If you've seen the hoopla surrounding ABC's newest program GCB (which stands for 'Good Christian B****es'), then you know it's got a lot of Christians (and Southerners) up in arms. Facebook, Twitter, and ABC's complaint lines are lit up with people that are angry, feeling that their culture, and religious beliefs have become the focus of satire.
Charisma Magazine seems to be at the forefront of this controversy, relating the airing of the show to the propaganda campaign that "Hitler used to kill six million Jews" (and yes, that means Godwin's law is alive and well).
But it has me wondering, what does Charisma hope to accomplish by such an article? Isn't that just playing right into the 'holier than thou, high and mighty, angry and offended' stereotype that GCB is trying to display? Isn't there a better way to get our message across than comparing the issue to the mass murder of an entire people group?
Between the anger and the angst, it seems no one has stopped to ask the hard questions---like is this stereotype sometimes true? And if so, how can we combat it?
I know I've certainly at one point or another portrayed a less than ideal version of Christianity (there is a reason why I don't have a fish on the back of my car....) and I assume you have to.
Let's start with that first. Let's start with our own hearts and motives instead of crying out against other people's.
It will be showing others the grace and love that should characterize our faith, and it will be doing this over and over again that will turn the tide on those stereotypes, and more importantly on people's hearts.
Jesus went to the cross silently, calmly, humbly. When Peter raised a sword in defense, Jesus rebuked him. In fact He told the disciples that if any town wouldn't receive them, to leave and kick the dust off their feet.
Christianity should never be a PR campaign. It should be a love revolution, surprising the public at large with acts of grace, humility, and truth. Showering the world with the light and love of Jesus.
And that's hard to do screaming from the rooftops in angry protest. The Lord doesn't need our well meaning defenses and bitter offenses....He needs hands that will love His children.
So whether it's GCB or ABC, maybe the question we should all be asking is simply WWJD?
Yes, I do agree with you and it is something we need to really think about.
LOVE your heart, friend. it's full of grace. e.
Great word, friend. And thank you for answering the question I had about what GCB means.
You are dead on here and I'm with you on the love revolution. Love more, condemn less. Love covers a multitude of offenses. One of the truths that i find in watching any type of "entertainment" is that God will speak to me through it if I have a heart to listen.
If it is making me angry... Why is it making me angry?
Is there any truth I can find here? Test everything and hold onto the good... At least that is what I try to do.
Thanks friend. I just think that it's going to be love and grace, not a Christian call-to-arms, that will save the day.
I love that phrase "Test everything..."


text:
#include <linux/errno.h>
#include <linux/sched.h>
#include <linux/syscalls.h>
#include <linux/mm.h>
#include <linux/fs.h>
#include <linux/smp.h>
#include <linux/sem.h>
#include <linux/msg.h>
#include <linux/shm.h>
#include <linux/stat.h>
#include <linux/mman.h>
#include <linux/file.h>
#include <linux/utsname.h>
#include <linux/personality.h>
#include <linux/random.h>
#include <linux/uaccess.h>
#include <linux/elf.h>

#include <asm/ia32.h>
#include <asm/syscalls.h>

/*
 * Align a virtual address to avoid aliasing in the I$ on AMD F15h.
 */
static unsigned long get_align_mask(void)
{
	/* handle 32- and 64-bit case with a single conditional */
	if (va_align.flags < 0 || !(va_align.flags & (2 - mmap_is_ia32())))
		return 0;

	if (!(current->flags & PF_RANDOMIZE))
		return 0;

	return va_align.mask;
}

unsigned long align_vdso_addr(unsigned long addr)
{
	unsigned long align_mask = get_align_mask();
	return (addr + align_mask) & ~align_mask;
}

static int __init control_va_addr_alignment(char *str)
{
	/* guard against enabling this on other CPU families */
	if (va_align.flags < 0)
		return 1;

	if (*str == 0)
		return 1;

	if (*str == '=')
		str++;

	if (!strcmp(str, "32"))
		va_align.flags = ALIGN_VA_32;
	else if (!strcmp(str, "64"))
		va_align.flags = ALIGN_VA_64;
	else if (!strcmp(str, "off"))
		va_align.flags = 0;
	else if (!strcmp(str, "on"))
		va_align.flags = ALIGN_VA_32 | ALIGN_VA_64;
	else
		return 0;

	return 1;
}
__setup("align_va_addr", control_va_addr_alignment);

SYSCALL_DEFINE6(mmap, unsigned long, addr, unsigned long, len,
		unsigned long, prot, unsigned long, flags,
		unsigned long, fd, unsigned long, off)
{
	long error;
	error = -EINVAL;
	if (off & ~PAGE_MASK)
		goto out;

	error = sys_mmap_pgoff(addr, len, prot, flags, fd, off >> PAGE_SHIFT);
out:
	return error;
}

static void find_start_end(unsigned long flags, unsigned long *begin,
			   unsigned long *end)
{
	if (!test_thread_flag(TIF_ADDR32) && (flags & MAP_32BIT)) {
		unsigned long new_begin;
		/* This is usually used needed to map code in small
		   model, so it needs to be in the first 31bit. Limit
		   it to that.  This means we need to move the
		   unmapped base down for this case. This can give
		   conflicts with the heap, but we assume that glibc
		   malloc knows how to fall back to mmap. Give it 1GB
		   of playground for now. -AK */
		*begin = 0x40000000;
		*end = 0x80000000;
		if (current->flags & PF_RANDOMIZE) {
			new_begin = randomize_range(*begin, *begin + 0x02000000, 0);
			if (new_begin)
				*begin = new_begin;
		}
	} else {
		*begin = current->mm->mmap_legacy_base;
		*end = TASK_SIZE;
	}
}

unsigned long
arch_get_unmapped_area(struct file *filp, unsigned long addr,
		unsigned long len, unsigned long pgoff, unsigned long flags)
{
	struct mm_struct *mm = current->mm;
	struct vm_area_struct *vma;
	struct vm_unmapped_area_info info;
	unsigned long begin, end;

	if (flags & MAP_FIXED)
		return addr;

	find_start_end(flags, &begin, &end);

	if (len > end)
		return -ENOMEM;

	if (addr) {
		addr = PAGE_ALIGN(addr);
		vma = find_vma(mm, addr);
		if (end - len >= addr &&
		    (!vma || addr + len <= vma->vm_start))
			return addr;
	}

	info.flags = 0;
	info.length = len;
	info.low_limit = begin;
	info.high_limit = end;
	info.align_mask = filp ? get_align_mask() : 0;
	info.align_offset = pgoff << PAGE_SHIFT;
	return vm_unmapped_area(&info);
}

unsigned long
arch_get_unmapped_area_topdown(struct file *filp, const unsigned long addr0,
			  const unsigned long len, const unsigned long pgoff,
			  const unsigned long flags)
{
	struct vm_area_struct *vma;
	struct mm_struct *mm = current->mm;
	unsigned long addr = addr0;
	struct vm_unmapped_area_info info;

