(bitmap.getWidth(),
                bitmap.getHeight(), pixels);
    }

    private static byte[] getPixels(final Bitmap bitmap) {
        if (bitmap != null) {
            final byte[] pixels = new byte[bitmap.getWidth()
                    * bitmap.getHeight() * 4];
            final ByteBuffer buf = ByteBuffer.wrap(pixels);
            buf.order(ByteOrder.nativeOrder());
            bitmap.copyPixelsToBuffer(buf);
            return pixels;
        }

        return null;
    }

    public static int getFontSizeAccordingHeight(int height) {
        TextPaint paint = new TextPaint();
        Rect bounds = new Rect();

        paint.setTypeface(Typeface.DEFAULT);
        int text_size = 1;
        boolean found_desired_size = false;

        while (!found_desired_size) {
            paint.setTextSize(text_size);
            String text = "SghMNy";
            paint.getTextBounds(text, 0, text.length(), bounds);

            text_size++;

            if (height - bounds.height() <= 2) {
                found_desired_size = true;
            }
        }
        return text_size;
    }

    private static String getStringWithEllipsis(String string, float width,
                                                float fontSize) {
        if (TextUtils.isEmpty(string)) {
            return "";
        }

        TextPaint paint = new TextPaint();
        paint.setTypeface(Typeface.DEFAULT);
        paint.setTextSize(fontSize);

        return TextUtils.ellipsize(string, paint, width,
                TextUtils.TruncateAt.END).toString();
    }
}


text:
\section{Introduction}\label{sec:intro}
In low-mass X-ray binaries (LMXBs) a black hole or neutron star accretes matter from a (sub-) solar-mass companion star. The donor typically overflows its Roche lobe and transfers mass to an accretion disc that surrounds the compact primary. Thermal-viscous instabilities in the accretion disc are thought to be the reason that many LMXBs are transient, i.e., cycle through outburst and quiescent episodes \citep[e.g.,][for a review]{lasota01}. Material is rapidly accreted during weeks--months long outbursts, resulting in X-ray luminosity of $L_{\mathrm{X}}$$\simeq$$10^{35}-10^{39}~\mathrm{erg~s}^{-1}$. In intervening quiescent phases, the luminosity is orders of magnitude lower and little or no matter is reaching the black hole or neutron star.

Along the course of an accretion outburst, prominent changes in the X-ray spectral and variability properties can be observed that are thought to reflect changes in the accretion geometry \citep[e.g.,][]{homan2005,vanderklis2006review,gladstone2007,munozdarias2014}. Broadly, the distinction is made between soft and hard X-ray spectral states, depending on the relative contributions of the soft X-rays emitted by the accretion disc and the hard X-rays produced by a corona (a population of hot electrons, the exact nature of which is not established) to the overall X-ray spectrum. Moreover, hard states show stronger variability, with lower characteristic frequencies, than soft states.

In the case of neutron stars, matter accumulates on the stellar surface where it undergoes thermonuclear burning that converts the accreted H/He into heavier elements \citep[e.g.,][for reviews]{lewin95,strohmayer06,schatz2006}. If radiative cooling of the burning layer is slower than the energy generation rate, a thermonuclear runaway occurs that causes the entire layer to ignite on a time-scale of $\simeq$1~s. This explosive energy release results in a bright burst of X-ray emission characterised by an initial fast rise due to the rapid burning of the fuel layer, followed by a slower decay phase as the burning ashes cool. Thousands of such type-I X-ray bursts (shortly X-ray bursts hereafter) have been observed from $\simeq$100 Galactic neutron star LMXBs \citep[e.g.,][]{cornelisse2003,galloway06}.

The spectra of X-ray bursts are blackbody-like with a temperature of $kT_{\mathrm{bb}}$$\simeq$1--3~keV that evolves over time. At the peak, the X-ray burst emission may exceed the Eddington limit ($L_{\mathrm{Edd}}\simeq2\times10^{38}~\mathrm{erg~s}^{-1}$), causing the photosphere of the neutron star to expand due to radiation pressure. Such photospheric radius expansion (PRE) can be identified through time-resolved spectroscopy as a peak in the blackbody emission area that is accompanied by a dip in the observed temperature \citep[e.g.,][]{lewin1993}.

It has long been realised that there is an intricate connection between the properties of the accretion flow and the observable manifestation of X-ray bursts. For example, the rate at which mass is accreted on to the neutron star determines the duration and recurrence time of X-ray bursts \citep[e.g.,][]{fujimoto81,bildsten98,cornelisse2003,peng2007}. Furthermore, the accretion geometry  influences the ignition conditions \citep[e.g.,][]{cavecchi2011,zand2012}, spectral evolution \citep[e.g.,][]{kajava2014,poutanen2014_4u1608}, and rapid variability \citep[e.g.,][]{muno2004,galloway06} of X-ray bursts.

In turn, the sudden and intense radiation caused by X-ray bursts can affect the surrounding accretion flow e.g., by cooling or ejecting the corona \citep[e.g.,][]{maccarone2003,kluzniak2013,mishra2014}, and exerting a drag on the accretion disc, driving a mass outflow from it, or changing its structure \citep[e.g.,][]{walker1989,miller1996,ballantyne2005}. Indeed, observational evidence has been accumulating that all these various effects occur. For example, hard (30--50 keV) flux deficits seen during X-ray bursts of several sources may be indicative of coronal cooling \citep[][]{maccarone2003,chen2012_xrbs_igrj1747,chen2013_aqlx1_bursts,ji2013_xrbs_4u1636,ji2014_bursts,ji2014_aa}. Furthermore, absorption and emission features detected during particularly long and intense X-ray bursts may point to a mass outflow or sudden changes in the accretion disc structure \citep[e.g.,][]{ballantyne2004,ballantyne2005,zand2011,degenaar2013_igrj1706,keek2014_refl}. Moreover, several recent studies suggest that the accretion emission is temporarily enhanced during X-ray bursts, possibly resulting from a radiation drag asserted on the inner accretion disc \citep[][]{intzand2013,worpel2013,worpel2015,ji2014_4u1608,keek2014,peille2014}.

All of the above physical processes are likely operating, possibly competing, during X-ray bursts. Given that hard and soft X-ray states are thought to reflect different accretion geometries, the impact of X-ray bursts is likely state dependent. Indeed, a reduction of the $>$30~keV emission is only seen for X-ray bursts occurring in the hard X-ray spectral state when the corona contributes most prominently to the overall X-ray spectrum \citep[][]{chen2012_xrbs_igrj1747,chen2013_aqlx1_bursts}. Furthermore, the enhancement of the accretion emission shows different patterns in the two different spectral states \citep[e.g.,][]{ji2014_4u1608}.