	/* requested length too big for entire address space */
	if (len > TASK_SIZE)
		return -ENOMEM;

	if (flags & MAP_FIXED)
		return addr;

	/* for MAP_32BIT mappings we force the legacy mmap base */
	if (!test_thread_flag(TIF_ADDR32) && (flags & MAP_32BIT))
		goto bottomup;

	/* requesting a specific address */
	if (addr) {
		addr = PAGE_ALIGN(addr);
		vma = find_vma(mm, addr);
		if (TASK_SIZE - len >= addr &&
				(!vma || addr + len <= vma->vm_start))
			return addr;
	}

	info.flags = VM_UNMAPPED_AREA_TOPDOWN;
	info.length = len;
	info.low_limit = PAGE_SIZE;
	info.high_limit = mm->mmap_base;
	info.align_mask = filp ? get_align_mask() : 0;
	info.align_offset = pgoff << PAGE_SHIFT;
	addr = vm_unmapped_area(&info);
	if (!(addr & ~PAGE_MASK))
		return addr;
	VM_BUG_ON(addr != -ENOMEM);

bottomup:
	/*
	 * A failed mmap() very likely causes application failure,
	 * so fall back to the bottom-up function here. This scenario
	 * can happen with large stack limits and large mmap()
	 * allocations.
	 */
	return arch_get_unmapped_area(filp, addr0, len, pgoff, flags);
}

redpajama_set_name: RedPajamaGithub


text:
http://www.revelist.com/movies/golden-globes-snubbed-women-directors/16881
The Golden Globes Snubbed All Women Directors
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Despite some incredible women-run films and shows this year, not a single woman was recognized in the best director category.
Chloe Wilt
@chloewiltatx
#Movies
photo: AnnaPurna Pictures
The Golden Globes has had a contentious relationship with women directors, namely because it refuses to recognize them for their accomplishments.
It's been two years since most women attending the 2018 Golden Globes wore all black in support of the Time's Up movement, and Natalie Portman called out the Hollywood Foreign Press for nominating only men in the Best Director category. There's still a problem with diversity and representation.
This year's nominees for Best Director are, once again, all men, and many in the entertainment industry are sick of it. Even though plenty of women charged some of the best films (that were nominated in other categories), they weren't recognized for their work. As awards season begins again, here's hoping the lack of diversity isn't a trend.
All of the nominees for Best Director this year, and most of the past years, were men.
A post shared by Golden Globes (@goldenglobes) on Dec 9, 2019 at 7:57am PST
In 77 awards shows, only five women have ever been nominated for Best Director: Barbra Streisand, Jane Campion, Sofia Coppola, Kathryn Bigelow, and Ava DuVernay. Only one woman, Streisand, has won. This year, Bong Joon Ho, Sam Mendes, Todd Phillips, Martin Scorsese, and Quentin Tarantino are nominated for their films.
When They See Us was snubbed too.
Thank you. I am!
These things are a cherry on top. The sundae is yummy with or without it. And this one has been particularly delicious.
Okay, now I want ice cream. xo https://t.co/hip5ibyE2l
— Ava DuVernay (@ava) December 9, 2019
Ava DuVernay's incredible four-part miniseries chronicling the heartbreaking story of the Central Park Five definitely should have been recognized in any of the categories this year. Sadly, however, it did not land a single one. DuVernay isn't sweating it though; the film received 15 Emmy nominations and two wins earlier this year.
After one fan wished the director a good morning following the news, DuVernay replied, "Thank you. I am! These things are a cherry on top. The sundae is yummy with or without it. And this one has been particularly delicious. Okay, now I want ice cream. xo."
Greta Gerwig definitely should have been on the docket for Best Director, This is the second time she's been overlooked.
A post shared by Emma Watson (@emmawatson) on Dec 3, 2019 at 4:37pm PST
Emma Watson shared a video discussing Gerwig's vision for the classic novel's retelling. In 2018, Gerwig missed out on a director nomination for Lady Bird at the Golden Globes, but was nominated and lost at the Academy Awards. This time, she wasn't given the chance, even though Little Women was nominated in other categories.
Lorene Scafaria's Hustlers landed J.Lo a Golden Globe nom, but not for the director.
A post shared by lorenescafaria (@lorenescafaria) on Apr 8, 2019 at 6:05pm PDT
Scafaria told a brilliant story about cunning women who get what they want no matter the cost. The criminal tale had some people comparing Scafaria to great directors such as Martin Scorsese or Francis Ford Coppola. Either way, the critically acclaimed film wasn't enough for the Hollywood Foreign Press to recognize her.
Lulu Wang definitely deserved a nod for The Farewell.
A post shared by LULU WANG (@thumbelulu) on Aug 24, 2019 at 10:54am PDT
Lulu Wang talked through the various interpretations of her script for The Farewell. This story was Awkwafina's first time in a dramatic role and it landed her the Golden Globe nomination. Wang led the charge on this heartfelt story about Asian American families, and she deserved more in the awards sphere.
At the 2018 Golden Globes, Natalie Portman called out the all-male director nominees.
Many of the celebrities attending the awards show in 2018 were shocked at Portman's shade, but thought it was well-deserved. So many women-led films deserved more recognition that year and in past years, too. Women have often been ignored behind-the-scenes in the film industry for too long, and it's not going unnoticed.
Patty Jenkins, the director of Wonder Woman, said to ET News, "Look, it's been a little glaring that women directors don't get nominated so often. And it is odd, particularly when their films are being celebrated in every other way."
#awardsshows
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redpajama_set_name: RedPajamaCommonCrawl


Most people think they know how they would react if they were involved in a motor vehicle crash that injured themselves or their loved ones. Anyone who has been seriously injured in one, or seen a loved one seriously injured, knows that the days and weeks that follow can be both traumatizing and confusing.
At Hyland Law Firm, LLC, getting our clients full and fair compensation for their negligently caused injuries is our primary goal, but it isn't our only one. Attorney Charlie Hyland believes it's just as important to simplify what can be a confusing legal process for clients, and to provide straightforward and easy-to-understand legal advice. With nearly 25 years as a lawyer under his belt, he knows how to relate to clients on a personal level and fight to hold negligent parties accountable for the way they impact our clients' lives.
Whether you or your loved one was injured in a rear-end collision, a T-bone accident, a hit-and-run or any other type of injury-causing accident, our personal injury firm is ready to evaluate your options for getting the compensation you need.
Insurance companies are happy to avoid paying the full value of injury claims by either denying them altogether or making a settlement offer that seems attractive at first glance, but which fails to account for the long-term costs that can arise with serious injuries.
Having spent years working in the insurance defense field, and now as a plaintiff-side lawyer, Charlie Hyland can see through insurance companies' assertions and fight at the negotiating table or in a courtroom for compensation to cover medical expenses, pain and suffering, lost wages and lost earning potential.
With so much technology in today's cars, distracted driver accidents are becoming increasingly common. We can represent you if the other driver failed to pay attention to the road and you paid the price.
Email our Overland Park offices now or call for a free case evaluation with motor vehicle accidents lawyer Charlie Hyland.


text:
ACCEPTED

#### According to
Index Fungorum

#### Published in
Bull. trimest. Soc. mycol. Fr. 99(1): 92 (1983)

#### Original name
Cortinarius marcellae Rob. Henry

### Remarks
null


text:
<?php

namespace g5\HomeBundle\Twig\Extension;

class JSExtension extends \Twig_Extension
{
    /**
     * {@inheritdoc}
     */
    public function getFunctions()
    {
        return array(
            'toJS' => new \Twig_Function_Method($this, 'toJS', array(
                'is_safe' => array('html')
            )),
        );
    }

    /**
     * Exports a json string to valid javascript
     *
     * @param string $name The variable name
     * @param string $json The json data
     *
     * @return string
     */
    public function toJS($name, $json)
    {
        return '<script type="text/javascript">var '.$name.' = '.$json.';</script>';
    }

    /**
     * {@inheritdoc}
     */
    public function getName()
    {
        return 'g5_js_extension';
    }
}


Alexander Porfyrevich Borodin (November 12, 1833 - February 27, 1887) was a Russian composer who made his living as a chemist. He was a member of The Five, a group of composers dedicated to producing a specifically Russian music.
Borodin was born in Saint Petersburg, the illegitimate son of a prince who had him registered instead as the son of one of his serfs. He received a good education, including piano lessons, but it was chemistry in which he specialised, and he did not receive any formal lessons in composition until 1863, when he was taught by Mily Balakirev.
In 1869, Balakirev conducted Borodin's first symphony, and in the same year, Borodin started on his second symphony. This new symphony was a failure at its premiere, but Franz Liszt arranged a performance of it in Germany in 1880, and this brought Borodin some fame outside Russia.
Also in 1869, Borodin began work on his opera, Prince Igor, seen by some to be his most significant piece. It contains the Polovtsian Dances, which are often performed as a stand-alone work, and in that form probably constitute his best known composition. Borodin left the opera incomplete at his death, composition being slowed by his heavy workload as a chemist. It was completed posthumously by Nicolai Rimsky-Korsakov and Alexander Glazunov.
Despite being recognised as an accomplished composer, Borodin always earned a living as a chemist, and gained great respect in that field also, being particularly noted for his work on aldehydes. As a result, he was not as prolific a composer as many of his contemporaries, but he did write the popular symphonic poem In the Steppes of Central Asia, two string quartets and a handful of songs and piano pieces. He also started work on a third symphony, but that, also, was incomplete at his death (two movements of it were later completed by Glazunov).
Borodin, Alexander Porfir'yevich (1833 - 1887) - provides information on the Russian composer.
Alexander Porfir'yevich Borodin - Musica Classica classical music dictionary includes biography, illustrations, catalogue, and selected works with MIDI audio files.
Borodin, Aleksandr - Encyclopedia.com article includes pronunciation guide and bibliography.
EMORY UNIVERSITY: 19th-Century Music: Borodin - Student project by Stacey Roach. Biography, characteristics of the music, important works, and specific works.
MSN Learning & Research - Multimedia: Borodin's Polovtsian Dances - Information and sound file.