Studying accretion changes during an X-ray burst is somewhat challenging for soft X-ray states, because the accretion emission is then difficult to disentangle from the soft X-ray burst radiation \citep[e.g.,][]{barriere2014_grs,worpel2015}. On the other hand, during hard X-ray states both the accretion flux and the X-ray burst flux are typically lower, and hence good sensitivity is required to discern how a burst affects the accretion flow. In this work we exploit the excellent sensitivity of \textit{NuSTAR}\ up to an energy of $\simeq$79 keV, to study an X-ray burst from the neutron star LMXB 4U 1608--52, detected during a hard X-ray state in 2014 \citep[][]{degenaar2015_4u1608}.

\begin{figure}
 \begin{center}
\includegraphics[width=8.3cm]{figure1.pdf}
    \end{center}
\caption[]{{\textit{MAXI}/GSC (2--20 keV, black) and \textit{Swift}/BAT (15--50 keV, red) light curves of the outburst that started in 2014 October (5-d bins). The time of our \textit{NuSTAR}\ observation is indicated by the vertical dotted line. \\}}
 \label{fig:maxibat}
\end{figure}

\begin{figure*}
 \begin{center}
\includegraphics[width=8.0cm]{figure2a.pdf}\hspace{+0.2cm}
\includegraphics[width=8.0cm]{figure2b.pdf}
    \end{center}
\caption[]{{\textit{NuSTAR}\ FPMA/FPMB summed, background-corrected 3--79 keV count rate light curve (top panels) and 7--30 keV / 3--7 keV hardness ratio (bottom panels). The X-ray burst was cut out for representation purposes and is shown separately in Fig.~\ref{fig:lcE}; the time at which it occurred is indicated by the vertical grey bars. In the top panels the dashed black line indicates a linear decay fit to the overall light curve (i.e., using all satellite orbits). Left: the entire observation using 100 s bins for the light curve and 500 s bins for the hardness ratio. Right: zoom of \textit{NuSTAR}\ orbit 3, using 100 s bins for both the light curve and the hardness ratio. During this orbit the count rate evolution was better described by a linear function with a positive slope (red dashed line).
}}
 \label{fig:lc}
\end{figure*}

\subsection{4U 1608--52}
4U 1608--52\ is a prolific transient neutron star LMXB and X-ray burster. Since its discovery in 1972 \citep[][]{grindlay1976,tananbaum1976}, accretion outbursts have been observed roughly once every 1--2 years \citep[e.g.,][]{lochner1994,chen97,simon2004,galloway06}. Occasionally these outbursts are bright, reaching up to an X-ray luminosity of $L_{\mathrm{X}}$$\simeq$$(1-5) \times 10^{37}~(D/3.6~\mathrm{kpc})^2~\mathrm{erg~s}^{-1}$. However, more often the source exhibits fainter outbursts that peak at few times $10^{36}~(D/3.6~\mathrm{kpc})^2~\mathrm{erg~s}^{-1}$.

In addition to regular X-ray bursts, one superburst was detected from 4U 1608--52: A very long and energetic explosion thought to result from the ignition of a thick layer of carbon \citep[][]{keek2008}. Assuming that its brightest X-ray bursts reach the Eddington limit, a source distance of $D$$\simeq$2.9--4.5~kpc has been estimated \citep[e.g.,][]{galloway06,poutanen2014_4u1608}.\footnote{An alternative method based on interstellar extinction suggests a larger distance of $D=5.9^{+2.0}_{-1.9}$~kpc \citep[][]{guver2010}, although the X-ray burst behaviour favours a closer distance \citep[][]{poutanen2014_4u1608}.} The detection of burst oscillations has revealed the spin period of the neutron star \citep[$P_{\mathrm{s}}$$\simeq$620~Hz;][]{muno2001,galloway06}.

In 2014 October, \textit{MAXI}\ detected renewed activity from 4U 1608--52\ \citep[][see Fig.~\ref{fig:maxibat}]{negoro2014_4u1608}. An observation with \textit{NuSTAR}\ \citep[][]{harrison2013_nustar} performed shortly after the onset of this outburst revealed the characteristic signatures of disc reflection: a broad Fe-K line peaking near 7 keV and a Compton hump at $\simeq$20--30 keV \citep[][]{degenaar2015_4u1608}. The high data quality allowed us to constrain the accretion geometry in terms of the inner disc radius ($R_{\mathrm{in}}$$\simeq$7--10~$GM/c^2$), disc inclination ($i$$\simeq$$30^{\circ}$--$40^{\circ}$) and height of the corona ($h$$<$8.5$~GM/c^2$). The measured 3--79 keV unabsorbed flux was $F_{3-79}\simeq$$2\times10^{-9}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$, of which $>$95 per cent could be ascribed to a hard spectral component modelled by a $\Gamma \simeq 2$ power law with a high-energy cutoff of $E_{\mathrm{cut}}\gtrsim$300~keV. This spectral shape strongly suggests that 4U 1608--52\ was detected in a hard X-ray state during the \textit{NuSTAR}\ observation. Furthermore, it was accreting at a few per cent of the Eddington limit \citep[][]{degenaar2015_4u1608}. In this work we report on the detailed analysis of the X-ray burst that was detected during the \textit{NuSTAR}\ observation of 4U 1608--52.

\section{Observations and Analysis}
Fig.~\ref{fig:maxibat} shows the monitoring light curves of 4U 1608--52\ obtained with \textit{MAXI}/GSC \citep[2--20 keV;][]{maxi2009} and \textit{Swift}/BAT \citep[15--50 keV;][]{krimm2013}. We observed the source with \textit{NuSTAR}\ during the early part of the $\simeq$5-month long outburst (Fig.~\ref{fig:maxibat}), on 2014 October 16--17 from 23:00 to 17:10 UT (Obs ID 90002002002). \textit{NuSTAR}\ is sensitive at energies of 3--79 keV and consists of two co-aligned imaging telescopes, Focal Plane Mirror (FPM) A and B. The observation was spread over 12 different satellite orbits within a time frame of $\simeq 60$~ks, as illustrated in Fig.~\ref{fig:lc} (top left).

We reduced and analysed the \textit{NuSTAR}\ data using tools incorporated in \textsc{heasoft} version 16.6. Standard screening with \textsc{nustardas} resulted in a net on-source exposure time of $\simeq$32~ks. We created light curves and spectra with the \textsc{nuproducts} tool, using an aperture of 120 arcsec for the source and one of similar size for the background. The FPMA/FPMB light curves were background-corrected and summed using \textsc{lcmath}. 4U 1608--52\ was significantly detected above the background in the entire \textit{NuSTAR}\ band.

Since the spectra obtained with the two individual mirrors showed excellent agreement, we opted to combine the spectral data and ancillary response matrix files using \textsc{addascaspec}. The redistribution matrix files were combined with \textsc{addrmf}, where we weighted the responses of the two mirrors by their exposure times. All spectra were grouped to a minimum of 20 counts per bin and fitted using \textsc{XSpec} \citep[][]{xspec}. Throughout this work we use a distance of $D=3.6$~kpc towards 4U 1608--52\ and report errors as 1$\sigma$ confidence intervals unless noted otherwise.