Here is a simple way to start your own estate planning checklist. Make an list of your assets and liabilities. Everything you own and everything you owe. This is your estate.
Next, make a list of all the assets in your estate and where you want those assets to go upon your death. Your plan for where your estate's assets will go upon your death (or even in life) is your estate plan.
The following article will help you create your own estate planning checklist, which will in turn help you in taking the next steps to creating your estate plan.
Although estate planning has become more popular over the years, there are still some basic steps that some people leave out which can lead to a nightmare for those left behind. When an estate hasn't been planned sufficiently, it is often those left behind-family and friends-that have to deal with the mess. And what's worse, money you earmarked to go to those you love now goes to lawyers, accountants and the state.
For this reason, we have compiled a simple estate planning checklist of things that you need to consider when planning your estate. Of course, it will always be best to contact a professional since every situation is unique but this is a basic checklist that you can help you get on the right track.
A last will and testament ("a will") is a document that tells the executor of your estate how you wish him or her to distribute your assets. A will does not avoid court interaction. Instead, a will is a road map for the probate court.
Possess the mental capacity to know what he or she is creating, what his possessions are, and his relationship to individuals named in the will.
Be signed by two witnesses that are not named in the will or not involved in the preparation of the will, i.e. no conflict of interest.
The two witness rule does not apply if the will is a holographic will.
A holographic will must be completely written, signed and dated in the testator's handwriting.
A note of caution: a will only takes affect upon the death of the testator. As a result, if the testator becomes incapacitated, another document, such as a living trust and living will (see below) should also be part of any good estate planning checklist.
As mentioned previously, wills do not take affect when you are incapacitated, which is why a health care directive can be helpful. Essentially, this means that all health decisions are made by you ahead of time should you be incapacitated and unable to make important health care decisions. As well as this 'living will', you can also appoint an agent for your financial affairs via a durable power of attorney (DPOA).
Aside from your health, you may also need someone to make decisions regarding your finances if you find yourself incapacitated down the line. If you cannot handle your own affairs, this person that is trusted and chosen by you will become your agent and make important financial decisions for you.
When people think about estate planning, they often overlook incapacity planning. A durable power of attorney ensures that someone you trust remains in control of your property and finances if you are unable to do so yourself.
If you are to appoint a DPOA, it is best to ensure that your finances are kept up-to-date so that the process will be easier for them. For example, IRA and 401k accounts should be regularly assessed. Every so often, review the details and ensure that the beneficiaries are listed as you wish. Furthermore, keep all annuities and life insurance contracts informed as to your decisions and chosen beneficiaries.
Finally, you can ease the pressure on your financial DPOA by making sure that your assets are properly titled in the name of your living trust.
Nowadays, one of the biggest concerns when estate planning is that the desired beneficiary not receive the assets as planned without having to go through an expensive probate. In order to avoid a costly and time consuming probate, a revocable living trust, also known as an inter vivos trust, is an excellent solution.
By placing your assets in a revocable living trust, you will be able to manage your financial affairs throughout your life and have a management plan in place should you become incapacitated. Not only will a revocable living trust help to avoid probate, it will keep all personal information private and provide your successor trustee with the authority to manage your finances if you become incapacitated.
Once you have created a living trust you must properly fund your trust. Correctly titling your assets in the name of your trust will ensure that your trustee will be able to administer your trust without any problems. However, many people have failed to properly place a valuable asset into the name of the trust, which can result in costly court proceedings to correct this oversight.
If you choose to go the route of a living trust, a pour over will is a must. A pour over will simply grabs any assets not tiled in the name of the trust and "pours" those assets into the trust. Then the assets placed in the trust will be distributed by the trustee according to the terms of the trust.
A word of caution. One problem many people run into with a poor estate plan is that their assets are not placed into their trust. As a result, when the Trustor dies, these untitled or poorly titled assets become part of the decedent's estate. This can lead to problems, such as the assets having to be probated. Therefore, make sure all your assets are properly titled.
If you have minor children under the age of 18, providing the name of a guardian in your will is a must. If you fail to provide who you want to become the legal guardian of your children, the court will make that decision for you. You will also want to consider naming a separate trustee to manage your children's assets that you leave behind.
Sadly, many people leave assets to their children each year without realizing how dangerous this can be. If you plan to leave any money or property to your children, you should always name an adult as an executor or trustee who can manage the assets for them. For those with young children, consider naming someone different than the guardian in your will so that there are checks and balances in place between the trustee and the guardian. You can also give your child money in certain increments or at specific ages to make sure the money is not given to your children in one lump sum.
Who will take over your business due to incapacity, retirement, or death?
Do you have a plan in place to sell the business if no competent suitor can take over?
Will your successor have access to enough liquid assets to pay off existing debt obligations?
Do you have a business succession plan in place if your become disabled or incapacitated?
Do you have a business succession plan in place if you or one of your partners dies?
Do you have a family business succession plan if you're in business with family members?
When planning your estate, it is really important that you understand federal estate taxes to avoid any unnecessary taxes against your estate. The 2018 estate tax exemption will be $11.2 million or $22.4 million for a married couple. If your estate is valued above the exemption limit advanced estate planning may be necessary, including the use of irrevocable trusts, such as irrevocable life insurance trusts, charitable remainder trusts and charitable lead trusts.
Life insurance for estate planning should name a beneficiary and not list your estate as the beneficiary. Life insurance proceeds are typically tax free. However, if your estate planning life insurance enriches your estate above the current federal estate tax exemption limit of $11.2 million, your life insurance may be taxed as part of your overall estate. A great way to title your life insurance beneficiary designation is to name your spouse or children as the primary beneficiary and then name the trustee of your trust as the contingent beneficiary.
While some choose to go for a funeral prepayment plan, these can be unreliable. Instead, those with limited liquid funds should consider setting up a 'payable-on-death' (POD) account at your local bank. As long as you deposit funds into the account every now and then, these funds can go directly towards a family member who will take care of funeral costs. Since the cost of funerals can be significant for families with little money, this is a good way to ease the burden after you pass away.
As we said at the very beginning, these are some simple steps that you can take to ensure that you and your loved ones are in the best position should something happen to go wrong with your estate plan. After all, the best laid plans of mice and men often clash with Murphy's Law (what can go wrong, will go wrong). Therefore, seeking out a professional estate planner goes a long way to ensuring that your goals are met.
By having a professional service by your side, you can be sure that there will be no nasty surprises for your loved ones after you pass away. Although this estate planning checklist is an important step, it is obviously not specific to you and your situation. In order to get a tailored plan you need to consult with a professional.
When you have all of your documents in order and the professional is happy that you are doing everything you can, you then need to have an organized filing system so that everything will be easy should the worst happen. When you die, people will need access to your will, real estate deeds, insurance policies, trusts, certificates for bonds, annuities, and stocks, bank accounts, mutual funds, IRA accounts, 401k accounts, mortgages, loans, and other important assets such as life insurance policies. In today's age of digital assets, it is also critical to remember estate planning for digital accounts, and identifying passwords, etc.
There you have it, an in-depth estate planning checklist. Remember, an estate plan only works if your successor trustee or executor is aware of it. Make sure whoever will administer your estate when you die or become incapacitated has access to your documents. That way, if the unexpected occurs you will be prepared. Your beneficiaries will thank you for your advanced planning.


6th, 7th, 8th Grade "Life Group"
We amp it up Sunday nights for 6th-8th Grade with Snacks, Games, devotions, outings! Don't miss the fun. Bring a friend and come hang out with us Sunday Nights.
We amp it up Sunday nights for 5th Grade with Snacks, Games, devotions, outings! Don't miss the fun. Bring a friend and come hang out with us Sunday Nights.
Transitions is ShelbyCC's Sunday morning class for those transitioning from being a child to becoming a teenager. Transitions focuses on establishing core knowledge of the Bible, developing faith habits, and living a Christian life in a world that is increasingly hostile to youth. Join us as we tackle tough questions, dig deep into Christian history, and form a community around the resurrected Christ. Transitions meets during second service.
Sunday Morning 9:30 am come and catch up with other students as we talk about our week, sports, upcoming events, GOD, and have breakfast.
This class is geared towards high school students. Material covered, conversations, and activities all are topics appropriate for high school students.
We begin each sunday worshiping downstairs followed by class upstairs.
We amp it up Sunday nights for 9th~12th Grade with Snacks, Games, devotions, outings! Don't miss the fun. Bring a friend and come hang out with us Sunday Nights.


text:
Jake E. Lee explains why his Ozzy-era "white pearl" Charvel guitar was not used on 'Patina' album
Posted on November 10, 2018 by Olivier in Uncategorized // 0 Comments
Red Dragon Cartel and former Ozzy Osbourne and Badlands guitarist Jake E. Lee was recently interviewed by Ultimate Guitar.
Lee was asked whether he used his classic Ozzy-era white pearl Charvel guitar during the recording of Red Dragon Cartel's sophomore studio album Patina, which was released via Frontiers Music Srl yesterday. Lee advised:
"No. We recorded all this in Pennsylvania on Anthony's ranch studio, and I didn't bring it. I don't really bring that out. It's actually kind of unplayable these days.
"It was probably unplayable back in the '80s, but it was just the guitar I was used to. It has a really narrow and skinny neck.
"I dealt with it back then because it was my main guitar, but on that guitar, it's hard to play an open D chord on it, because the neck, it got shaved down by Charvel way back when, and it's so narrow at the nut that if you play to play an open D chord and you're fretting the G string on the 2nd fret, the open D won't sound.
"You really have to know exactly how you're going to finger it for it to work."
The interviewer then seemingly joked that it was good to know that only Lee could play that guitar to which the Red Dragon Cartel guitarist replied:
"Since I put it into retirement and I haven't played it a lot. For me, it's a really hard guitar to play. I showed Charvel, because they wanted to make a replica, but no, you can't make a replica; nobody's going to want it, nobody's going to play it!
"They said, 'Sure they will,' and I showed it to them, and they went, 'Holy shit! How in the fuck did you play this thing?' But anyway, to answer your question, no, I didn't even bring it out to the ranch."
You can read the rest of the interview with Jake E. Lee at Ultimate Guitar.


Service related add-ons can raise the value of products while encouraging higher levels of customer satisfaction. A paper by Lusche & Spohrer discusses the service-dominant (S-D) logic as a science that encourages systems-level thinking and provides greater value propositions. The development of service related products alleviates many human-oriented problems in business and government entities. Thinking about service requires moving beyond the obvious to incorporate difficult to account for complexity.
Improvement comes with a level of chaos as we learn that we are interconnected and influenced by a complex system of people, events, and actors. S-D logic helps us understand how the underlying principles that foster growth and creation are not readily apparent. They are part of the fabric of our environment but when taken together create the totality of our economic system.
Innovation changes the environment in a way that can encourage higher levels of functioning and interaction between business and customers. Sometimes this innovation is complex and at other times it is small and adjustable. Change is the process of generating new solutions to existing processes and enhancing smooth business functioning through continuous adjustment.
Current institutional logic works well when the market is simple and stable. Business and marketing management is focused heavily on analysis, planning and control but are not optimum when the environment changes. The process of strategizing is based upon fixed market assumptions that don't regularly leave enough room for unexpected adjustments.
It is important to consider the adjustments in business development as the business changes and adapts to its environment. When new products and services make their way onto the market they naturally create change among the economic actors who seek to maximize their earning potential. We can see this occur in the development of stronger and more reliable cell phones that incorporate apps to enhance their functionality.
All service development should think about strategy beyond the here and now and leave enough flexibility within the strategic decision-making process to adjust to changes and new developments as they occur. This requires openness to new information that can help a strategy adjust as that new information becomes relevant. Providing for some level of contingency planning of most likely change scenarios can be beneficial.
Lusch, R. & Spohrer, J. (2012). Evolving serve for a complex, resilient, and sustainable world. Journal of Marketing Management, 28 (13-14).


text:
Home > Biodiversity: Woody crops less harmful than arable crops
Biodiversity: Woody crops less harmful than arable crops
Study finds that EU biofuel target reduces biodiversity
Current estimates state that transport is responsible for about 25% of the energy-related greenhouse gas emissions worldwide. While biofuels are seen as a possible means to reduce these emissions, they are under heavy discussion in terms of economic cost benefits and their environmental and social impacts.
The EU promotes the production of biofuels and has set a target of 5.75% share of biofuels in the transport section for all EU Member States by 2010, and a target of 10% to be reached by 2020. Currently, the biofuel crops consist mainly of commonly known arable crops, such as cereals, maize or rape seed. Increasing the share of these crops could lead to the expansion of cultivated areas, and in turn, to an increasing pressure on the environment, habitat loss and biodiversity decrease, especially if forest, grassland, peatland and wetlands are converted into monoculture plantations for biofuels crops.
The so-called second generation biofuel crops, produced from nonfood, ligno-cellulosic materials such as wood, energy grass or any other cellulosic biomass, which are being developed, offer an alternative. The effects of their production on biodiversity are estimated to be less drastic than that of regular arable crops.
A recent paper by Eggers et al. presents a new method of assessing biodiversity impacts resulting from changing land use due to the production of biofuel crops in Europe, distinguishing between arable (first generation) and woody (second-generation) crop types. In particular, Eggers et al. focus on two questions:
(1) what might happen if we doubled the current EU biofuel target of 5.75%, and
(2) what might happen if we abolished the current biofuel target.
While biodiversity as such includes all forms of life, their impact assessment was restricted to a set of 313 species pertaining to four taxonomical groups.
The results indicate that more species might suffer from habitat losses rather than benefit from a doubled biofuel target, while abolishing the biofuel target would mainly have positive effects. However, the possible impacts vary spatially and depend on the choice of biofuel crop, with woody crops being less detrimental than arable crops. The results give an indication for policy and decision makers of what might happen to biodiversity under a changed biofuel policy in the European Union. The presented approach is considered to be innovative as to date no comparable policy impact assessment has been applied to such a large set of key species at the European scale.
Furthr information
Is biofuel policy harming biodiversity in Europe? by Jeannette Eggers, Katja Tröltzsch, Alessandra Falcucci, Luigi Maiorano, Peter H. Verburg, Erik Framstad, Gerald Louette, Dirk Maes, Szabolcs Nagy, Wim Ozinga and Ben Delbaere, is published in GCB Bioenergy 1, 2009, pp. 18-34, doi 10.1111/j.1757-1707.2009.01002.x
Source: European Forest Institute, 2009-04-20.
European Forest Institute (EFI)
Algae Biofuels: Economic Viability
BMELV: Aktionsprogramm zum Ausbau der Bioenergienutzung im ländlichen Raum


Maycee Barber (6-0) is a 20-year-old combatant who is signed to the Ultimate Fighting Championship. In her next outing, Barber will clash with J.J. Aldrich at UFC Fight Night 148 on March 23.
As the match-up draws closer, here are five things that you might not know about the unbeaten prospect.
She has gone up a division.
She started training at a young age.
Barber is a lifelong martial arts fanatic. She first commenced training at the tender age of three, initially in karate. During her formative years, the Coloradan would try out wrestling, judo, jiu-jitsu, as well as muay Thai and boxing. It was her combat sports enthusiast parents who first introduced their daughter to the fighting arts.
Back in 2010, her mother and father opened their own martial arts academy in Fort Collins. When not studying at school, the fledgling fighter could more often than not be found honing her skills there. Today, although the 20-year-old also seeks training elsewhere, she still spends much of her time at her home gym, Fort Collins Martial Arts.
She has a lot of confidence.
Barber's UFC tenure began with a debut second-round TKO win over Hannah Cifers at UFC Fight Night 139. Afterward, she had a talk with Dana White. "I told him that I was gonna be as big, if not bigger, than Conor McGregor and Ronda Rousey and all of the stars he has," said the confident fighter.
She didn't go to college.
Barber had barely entered her teens when she set her heart on becoming a professional mixed martial arts combatant. Due to her chosen career path, the uber-prospect saw no point in pursuing a college education.
In June 2017, the then 19-year-old took the first step on her professional journey. It was a victorious effort as she snatched a first-round armbar submission over Itzel Esquivel.
She has only needed the judges once.
Barber has run roughshod through her opposition to date. Five of her wins have come by stoppage, and only one foe has made it to the final bell. That was Mallory Martin, who Barber faced in her second professional outing.


text:
// Licensed to the .NET Foundation under one or more agreements.
// The .NET Foundation licenses this file to you under the MIT license.
// See the LICENSE file in the project root for more information.