\section{Results}\label{sec:results}

\subsection{Light curve analysis}\label{subsec:lc}

\subsubsection{Persistent accretion emission}\label{subsec:lcacc}
Fig.~\ref{fig:lc} shows the evolution of the persistent emission along the $\simeq$60-ks window during which 4U 1608--52\ was observed with \textit{NuSTAR}. An X-ray burst was detected during the third satellite orbit (grey shaded area in Fig.~\ref{fig:lc}), which is shown in Fig.~\ref{fig:lcE}. During the observation, the FPMA/FPMB summed count rate of the persistent (i.e., non-burst) accretion emission decreased by $\simeq$25 per cent from $\simeq$75$~\mathrm{counts~s}^{-1}$ at the start of the observation to $\simeq$55$~\mathrm{counts~s}^{-1}$ at the end. Making energy cuts shows that the decay is visible for energies up to $\simeq$30 keV; the count rate in the 30--79 keV band is consistent with being constant along the observation. Defining a hardness ratio as the ratio of counts in the 7--30 and 3--7 keV ranges suggests that there are no prominent spectral changes associated with the decay in count rate (Fig.~\ref{fig:lc} bottom left).

The overall light curve, excluding the X-ray burst, can be reasonably described by a simple linear function of the form $f(t)$$=$$a$$+$$bt$ where $t$ is the time since the start of the \textit{NuSTAR}\ observation. We obtain a constant offset of $a$$=$$71.89 \pm 0.11~\mathrm{counts~s}^{-1}$ and a slope of $b$$=$$-(2.55 \pm 0.03)\times10^{-4}$~counts~s$^{-2}$ ($\chi_{\nu}^2$=1.50 for 749 dof). This fit is shown as the dashed line in Fig.~\ref{fig:lc}. Individual satellite orbits could be described by decay slopes lying within $\simeq$3$\sigma$ of the value obtained for the overall light curve, as shown in Fig.~\ref{fig:linfit}. The exception is orbit 3, which is best fit with a positive slope of $b$$=$$(1.02 \pm 0.18)\times10^{-3}$~counts~s$^{-2}$ ($a$$=$$60.08 \pm 1.93~\mathrm{counts~s}^{-1}$, $\chi_{\nu}^2$=0.73 for 65 dof) and lies $\simeq$7$\sigma$ from the overall value (Fig.~\ref{fig:linfit}). Fig.~\ref{fig:lc} (top right) shows that the count rate started to rise $\simeq$1~ks into the observation, which was $\simeq$1.5~ks ($\simeq$0.5~h) before the X-ray burst detection (it is unclear whether there is a connection; see Section~\ref{subsec:persenhance}). The count rate increased by $\simeq$3 per cent and there appears no change in hardness associated with it (Fig.~\ref{fig:lc}, bottom right).

\subsubsection{Burst emission}\label{subsec:lcburst}
Fig.~\ref{fig:lcE} shows the light curve of the X-ray burst in different energy bands at 1-s resolution. The burst was detected up to $\simeq$30 keV. The inset in Fig.~\ref{fig:lcE} shows a zoom of the 30--79 count rate light curve at 10-s resolution. The 30--79 keV count rate is zero during a single bin around the X-ray burst peak, and there seems to be a small reduction in the 15--30 keV count rate at this time (dotted vertical line). However, the error bars are large and this possible `dip' is not significant.

The pre-burst 3--79 keV count rate was $\simeq$70~$\mathrm{counts~s}^{-1}$ (Fig.~\ref{fig:lc}) and the source returned to this level $\simeq$210~s after the start of the X-ray burst. We note that the duration of X-ray bursts depends strongly on the energy band considered. This is illustrated by Fig.~\ref{fig:lcE}, which shows that the X-ray burst decayed more rapidly at higher energies. This behaviour is typical and results from the gradual decrease in temperature as the burning ashes cool along the burst decay. The X-ray burst peaked $\simeq$10~s after the initial rise.

\begin{figure}
 \begin{center}
\includegraphics[width=8.3cm]{figure3.pdf}\hspace{+0.2cm}
    \end{center}
\caption[]{{\textit{NuSTAR}\ FPMA/FPMB summed, background-corrected count rate light curve of the X-ray burst in different energy bands (1-s bins). The inset shows the 30--79 keV light curve at 10-s resolution. The 15--30 keV count rates were multiplied by a factor of 5 for visual clarity.} The vertical dotted line marks the time of the X-ray burst peak and the dashed horizontal line the average 3--79 keV count rate over the entire observation.}
 \label{fig:lcE}
\end{figure}

\begin{figure}
 \begin{center}
\includegraphics[width=8.0cm]{figure4.pdf}\hspace{+0.2cm}
    \end{center}
\caption[]{{Values for the index of a linear fit to the count rate light curve for each individual satellite orbit, where $b$$<$0 indicates a decreasing intensity. The average value obtained from fitting the entire \textit{NuSTAR}\ light curve (i.e., all 12 orbits; Fig.~\ref{fig:lc}) is indicated by the dashed line. The X-ray burst occurred during \textit{NuSTAR}\ orbit 3, and was cut from the data for these fits. Errors are 1$\sigma$.
}}
 \label{fig:linfit}
\end{figure}

\subsection{Time-resolved spectroscopy of the X-ray burst}\label{subsec:spec}
To investigate the spectral evolution during the X-ray burst, we selected 14 consecutive intervals of varying length ($\simeq$2--65~s) to ensure $\simeq$1800~counts per spectrum. For all burst intervals, a spectrum created from $\simeq$100~s of data preceding the burst was subtracted as the underlying accretion emission. To model the burst we used a simple blackbody model (\textsc{bbodyrad}) and to account for interstellar extinction we employed the \textsc{tbabs} model with the abundances set to \textsc{wilm} \citep[][]{wilms2000}, and the cross-sections to \textsc{vern} \citep[][]{verner1996}. Once a best fit was found, we calculated the bolometric flux using the \textsc{cflux} convolution model with the energy boundaries set to 0.01 and 100 keV.
Due to the energy cut-off at 3~keV, the hydrogen column density is not well constrained by the \textit{NuSTAR}\ data. We therefore fixed it to $N_{\mathrm{H}}$$=$$1.5\times10^{22}~\mathrm{cm}^{-2}$, which is within the range of values reported for 4U 1608--52\ \citep[$N_{\mathrm{H}}\simeq$$(1-2)\times10^{22}~\mathrm{cm}^{-2}$; e.g.,][]{penninx1989,keek2008_1608,guver2010,degenaar2015_4u1608}.

The black histograms in Fig.~\ref{fig:resolvedspec} show the results of our time-resolved spectroscopy. The bolometric flux peaks $\simeq$10~s after its initial rise, the measured blackbody temperatures are $kT_{\mathrm{bb}}$$\simeq$1.2--2.2~keV, and the  emission radii inferred from the blackbody normalisation are $R_{\mathrm{bb}}$$\simeq$4--7~km (for $D$$=$3.6~kpc). From our time-resolved spectroscopy we estimate a total fluence of $f_{\mathrm{bol}}$$\simeq$$1\times10^{-6}~\mathrm{erg~cm}^{-2}$. Half of this is radiated during the first $\simeq$20~s of the burst. For $D$$=$3.6~kpc, the total radiated energy is $E_{\mathrm{burst}}$$\simeq$$1\times10^{38}$~erg. We find that the burst reached a peak flux of $F_{\mathrm{bol}}$$\simeq$$5.6\times10^{-8}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$, which is a factor of $\simeq$15 higher than the pre-burst accretion emission. The Eddington flux of 4U 1608--52\ is not well measured: PRE bursts show a spread in bolometric peak flux of $F_{\mathrm{bol}}$$\simeq$(1.0--1.9)$\times10^{-7}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$, which appears to depend on the accretion state \citep[e.g.,][]{kajava2014,poutanen2014_4u1608}. This suggests that the \textit{NuSTAR}-detected X-ray burst peaked at $\simeq$30--50 per cent of the Eddington limit. The main burst properties are summarised in Table~\ref{tab:burst}.

\subsubsection{Allowing the persistent emission to vary during the burst}
In the standard approach outlined above we implicitly assume that the accretion emission is constant during an X-ray burst, but recent studies suggest that this might not be true \citep[e.g.,][]{intzand2013,worpel2013,worpel2015,ji2014_4u1608,keek2014}. We therefore repeated our spectral analysis by only subtracting the instrument background and then modelling the persistent emission together with the burst, as proposed by \citet{worpel2013}.

Analysis of the time-averaged accretion spectrum revealed a power-law like shape with no evidence for a spectral cutoff in the \textit{NuSTAR}\ bandpass \citep[][]{degenaar2015_4u1608}. We therefore use the \textsc{pegpwrlw} model for the accretion emission, the normalisation of which gives the unabsorbed model flux in a specified energy band (we choose 3--79 keV). A spectrum extracted from $\simeq$100~s prior to the X-ray burst can be described by $\Gamma$$=$$2.16\pm0.04$, and an unabsorbed 3--79 keV flux of $F_{3-79}$$=$$(2.16\pm0.07)\times10^{-9}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$ (for $N_\mathrm{H}$$=$$1.5\times10^{22}~\mathrm{cm}^{-2}$ fixed; $\chi_{\nu}^{2}=1.12$ for 104 dof). We fixed the \textsc{pegpwrlw} parameters to these values and then modelled the burst plus accretion emission as \textsc{tbabs*(bbodyrad+constant*pegpwrlw)}, where the constant factor ($f_a$) is introduced to parametrize changes in the accretion flux. The accretion emission was thus only allowed to change in normalisation, not in shape. Leaving the power-law index free resulted in very large errors, which indicates that we cannot address any possible changes in the shape of the spectral emission.

The results of allowing the persistent emission to change are shown as the red histograms in Fig.~\ref{fig:resolvedspec}. Overall, this provides a better fit to the burst spectra than keeping it fixed to the pre-burst value (fourth panel in Fig.~\ref{fig:resolvedspec}). This is also illustrated by Fig.~\ref{fig:spec}, which compares a spectrum taken $\simeq$35~s along the burst tail and fitted using the two different methods. When subtracting a pre-burst spectrum and fitting a blackbody to the burst (black curve in Fig.~\ref{fig:spec}), the model underestimates the data at $\gtrsim$15~keV. These residuals disappear when the persistent emission is allowed to vary in normalisation (red curve in Fig.~\ref{fig:spec}). We find that the constant multiplication factor is $f_{\mathrm{a}}$$>$1 during the larger part of the X-ray burst (bottom panel in Fig.~\ref{fig:resolvedspec}). It reached a maximum of $f_{\mathrm{a}}$$\simeq$5 around the burst peak, after which it gradually decreased and settled at $f_{\mathrm{a}}$$\simeq$1 around $\simeq$100~s after the start of the burst. This suggests that the accretion emission was temporarily enhanced in response to the X-ray burst.

\begin{table}
\caption{X-ray burst properties.}
\begin{threeparttable}
\begin{tabular*}{0.49\textwidth}{@{\extracolsep{\fill}}lc}
\hline
Parameter (unit)  & Value \\
\hline
Total duration, $t_{\mathrm{b}}$ (s)  & $\simeq 210$  \\
Total fluence, $f_{\mathrm{tot}}$ ($\mathrm{erg~cm}^{-2}$)  & $\simeq 1.0 \times 10^{-6}$   \\
Radiated energy, $E_{\mathrm{b}}$ (erg)  & $\simeq 1.2 \times 10^{38}$   \\
Bolometric peak flux, $F_{\mathrm{bol}}$ ($\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$)  & $\simeq 5.6 \times 10^{-8}$   \\
Accretion flux, $F_{\mathrm{acc}}$ ($\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$)  & $\simeq 4 \times 10^{-9}$ \\
\hline
\end{tabular*}
\label{tab:burst}
\begin{tablenotes}
\item[] {\it Notes.} The bolometric (unabsorbed) peak flux is for the 0.01--100 keV energy range. A distance of $D=3.6$~kpc was assumed to calculate the total energy radiated during the X-ray burst. For reference, we note that the bolometric peak flux measured during PRE bursts of 4U 1608--52\ suggests that the Eddington flux lies in a range of $F_{\mathrm{Edd}}$$\simeq$$(1.0-1.9)\times10^{-7}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$ \citep[e.g.,][]{kajava2014,poutanen2014_4u1608}.
\end{tablenotes}
\end{threeparttable}
\end{table}

\begin{figure}
 \begin{center}
\includegraphics[width=8.9cm]{figure5.pdf}
    \end{center}
\caption[]{{Results from time-resolved spectroscopy of the X-ray burst. In black the standard analysis in which a pre-burst persistent emission spectrum is subtracted from the burst spectra. In red an alternative method in which the persistent flux was allowed to vary during the burst by a factor $f_{a}$. From top to bottom: the bolometric thermal flux (0.01--100 keV), the blackbody temperature and normalisation, the reduced chi-square value of the fits, and the constant multiplication factor $f_{a}$.
}}
 \label{fig:resolvedspec}
\end{figure}

\begin{figure}
 \begin{center}
\includegraphics[width=8.0cm]{figure6.pdf}
    \end{center}
\caption[]{{\textit{NuSTAR}\ FPMA/FPMB combined spectrum and model fit (top panel), and data to model ratio (bottom panel) of an interval during the X-ray burst tail. In black the standard method where a spectrum of the pre-burst accretion emission is subtracted for the burst analysis. In red an alternative approach in which only the instrumental background is subtracted and the persistent emission is modelled to allow for changes in its normalisation. Dashed curves indicate the burst (blackbody) emission, and the dotted curve the accretion (power law) emission.}}
 \label{fig:spec}
\end{figure}

\subsection{Unsupervised spectral decomposition of the X-ray burst}\label{subsec:nmf}
Our spectral analysis presented in Section~\ref{subsec:spec} suggests that the accretion flux was enhanced during the X-ray burst. Since the intense X-ray burst emission may change the structure of the accretion disc or cool the corona \citep[e.g.,][]{maccarone2003,ballantyne2005}, it would not be surprising if the spectral shape of the persistent emission changed as well. However, the quality of the spectral data did not allow us to investigate this.

Moving beyond conventional spectral fitting, unsupervised spectral decomposition methods have proven a powerful tool to map out the spectral variability of both supermassive and stellar-mass black holes \citep[][]{mittaz1990,vaughan2004,malzac2006,koljonen2013,parker2015}. For example, a study of the black hole LMXB GX 339--4 demonstrated how different emission components can be successfully disentangled and can reveal variations in the accretion disc in a regime where the disc flux is too low to be tracked by conventional spectral analysis \citep[][]{koljonen2015}. This is not unlike the situation for X-ray bursts, where the emission of the accretion flow is swamped by that of the burst. This motivated us to investigate the applicability of such techniques for X-ray burst studies.