using System.Linq;
using Cake.Core.Tests.Fixtures;
using Xunit;

namespace Cake.Core.Tests.Unit.Scripting.Analysis
{
    public sealed class ScriptAnalyzerTests
    {
        public sealed class TheConstructor
        {
            [Fact]
            public void Should_Throw_If_File_System_Is_Null()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.FileSystem = null;

                // When
                var result = Record.Exception(() => fixture.CreateAnalyzer());

                // Then
                Assert.IsArgumentNullException(result, "fileSystem");
            }

            [Fact]
            public void Should_Throw_If_Environment_Is_Null()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.Environment = null;

                // When
                var result = Record.Exception(() => fixture.CreateAnalyzer());

                // Then
                Assert.IsArgumentNullException(result, "environment");
            }

            [Fact]
            public void Should_Throw_If_Log_Is_Null()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.Log = null;

                // When
                var result = Record.Exception(() => fixture.CreateAnalyzer());

                // Then
                Assert.IsArgumentNullException(result, "log");
            }
        }

        public sealed class TheProcessMethod
        {
            [Fact]
            public void Should_Throw_If_File_Path_Is_Null()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();

                // When
                var result = Record.Exception(() => fixture.Analyze(null));

                // Then
                Assert.IsArgumentNullException(result, "path");
            }

            [Fact]
            public void Should_Throw_If_Script_Was_Not_Found()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();

                // When
                var result = Record.Exception(() => fixture.Analyze("/Working/notfound.cake"));

                // Then
                Assert.IsType<CakeException>(result);
                Assert.Equal("Could not find script '/Working/notfound.cake'.", result?.Message);
            }

            [Fact]
            public void Should_Return_Code_Read_From_File()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "Console.ReadKey();");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(2, result.Lines.Count);
                Assert.Equal("#line 1 \"/Working/script.cake\"", result.Lines[0]);
                Assert.Equal("Console.ReadKey();", result.Lines[1]);
            }

            [Theory]
            [InlineData("#r \"hello.dll\"")]
            [InlineData("#reference \"hello.dll\"")]
            public void Should_Return_Single_Assembly_Reference_Found_In_Source(string source)
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", source);

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.References.Count);
                Assert.Equal("hello.dll", result.Script.References.ElementAt(0));
            }

            [Theory]
            [InlineData("#r \"hello.dll\"\n#r \"world.dll\"")]
            [InlineData("#r \"hello.dll\"\nConsole.WriteLine();\n#r \"world.dll\"")]
            public void Should_Return_Multiple_Assembly_References_Found_In_Source(string source)
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", source);

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(2, result.Script.References.Count);
                Assert.Equal("hello.dll", result.Script.References.ElementAt(0));
                Assert.Equal("world.dll", result.Script.References.ElementAt(1));
            }

            [Theory]
            [InlineData("#l \"utils.cake\"")]
            [InlineData("#load \"utils.cake\"")]
            public void Should_Process_Single_Script_Reference_Found_In_Source(string source)
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", source);
                fixture.GivenScriptExist("/Working/utils.cake", "Console.WriteLine();");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Includes.Count);
                Assert.Equal("/Working/utils.cake", result.Script.Includes[0].Path.FullPath);
            }

            [Theory]
            [InlineData("#l \"utils.cake\"\n#l \"other.cake\"")]
            [InlineData("#load \"utils.cake\"\n#load \"other.cake\"")]
            public void Should_Process_Multiple_Script_References_Found_In_Source(string source)
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", source);
                fixture.GivenScriptExist("/Working/utils.cake", "Console.WriteLine();");
                fixture.GivenScriptExist("/Working/other.cake", "Console.WriteLine();");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(2, result.Script.Includes.Count);
                Assert.Equal("/Working/utils.cake", result.Script.Includes[0].Path.FullPath);
                Assert.Equal("/Working/other.cake", result.Script.Includes[1].Path.FullPath);
            }

            [Fact]
            public void Should_Process_Using_Directives()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "using Cake.Core;");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Namespaces.Count);
                Assert.Equal("Cake.Core", result.Script.Namespaces.ElementAt(0));
            }

            [Fact]
            public void Should_Process_Using_Alias_Directives()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "using Core = Cake.Core;");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.UsingAliases.Count);
                Assert.Equal("using Core = Cake.Core;", result.Script.UsingAliases.ElementAt(0));
            }

            [Fact]
            public void Should_Keep_Using_Block()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "using(new Temp())\n{\n}");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(0, result.Script.UsingAliases.Count);
                Assert.Equal(0, result.Script.Namespaces.Count);
                Assert.Equal(4, result.Lines.Count);
                Assert.Equal(result.Lines[0], "#line 1 \"/Working/script.cake\"");
                Assert.Equal(result.Lines[1], "using(new Temp())");
                Assert.Equal(result.Lines[2], "{");
                Assert.Equal(result.Lines[3], "}");
            }

            [Fact]
            public void Should_Comment_Out_Shebang()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#!/usr/bin/cake\nConsole.WriteLine();");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(3, result.Lines.Count);
                Assert.Equal(result.Lines[0], "#line 1 \"/Working/script.cake\"");
                Assert.Equal(result.Lines[1], "// #!/usr/bin/cake");
                Assert.Equal(result.Lines[2], "Console.WriteLine();");
            }

            [Fact]
            public void Should_Process_Addin_Directive_Without_Source()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#addin \"Hello.World\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Addins.Count);
                Assert.Equal("nuget:?package=Hello.World", result.Script.Addins.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Process_Addin_Directive_Using_Uri()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#addin \"npm:?package=node\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Addins.Count);
                Assert.Equal("npm:?package=node", result.Script.Addins.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Process_Addin_Directive_With_Source()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#addin \"Hello.World\" \"http://source\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Addins.Count);
                Assert.Equal("nuget:http://source/?package=Hello.World", result.Script.Addins.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Process_Tool_Directive_Without_Source()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#tool \"Hello.World\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Tools.Count);
                Assert.Equal("nuget:?package=Hello.World", result.Script.Tools.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Process_Tool_Directive_With_Source()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#tool \"Hello.World\" \"http://source\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Tools.Count);
                Assert.Equal("nuget:http://source/?package=Hello.World", result.Script.Tools.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Process_Tool_Directive_Using_Uri()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#tool \"npm:?package=node\"");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(1, result.Script.Tools.Count);
                Assert.Equal("npm:?package=node", result.Script.Tools.ElementAt(0).OriginalString);
            }

            [Fact]
            public void Should_Insert_Line_Directives_When_Processing_Load_Directives()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/a.cake", "int x=0;\n#l b.cake\nint y=2;");
                fixture.GivenScriptExist("/Working/b.cake", "int z=1;\n#l c.cake\nint p=4;");
                fixture.GivenScriptExist("/Working/c.cake", "int o=3;\n#r d.dll");