The aim of unsupervised decomposition methods is to find the minimum number of components that can together describe most of the physically interesting variability that is present in the data (in order words, it is an attempt to identify hidden structure in complex data). This can be achieved by using a mathematical approach in which the data are described as matrices. In this work we chose non-negative matrix factorisation \citep[NMF;][]{paatero1994,lee1999} as our spectral decomposition method, which was found to be most successful in disentangling different spectral components in the study of GX 339--4 \citep[][]{koljonen2015}. We briefly describe the NMF technique below for our specific application, but for general details the reader is referred to \citet{koljonen2015}.

\subsubsection{NMF analysis}
The input for the NMF analysis is a data matrix composed of collection of discrete X-ray spectra \textsf{\textbf{X$_{ij}$}}, each consisting of counts detected in an energy bin $j$, measured at time $i$. Here we chose to divide the X-ray burst in equal time steps of 10 s to strike a balance between having a sizeable sample of spectra, but at the same time maintaining a sufficient number ($>$500) of counts per interval. This resulted in $i$$=$21 time-resolved spectra covering energies of 3--20 keV. Each of these spectra were then divided into $j$$=$25 energy slices with bin widths of 0.4--1.2~eV to ensure a positive flux in each energy bin. The NMF method then decomposes this input data matrix as $k$ separate source signals \textsf{\textbf{S$_{ki}$}} that are weighted over the energy bands as \textsf{\textbf{W$_{jk}$}}, such that the spectra are described as \textsf{\textbf{X}}$\approx$\textsf{\textbf{WS}}. The matrices \textsf{\textbf{S}} and \textsf{\textbf{W}} thus approximate the input collection of spectra \textsf{\textbf{X}}, and can be thought of as a spectral component (\textsf{\textbf{W}}, weights across energy bands) and its amplitude (\textsf{\textbf{S}}, signal).

The source signal and the weight matrix that decompose the collection of input spectra are found by minimising a cost function under the constraint that they must be non-negative. To calculate the standard NMF \citep[][]{brunet2004}, we use the NMF package \citep[][]{gaujoux2010} that picks random starting values for \textsf{\textbf{S}} and \textsf{\textbf{W}} from a uniform distribution with values [0,max(\textsf{\textbf{X}})]. Using a multiplicative rule from \citet{lee2001}, the starting values are updated iteratively 10\,000 times to find a local minimum of the cost function. To avoid biases against local minima, we repeated the process for 300 different starting points.

The first step is to find the number of significant components $k$ that are needed to explain the variability in the data, i.e., the degree of factorisation. Statistical and systematic noise will give rise to components that are not related to physically interesting variations and therefore need to be filtered out. To achieve this, we use the $\chi^2$-diagram method outlined in \citet{koljonen2015}. This diagram provides a quality measure of how well a factorisation describes the data, and allows to reduce the number of components to only those ones that vary above the noise level. The choice for $k$ should be a knee in the diagram close to a value of $\chi^2=1$, where the slope changes from steep (increasing $k$ gives a large improvement) to more shallow (further increasing $k$ does not yield a large change in $\chi^2$ any more). Fig.~\ref{fig:chi} shows the $\chi^2$-diagram for our set of spectra. In this case we identify $k = 4$ as the position where adding more components does not decrease $\chi^2$ strongly, and therefore chose that as the number of significant components.

\begin{figure}
 \begin{center}
\includegraphics[width=8.5cm]{figure7.pdf}
    \end{center}
    \vspace{-0.2cm}
\caption[]{{Quality measure of how well a certain factorisation ($k$) in the NMF analysis describes the data. This provides means to separate the significantly varying components from noise. We identify $k$$=$4 (see arrow) as the position where adding more components does not decrease $\chi^2$ strongly, and therefore chose that as the number of significant components.}}
 \label{fig:chi}
\end{figure}

\begin{figure}
 \begin{center}
\includegraphics[width=8.5cm]{figure8.pdf}
    \end{center}
        \vspace{-0.2cm}
\caption[]{{Results of the NMF analysis. The top four panels show how the significant components evolve over time (each time step $i$ represents 10 s), and lower panel shows their energy distribution (the energy slices $j$ have widths of 0.4--1.2 keV). Based on the strength of the source signals (\textsf{\textbf{S$_{ki}$}}) and the curvature of the energy spectra (\textsf{\textbf{W$_{jk}$}}) we identify the $k$=1,4 components with the accretion emission, and $k$=2,3 with the burst emission.}}
 \label{fig:nmf}
\end{figure}

We thus performed the NMF analysis assuming $k$=4 significant components, the results of which are shown in Fig.~\ref{fig:nmf}. The top four panels show how the amplitude of each NMF component changes over time, and their energy distribution is shown in the bottom panel. Note that the numbering of the components is random and does not reflect any particular order. The $k$=1 and $k$=4 components have a flat energy spectrum and a relatively weak signal, whereas the $k$=2 and $k$=3 components are characterised by a curved energy spectrum and a stronger signal. It is therefore likely that the $k$=1 and $k$=4 components are linked to the accretion emission, and the $k=$2 and $k=$3 components to the burst emission. The fact that there are two components for both the accretion flow and the burst emission, suggests that both do not only vary in normalisation but also in spectral shape.

\subsubsection{Reconstruction of spectra from the NMF analysis}
The summed signals accurately describe the fluxes of the spectral components, but we do not expect a one-to-one correspondence between the individual NMF components and the spectral parameters (i.e., we cannot simply identify $k$=1 as the power-law index for instance). This is because the NMF is a linear technique and a varying power law index or blackbody temperature introduces non-linear effects \citep[e.g.,][]{mittaz1990}. However, we can assign physical meaning to the different emission components, and track the evolution of individual spectral parameters, by re-constructing spectra for each time interval from the NMF components as \textsf{\textbf{X$_{\mathrm{pow}}$}}$=\Sigma_{k=1,4}$\textsf{\textbf{W$_{jk}$}}$\times$\textsf{\textbf{S$_{ki}$}} and \textsf{\textbf{X$_{\mathrm{bb}}$}}$=\Sigma_{k=2,3}$\textsf{\textbf{W$_{jk}$}}$\times$\textsf{\textbf{S$_{ki}$}}. Fitting these NMF-built spectra (i.e., that have reduced dimensionality) in \textsc{XSpec} reveals that those constructed from the $k$=1,4 components can indeed be fitted by a power law with an index of $\Gamma$$\simeq$2, consistent with the pre-burst accretion emission. The spectra build from the NMF components $k$=2,3 can be fitted by a blackbody with a temperature of $kT_{\mathrm{bb}}$$\simeq$1--2~keV, as expected for an X-ray burst (Section~\ref{subsec:spec}).

Fig.~\ref{fig:nmfspec} shows our time-resolved analysis of the spectra constructed through the NMF. This sketches a similar picture as found from our conventional spectral analysis (Section~\ref{subsec:spec}): The burst emission (black histograms) peaks $\simeq$10~s after the initial rise, and can be described by a blackbody with a temperature varying between $kT_{\mathrm{bb}}$$\simeq$1.2 and 2.1~keV, and an inferred emission radius of $R_{\mathrm{bb}}$$\simeq$1--6~km (for $D$$=$3.6~kpc). This demonstrates that the NMF successfully reduced the data to its most significant components and is still able to accurately describe the evolution of the burst emission (i.e., retaining the most relevant information). In addition, the NMF allows us to resolve changes in the accretion emission (red histograms in Fig.~\ref{fig:nmfspec}).

\subsubsection{Possible change in the accretion spectrum}
As can be seen from the top panel in Fig.~\ref{fig:nmfspec}, the accretion flux appears enhanced compared to the pre-burst level (dashed line) until $\simeq$100~s into the burst. For comparison with our conventional spectral analysis, we divide the power-law flux during the burst by the pre-burst value ($F_{\mathrm{3-79}} = 2 \times 10^{-9}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$; Section~\ref{subsec:spec}), to determine the constant multiplication factor $f_a$. This quantity is plotted in the bottom panel of Fig.~\ref{fig:nmfspec} and shows similar behaviour as inferred in Section~\ref{subsec:spec}: $f_a$ reaches a maximum value of several times the pre-burst level around the burst peak and returns to a value of $f_a$$\simeq$1 after $\simeq$100~s. The NMF analysis suggests that, in addition, the power-law slope is variable. It attends a value of $\Gamma$$\simeq$1.9 at the start (first 10-s spectrum) and end ($t$$>$100~s) of the X-ray burst, but is increased to $\Gamma$$\simeq$2.3 in between, except for a single low point with $\Gamma$$\simeq$1.6. This could indicate that the accretion emission softened in response to the X-ray burst.

To investigate whether similar variability in the power-law slope is seen in the absence of a burst, we investigated a series of spectra extracted from an interval of $\simeq$200--700~s prior to the burst. We choose 25-s time steps to achieve an approximately similar number of counts per spectrum as for the burst spectra. The power-law indices inferred from fitting these 21 spectra with a simple power law (with $N_H$$=$$1.5\times10^{22}~\mathrm{cm}^{-2}$ fixed) is shown in Fig.~\ref{fig:preburstspec}. The index varied irregularly between a minimum/maximum value of $\Gamma=1.9/2.3$ with typical errors of $\pm0.2$ (90 per cent confidence). This is not unlike the variability seen during the X-ray burst. Therefore we cannot conclusively ascribe the apparent softening as being due to the X-ray burst rather than random variations.

\begin{figure}
 \begin{center}
\includegraphics[width=8.0cm]{figure9.pdf}
    \end{center}
    \vspace{-0.2cm}
\caption[]{{Analysis of the NMF-constructed spectra. Burst emission is indicated by black histograms, and accretion emission by red histograms. From top to bottom: the 3--20 keV flux, the blackbody temperature and normalisation, the power-law index, and the constant multiplication factor for the persistent flux $f_{a}$. In the plot for the power-law index the dashed horizontal line corresponds to the value inferred from the first interval. Errors represent 90 per cent confidence intervals here.}}
 \label{fig:nmfspec}
\end{figure}

\begin{figure}
 \begin{center}
\includegraphics[width=8.0cm]{figure10.pdf}
    \end{center}
    \vspace{-0.2cm}
\caption[]{{Power-law indices inferred from fitting 21 spectra of $\simeq$25-s length obtained from an interval of $\simeq$200--700~s prior to the X-ray burst. The spread in $\Gamma$ values is not unlike that seen in the fourth panel in Fig.~\ref{fig:nmfspec}, which indicates that the observed changes during the X-ray burst could be due to random variations. Errors are 90 per cent confidence intervals here.
}}
 \label{fig:preburstspec}
\end{figure}

\section{Discussion}\label{sec:discussion}
We report on the detection of a type-I X-ray burst during a \textit{NuSTAR}\ observation of the neutron star LMXB 4U 1608--52. The burst had a
duration of $t_{\mathrm{burst}}$$\simeq$200~s, a relatively low peak flux of $F_{\mathrm{peak}}$$\simeq$0.3--0.5$~F_{\mathrm{Edd}}$, and a total radiated energy of $E_{\mathrm{rad}}$$\simeq$$1\times 10^{38}~$erg. Detailed analysis of the non-burst emission revealed that the burst occurred during a hard X-ray spectral state, with the neutron star accreting at a few per cent of the Eddington limit \citep[][]{degenaar2015_4u1608}.

\vspace{-0.4cm}
\subsection{Enhancement of the persistent emission}\label{subsec:persenhance}
The fact that 4U 1608--52\ was in a hard X-ray spectral state made it possible to address whether the accretion emission was altered by the intense X-ray burst emission. We performed time-resolved spectroscopy of the burst and the underlying accretion emission, where we allowed the latter to change in flux. Despite that the burst was not very long, bright, or energetic, we found that the accretion flux was enhanced by a factor of $\simeq$5 during the peak of the X-ray burst and returned to its pre-burst level after $\simeq$100~s. Such enhancements have been detected in a large number of bursts from many different sources, both during hard and soft X-ray spectral states, and both for PRE and non-PRE bursts \citep[][]{intzand2013,worpel2013,worpel2015,ji2014_4u1608,ji2015_gs1862,peille2014}.

The burst-accretion interaction is complex, but the increase of the persistent emission during bursts has been associated with the Poynting-Robertson drag, in which transfer of momentum by the burst photons reduces the angular momentum of the inner accretion disc, hence allowing more matter to fall towards the neutron star and enhance the accretion rate \citep[e.g.,][]{walker1992}. For 4U 1608--52, analysis of the reflection spectrum revealed that the inner accretion disc resided close to the neutron star \citep[$R_{\mathrm{in}}$$\simeq$7--10~$GM/c^2$;][]{degenaar2015_4u1608}, so this seems a viable explanation for the observed enhancement in accretion flux. We note that studies of the rapid time variability in 4U 1608--52 suggested (small) changes in the inner accretion disc radius in response to nuclear burning on the neutron star surface \citep[][]{yu2002}, which may fit in with this picture. Reprocessing of burst photons by the accretion disc or corona could possibly also enhance the accretion emission during an X-ray burst \citep[e.g.,][]{ballantyne2005,intzand2013}.

Apart from changes in the accretion flux {\it during} the X-ray burst, we observed a small ($\simeq$3 per cent) increase in intensity that started $\simeq$0.5~h \textit{prior} to the X-ray burst detection. Such a rise was not seen during any of the other \textit{NuSTAR}\ orbits, which instead showed the count rate to gradually decrease over time. An enhanced accretion flux was also reported prior to three superbursts \citep[][]{kuulkers2002,chenevez2011_superburst,keek2014}. For two of these, the accretion emission remained enhanced directly after a normal X-ray burst was ignited, $\simeq$0.5~h before the superburst. The enhanced emission could therefore be related to the neutron star surface remaining hot after the normal burst. For 4U 1608--52, there was a data gap of $\simeq$2.3~ks before the satellite orbit in which the enhancement was observed, so a prior X-ray burst could have been missed. However, it seems that the accretion emission was not enhanced right from the start of this orbit, but began to rise only $\simeq$1~ks into the observation. Arguably, an association with a missed X-ray burst therefore seems unlikely.