                // When
                var result = fixture.Analyze("/Working/a.cake");

                // Then
                Assert.Equal(13, result.Lines.Count);
                Assert.Equal(result.Lines[0], "#line 1 \"/Working/a.cake\"");
                Assert.Equal(result.Lines[1], "int x=0;");
                Assert.Equal(result.Lines[2], "#line 1 \"/Working/b.cake\"");
                Assert.Equal(result.Lines[3], "int z=1;");
                Assert.Equal(result.Lines[4], "#line 1 \"/Working/c.cake\"");
                Assert.Equal(result.Lines[5], "int o=3;");
                Assert.Equal(result.Lines[6], "// #r d.dll");
                Assert.Equal(result.Lines[7], "#line 2 \"/Working/b.cake\"");
                Assert.Equal(result.Lines[8], "// #l c.cake");
                Assert.Equal(result.Lines[9], "int p=4;");
                Assert.Equal(result.Lines[10], "#line 2 \"/Working/a.cake\"");
                Assert.Equal(result.Lines[11], "// #l b.cake");
                Assert.Equal(result.Lines[12], "int y=2;");
            }

            [Fact]
            public void Should_Process_Break_Directive()
            {
                // Given
                var fixture = new ScriptAnalyzerFixture();
                fixture.GivenScriptExist("/Working/script.cake", "#break");

                // When
                var result = fixture.Analyze("/Working/script.cake");

                // Then
                Assert.Equal(2, result.Lines.Count);
                Assert.Equal(result.Lines[0], "#line 1 \"/Working/script.cake\"");
                Assert.Equal(result.Lines[1], @"if (System.Diagnostics.Debugger.IsAttached) { System.Diagnostics.Debugger.Break(); }");
            }
        }
    }
}


text:
HomeBusiness NewsCrypto trading site FTX under federal investigation amid bankruptcy
Crypto trading site FTX under federal investigation amid bankruptcy
Mon, November 14, 2022 by ABC News
Leon Neal/Getty Images
(NEW YORK) — The collapse of cryptocurrency exchange FTX is now the subject of an investigation by federal prosecutors in New York, sources familiar with the matter told ABC News.
Prosecutors join regulators from the Securities and Exchange Commission and the Commodity Futures Trading Commission in investigating the circumstances of FTX's bankruptcy.
At issue, the sources said, is whether FTX violated securities laws when it reportedly gave customer funds to Alameda Research, the trading firm of FTX founder Sam Bankman-Fried.
A spokesman for the U.S. Attorney's Office for the Southern District of New York declined to comment.
Authorities in the Bahamas, where FTX was located, have also launched a criminal investigation, according to a statement from the Royal Bahamas Police.
Earlier this month, concerns of financial instability at FTX — a top platform where users buy and sell crypto — triggered a wave of customer withdrawals totaling billions of dollars. But FTX lacked sufficient funds to pay sellers, instead imposing a halt on withdrawals altogether.
On Friday, FTX began bankruptcy proceedings in the U.S., as it assesses the value of its remaining assets, a company announcement said.
Bankman-Fried, 30, a prominent crypto entrepreneur and the CEO of FTX, resigned on Friday, the announcement added.
The fall of FTX centers in part on the cryptocurrency exchange's close relationship with Alameda Research, a crypto hedge fund also founded by Bankman-Fried.
FTX lent customer deposits to Alameda Research to help it meet its liabilities, and top executives at Alameda Research were aware of it, The Wall Street Journal reported.
FTX did not immediately respond to a request for comment from ABC News.
FTX faced a sudden selloff last week of a native cryptocurrency called FTT after news outlet CoinDesk reported that a significant portion of Alameda Research's assets consisted of the token, calling into question the financial independence of FTX.
Changpeng Zhao, the CEO of rival crypto exchange Binance, announced that he would sell $580 million worth of the token, causing a further spike in customer withdrawals that totaled $5 billion in a single day.
The selloff, akin to a bank run, put FTX in a difficult position of meeting the sudden demand for customer funds.
Some crypto traders on the platform have said they cannot access their money and may never get it back. The debacle coincides with a rough year for crypto, as the value of bitcoin has fallen more than 60%.
The year crypto broke: How customers, investors lost millions and what's being done
FTX naming-rights agreement for Miami Heat arena terminated in bankruptcy court
Former CEO of crypto firm Celsius sued in New York over alleged fraud
FTX crypto CEO Sam Bankman-Fried pleads not guilty in Manhattan federal court
FTX crypto CEO Sam Bankman-Fried expected to plead not guilty in court Tuesday
FTX founder Sam Bankman-Fried agrees to be extradited to US after chaotic hearing
Wind: S 5 mph Visibility: 10 mi


www.MasterChartsTrading.com Friday, March 6 2015 Weekly Market Recap.
Market breadth deteriorated somewhat- this is to be expected – the run-up from February 2nd low was as much as 7% and in a steep manner. So far there is no divergences in the AD Lines and New Highs – New Lows Indicator is in still in the positive territory. The breadth momentum oscillators (ITBM and ITVM) rolled over below their 10-day exponential moving average, which is somewhat bearish. However the breadth momentum is still in the positive territory, which means we could still see new highs before the next washout.
To highlight a sector, which was on fire for the past few months, I chose the biotech ETF - IBB. From its low in mid October IBB is up over 40%. It is certainly entitled to a rest that I believe we may be getting shortly.
Another industry group that may be poised to become a new market leader is the solar group (TAN). TAN broke out of a long consolidation on February 12 and pretty much never looked back. The important thing is TAN now became long-term bullish and pullbacks would be considered a buying opportunities.
TLT broke down on Friday with a gap and a follow-through. Our buy signal for TLT was on February 24, but bonds looked to be in trouble as early as February 26. Bonds are still bullish in the long-term.
Gold lost 3.75% for the week and decisively broke support from last week. Gold is certainly oversold short-term, but is clearly in a long-term downtrend. We could easily see newlows in gold soon.
Gold Miners are leveraged to the price of gold, so today's "mild" price drop in gold translated into a rout in gold miners. GDX collapsed 7.45%! Market breadth for the gold miners ETF is confirming the move lower. Just like gold itself, gold miners are very oversold and ripe for some sort of a counter-trend bounce. But these bounce are likely to be shorted, since both gold and the miners are in a long-term downtrend.


text:
То́лвоя́рви () — российское озеро в западной части Республики Карелия, часть водного бассейна реки Вуокса.

Общие сведения
Форма озера продолговатая, вытянута в меридиональном направлении. На озере 23 острова общей площадью 0,82 км², крупнейший остров — Коттисаари (0,52 км²). Берега возвышенные, каменисто-песчаные, покрыты хвойным лесом.