\vspace{-0.4cm}
\subsection{Possible change in the shape of the accretion spectrum}\label{subsec:shapechange}
The intense radiation from an X-ray burst may clear, or change the shape of, the inner accretion disc \citep[see e.g.,][for a discussion of various possible effects]{ballantyne2005}. Furthermore, the presence of a corona (a hot population of electrons) can cause burst photons to Compton up-scatter and hence produce a high-energy emission tail. In turn, the burst photons may be able to efficiently cool or even eject the corona \citep[e.g.,][]{maccarone2003,kluzniak2013,ji2015_gs1862}. Therefore, it seems reasonable to expect that an X-ray burst does not only change the flux, but also the spectral shape of the accretion emission.

Conventional time-resolved spectroscopy of the burst did not allow us to address whether the shape of the accretion emission was changing along with its flux. However, we were able to address this in more detail by using an unsupervised spectral decomposition method, in which the data are reduced to only the most significantly varying components \citep[e.g.,][]{koljonen2015}. This way we found that the accretion emission possibly softened during the X-ray burst. However, investigating short ($\simeq$25~s) time slices of the accretion emission prior to the X-ray burst showed changes of similar magnitude. Therefore, we cannot exclude random variations as the cause of the apparent softening. Nevertheless, it is suggestive that the power-law index was increased during several consecutive intervals around the burst peak and returned to the pre-burst level at the same time as the accretion flux settled back to its pre-burst value. Therefore, it is interesting to explore the physical interpretation of the possible softening of the accretion emission.

\citet{keek2014} reported changes in the spectral shape of the accretion emission during a (non-PRE) superburst from 4U 1636--536. It was found that the persistent emission increased by a factor of $\simeq$1.8, and that the cut-off energy decreased from $\simeq$20 to 10~keV during the X-ray burst. This may be interpreted as cooling of the corona by the injection of the soft burst photons \citep[][]{keek2014}. In case of 4U 1608--52, there was no detectable high-energy cutoff in the non-burst accretion emission \citep[][]{degenaar2015_4u1608}. However, the possible softening of the power-law index might indicate the same physical process.

Cooling of the corona has also been invoked to explain the hard X-ray ($>$30~keV) deficits seen when stacking hard state bursts of a number of sources \citep[][]{chen2012_xrbs_igrj1747,chen2013_aqlx1_bursts,ji2013_xrbs_4u1636,ji2014_bursts,ji2014_aa}. In case of 4U 1608--52, we did not find such a deficit in the 30--79~keV light curve during the \textit{NuSTAR}-detected X-ray burst. A stacking study of a large sample of X-ray bursts detected from 4U 1608--52\ with \textit{RXTE}\ did not reveal a hard X-ray deficit either \citep[][]{ji2014_aa}. Such a deficit may be absent if the corona is far away, or if the hard X-ray source is in fact an equatorial boundary/spreading layer on the neutron star surface \citep[e.g.,][]{kluzniak1991,inogamov1999,popham2001}, so that most of the burst flux does not pass through the ``corona'' and therefore does not result in notable cooling. Detailed analysis of the \textit{NuSTAR}\ reflection spectrum revealed a compact corona with a height of only $h$$<$8.5~$GM/c^2$ above the neutron star, which may favour the boundary layer scenario. However, given the low count rate at $\gtrsim$30~keV, sensitivity limits may have prevented us from detecting a high-energy deficit during the burst.

Since the increase in power-law index (i.e., possibly representing cooling) persisted as long as the accretion emission was enhanced, one may wonder whether cooling of the corona due to an X-ray burst could condense matter back on the disc and thereby temporarily enhance the accretion rate. We can roughly estimate the mass-accretion rate on to the neutron star in 4U 1608--52\ from the average persistent flux measured by \textit{NuSTAR}\ ($F_{\mathrm{3-79}}$$\simeq$$2 \times 10^{-9}~\mathrm{erg~cm}^{-2}~\mathrm{s}^{-1}$). Assuming a bolometric correction factor of $\simeq$2, this suggests $L_{\mathrm{bol}}$$\simeq$$6\times 10^{36}~(D/3.6~\mathrm{kpc})^2~\mathrm{erg~s}^{-1}$ and $\dot{M}$=$LR/GM$$\simeq$$3\times10^{16}~\mathrm{g~s}^{-1}$ (where $G$ is the gravitational constant and $M$$=$$1.4~\mathrm{M}_{\odot}$ and $R$$=$$10$~km are the adopted mass and radius of the neutron star, respectively). If we take the accretion rate to be enhanced by a factor $\simeq$2 on average for a duration of $\simeq$100~s, this suggests that $\simeq$$7\times10^{18}$~g ($\simeq$$3\times10^{-15}~\mathrm{M}_{\odot}$) of additional mass was accreted in response to the X-ray burst.

If the corona is spherical with a radius of $\simeq$10~km and a surface density of $\simeq$$10^{24}~\mathrm{g~cm}^{-2}$ (corresponding to the Thomson optical depth of the corona of $\tau$$\simeq$1), this would imply a total number of $\simeq$$3\times10^{36}$~particles or $\simeq$$5\times10^{12}$~g (for a proton mass of $1.67\times10^{-24}$~g). This falls short by orders of magnitude of our simple estimate above. Therefore, there was likely not enough mass in the corona to account for (all of) the additional matter that was accreted during the X-ray burst.

We note that the above discussion is based on the assumption that the burst emission can be well-approximated by a pure blackbody. If the spectrum is harder, as may be expected due to atmospheric effects \citep[e.g.,][]{foster1986}, we might see the persistent emission compensating for this in our model fits by getting softer. However, deviations from a blackbody are expected to be strongest near the Eddington flux \citep[e.g.,][]{suleimanov2011}, whereas this burst peaked below $\simeq$50 per cent of the Eddington limit. Realistic atmosphere models for X-ray bursts are complex, hence complicating spectral fitting, and do not yield better fits to the data than a blackbody \citep[e.g.,][]{intzand2013,keek2014}.

\vspace{-0.2cm}
\subsection{The prospects of \textit{NuSTAR}\ and NMF for burst studies}\label{subsec:prospects}
Due to the hard X-ray spectrum of 4U 1608--52, \textit{NuSTAR}\ proved very valuable to disentangle the accretion and burst emission. Moreover, a strong aspect of \textit{NuSTAR}\ is that it provides excellent reflection spectra that can place strong constraints on the accretion geometry in X-ray binaries, such as the location of the inner accretion disc and the corona \citep[e.g.,][]{fuerst2015,miller2015,parker2015}. Analysis of the \textit{NuSTAR}\ reflection spectrum of 4U 1608--52\ was presented in \citet{degenaar2015_4u1608}. As discussed in Section~\ref{subsec:shapechange}, these tight constraints on the accretion geometry  provide valuable information for interpreting the effect of X-ray bursts on the accretion emission.

The quality of current data does not allow us to detect changes in the accretion emission during bursts via spectral analysis \citep[see also][]{worpel2015}, except in special cases \citep[][]{keek2014}. Applying unsupervised spectral decomposition methods can possibly provide more insight into this. Our NMF analysis of the burst of 4U 1608--52\ proved that the method was successful in disentangling the accretion emission from that of the burst. The evolution of the burst emission inferred from the NMF yielded similar results to that found in conventional spectral fitting. In addition, it allowed to better resolve changes in the accretion emission. Applying NMF or similar methods to a larger sample of X-ray bursts may be a promising avenue to gain further insight into the burst-accretion interaction, even before the launch of future X-ray missions.

\vspace{-0.5cm}
\section*{Acknowledgements}
ND acknowledges support via an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2013-IEF-627148.  DA is supported by the Royal Society. This work is based on data from the \textit{NuSTAR}\ mission, a project led by California Institute of Technology, managed by the JPL, and funded by NASA. We made use of \textit{MAXI}\ data provided by RIKEN, JAXA and the MAXI team, and publicly available light curves from the \textit{Swift}/BAT transient project. The authors are grateful to the anonymous referee for valuable comments that helped improve this manuscript.

\vspace{-0.5cm}
\footnotesize{

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Today air conditioning product and applications designers, as a result of climate change contribution concerns for high direct global warming potential (GWP) refrigerants, are being asked to consider lower GWP refrigerants with various degrees of flammability. In recent year, the HVACR industry has been actively investigating the safety of flammable refrigerants by determining their risks, potential occurrences and severity of events. Today R410A is used to cover most air conditioning applications and all lower GWP alternatives presented to date have some degree of flammability with most being ASHRAE 34 flammability class 2L.  A novel R410A alternative refrigerant blend, R452B or DR55, has recently been studied in a 4 ton RTU to determine the potential for compositional fractionation in various modes of operation. In addition, the ASHRAE flammability process needed to classify refrigerant flammability and flammability classification data for R452B will be presented in this paper. The unit compositional data and the ASHRAE classification process and data will be compared and contrasted to show differences in potential flammability interpretations and design safety implications.


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Q: Extended display for two monitors I have three monitors connected to a windows 7 machine. I would like to extend the monitor from far left to the monitor in far right. And keep the middle screen independent.
Is there anyway to do this? I have two graphics cards.All NEC monitors connected with DVI cables. The middle screen directly connected to one of the graphics card, and other two screens are connected using a dvi split cable. The main reason i want to do this is to share the left most and right most screen for a remote desktop and and the middle screen for another remote desktop session. The middle screen is connected to AMD Radeon 6320 and the dvi splitter is connected to AMD Firepro 2270

A: Just connect left and right monitor seperetaly (with seperate cable) to your graphic card (as long as it has 2x DVI outputs or 1x DVI and 1x HDMI or DP (u can convert with adapter from them)).
If I'm not mistaken (correct me if I am), you are using split cable, that is from one DVI port in graphic card you connect two monitors?
If that's the case, then you can't have two seperate displays (neither you can't extend left monitor to right monitor) because you have one signal output.
Reason is simple: computer does not recognise two monitors, but only one.
Also, please provide model of the GPU that will be in charge of managing two monitors.
Model of each monitor would be helpful too.

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Sibling spat leads to broken window, cuts
DESTIN - Lawmen say a man who was angry with his twin brother was arrested after he threw something at a window, causing it to break and shower his brother with glass.
An Okaloosa County Sheriff's deputy went to an Airport Road apartment on Oct. 20 after receiving a report of an unknown problem. Once there he noticed the front window was almost entirely broken out, with glass lying on the front porch. Inside he saw a man lying on a bed, "bleeding profusely from multiple cuts on his hands," the deputy wrote in the arrest report.
The man who called lawmen said his twin was mad and locked him out of their apartment. He tried to get his brother to unlock the door, but his brother struck the window from inside, causing it to break and cover him with glass. He suffered multiple cuts on his arms and legs.
The brother accused of breaking the window said he was mad and threw something at the window. He denied trying to strike his brother.
The report didn't say what he threw at the window.
He was charged with battery.


text:
The Cast Of 'Back To The Future' Reunited At A Fan Convention
No DeLorean required!
Kate Streit 2018-08-15
Kate Streit · August 15, 2018
The cast of "Back to the Future" headed back to the past when the actors reunited at the Fan Expo Boston on Aug. 10. Stars of the 1985 classic film and its subsequent sequels, including Michael J. Fox (Marty McFly), Christopher Lloyd (Dr. Emmett Brown), Lea Thompson (Lorraine Baines) and Thomas Wilson (Biff Tannen), were present at the Boston Convention Center for the multi-genre convention, where they participated in a panel discussion.
The co-stars also posed for photos and signed autographs for fans. Thompson posted this photo of the whole gang on Twitter:
Friends from the past in the future! @FANEXPOBoston So fun. Love these men @realmikefox @TomWilsonUSA #chrislloyd #bttf pic.twitter.com/19EEUoAQ26
— Lea Thompson (@LeaKThompson) August 11, 2018
"Friends from the past in the future! @FANEXPOBoston So fun. Love these men @realmikefox @TomWilsonUSA #chrislloyd #bttf," she wrote.
The cast said during their panel discussion that a "Back to the Future 4" could still be in the cards and spoke to the franchise's enduring cultural impact.
"This movie was so powerful to show to your children because it's the idea that if you do the right thing, if you have the courage, if you stand up for yourself at the right moment of your life, you can change not only your future but your children's future," Thompson said, according to MassLive.
Some fans of the trilogy had dressed up in Marty's classic puffy vest for the event, prompting Fox to comment how hot it had been to wear during filming.
"It looked great but it was terrible to wear," he said, according to MassLive.
Some fans seemed to think it was worth the trouble, though:
My density came true today as I finally met the cast of my favorite film of all time! Back to the Future has meant so much to me for so many years, so this is so surreal! Such an honor! I'm still speechless! @fanexpoboston was a blast! 🤩 ••• @realmikejfox @lea_thompson @mrchristopherlloyd @tomwilsonusa @fanexpoboston #BackToTheFuture
A post shared by Eric Patrick Cameron (@ericcameronfilms) on Aug 11, 2018 at 7:46pm PDT
Wilson recalled seeing an industry screening of the first movie in Hollywood where he realized it was destined to be a classic.
"The applause the movie got just said, 'Wait a minute. This is something different,'" he said. "People from the very beginning, they just loved the movie."
Despite the actors' interest, filmmaker Robert Zemeckis, who holds the rights to the series along with writer/producer Bob Gale, has previously said that a reboot is out of the question.
"Oh, God no," Zemeckis told the Telegraph in 2015 about the possibility of another film. "That can't happen until both Bob and I are dead. And then I'm sure they'll do it unless there's a way our estates can stop it."
Would you watch a fourth installment of "Back to the Future?"
Tags:80s moviesback to the futuremichael j foxmovie franchisemovie rebootsmovies
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Michael J Fox walking across the street in a scene from the film 'Back To The Future', 1985. (Photo by Universal/Getty Images)


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Home > TCL > Vol. 64 (2021) > Iss. 2
Purkis and Mastermans' "The Awesome Autistic Go-To Guide: A Practical Handbook for Autistic Teens and Tweens" (book review)
Susanah J. Wilson Hanson, Trinity School for Ministry
Wilson Hanson, Susanah J. (2021) "Purkis and Mastermans' "The Awesome Autistic Go-To Guide: A Practical Handbook for Autistic Teens and Tweens" (book review)," The Christian Librarian: Vol. 64 : Iss. 2 , Article 16.
Available at: https://digitalcommons.georgefox.edu/tcl/vol64/iss2/16
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