Озеро является промежуточным звеном в цепочке соединённых короткими протоками озёр, конечным из которых является озеро Ала-Толваярви:
Хирвасъярви → Толвоярви → Юриккаярви → Сариярви → Юля-Толваярви → Сарсаярви → Ала-Толваярви. Из озера Ала-Толваярви вытекает река Толвайоки, которая впадает в озеро Виксинселькя, из которого, далее, через реку Койтайоки воды, протекая по территории Финляндии, в итоге попадают в Балтийское море.

Дно покрыто илисто-песчаными грунтами. Высшая водная растительность представлена зарослями тростника, камыша, осоки, кувшинки.

В озере обитают плотва, окунь, щука, лещ, ряпушка, налим.

История
До Зимней войны озеро было частью волости Корписелькя Выборгской губернии. Во время Зимней войны в районе озера произошла одна из значимых для Финляндии битв.

Область Толваярви служила полем боя и во время Великой Отечественной войны. Является перспективной территорией экологического туризма.

См. также
 Озёра Карелии

Панорама

Примечания

Литература

Ссылки

Бассейн Толвайоки
Озёра Суоярвского района

redpajama_set_name: RedPajamaWikipedia


text:
package nbasim.sim;

/** Represents a standard 7-game NBA playoff series between two teams. */

public class Series implements Simable {

    public static final int NUM_GAMES = 7;
    public static final int NUM_WIN = (NUM_GAMES / 2) + 1;
    private Team home;
    private Team away;
    private int homeWins;
    private int awayWins;

    public Series(Team h, Team a) {
        home = h;
        away = a;
        homeWins = 0;
        awayWins = 0;
    }

    public Team sim() {
        int currentGame = 1;
        Team winner = null;
        while(homeWins < NUM_WIN && awayWins < NUM_WIN) {
            Game g = new Game(home, away);
            Simulation s = new Simulation(g);
            winner = s.sim();
            if(Simulation.VERBOSE) {
                System.out.println(">> " + winner.toString() + " won game " + (currentGame++) + " <<\n");
            }
            if(home == winner) {
                homeWins++;
            } else {
                awayWins++;
            }
        }
        if(Simulation.VERBOSE) {
            System.out.println(winner.toString() + " won the series in " + (currentGame - 1) + " games\n");
        }
        return winner;
    }

}


On occasion, First State Bank & Trust Co. has repossessed collateral available for sale.
Each item is sold "as is" with no stated or implied warranty.
At this time, there is no repossessed collateral for sale.
© . First State Bank & Trust Company Carthage.


text:
\section{Introduction}\label{sec:01}
Modified Newtonian dynamics (MOND) is an alternative to the dark matter paradigm, through the modification of Newton's law of universal gravitation or Newton's second law of motion \cite{Milgrom1983.ApJ.270.365,Milgrom1983.ApJ.270.371,Milgrom1983.ApJ.270.384}. The former belongs to the traditional modified gravity, and construction of its relativistic counterpart has been extensively discussed. \citet{Bekenstein1984.ApJ.286.7} proposed the first one. However, there are two major problems: the acausal problem \cite{Bekenstein1984.ApJ.286.7} and the gravitational lensing problem \cite{Bekenstein1994.ApJ.429.480}. Further modifications of the theory have been proposed to address these issues, such as the phase coupling \cite{Bekenstein1988.PLB.202.497} and disformal transformations \cite{Bekenstein1992.inproceedings,Bekenstein1993.PRD.48.3641,Sanders1997.ApJ.480.492,Bekenstein2004.PRD.70.083509}. These attempts made great progress in shaping the relativistic MOND theory and explaining the local gravitational phenomena \cite{Famaey2012.LRR.15.10}. However, for the cosmological linear perturbations, no such theory has been shown to successfully fit all the current data about the cosmic microwave background anisotropies and matter power spectra \cite{Skordis2006.PRL.96.011301,Dodelson2006.PRL.97.231301,Zuntz2010.PRD.81.104015,Xu2015.PRD.92.083505,Tan2018.JCAP.05.037}. Recently, \citet{Skordis2021.PRL.127.161302} proposed a new MOND theory to address this observational fitting problem. Analysis of this theory is the topic of this paper. In addition, we note that modification of Newton's second law still requires further development to arrive at a complete and observationally accepted theory \cite{Milgrom1994.AnnPhysNY.229.384,Milgrom1999.PhysLettA.253.273,Petersen2020.AaA.636.A56,Milgrom2022.PRD.106.064060}.

MOND theories generally predict an universal radial acceleration relation (RAR) --- correlation between the observed radial acceleration and that predicted by baryons with Newtonian gravity. \citet{McGaugh2016.PRL.117.201101} first observed the RAR in the SPARC database, and further data confirmed the conclusion \cite{Lelli2017.ApJ.836.152,Tian2020.ApJ.896.70}. This may be regarded as an observational evidence supporting MOND. However, after \citet{McGaugh2016.PRL.117.201101}, the same relation was also observed in the $N$-body simulations of cold dark matter (CDM) \cite{Dai2017.PRD.96.124016,Keller2017.ApJL.835.L17,Garaldi2018.PRL.120.261301,Dutton2019.MNRAS.485.1886}. The mass discrepancy acceleration relation, which is similar to RAR, was also predicted by MOND, and observed in both observations \cite{Durazo2017.ApJ.837.179} and CDM simulations \cite{Navarro2017.MNRAS.471.1841,Ludlow2017.PRL.118.161103}. In particular, \citet{Keller2017.ApJL.835.L17} found that the CDM simulated RAR depends on the cosmological redshift. This result implies that, in the framework of CDM, rotating galaxies still satisfy the \textit{universal} RAR at high redshifts. However, the parameter characterizing the acceleration scale in RAR is redshift-dependent. Recently, \citet{Mayer2023.MNRAS.518.257} presented an explicit redshift evolution of this characteristic MOND acceleration scale $a_\mond$ in the \textit{Magneticum} CDM simulations.

In the relativistic MOND theories, $a_\mond$ is a parameter and could be time-varying. \citet{Milgrom1983.ApJ.270.365} conjectured that $a_\mond\propto cH$ based on the numerical coincidence of their values at today. In the framework of T\textit{e}V\textit{e}S theory (a relativistic MOND theory) \cite{Bekenstein2004.PRD.70.083509}, \citet{Bekenstein2008.PRD.77.103512} analyzed this issue after considering the cosmological background evolution of the relevant fields. They found that $a_\mond$ changes on time scales much longer than the Hubble timescale. In this paper, we present the first analysis of the possible time evolution of the local Newtonian and MOND parameters in the \SZ theory \cite{Skordis2021.PRL.127.161302}. The method is principally the same as that in \cite{Bekenstein2008.PRD.77.103512}. Our result demonstrates how to reproduce the \textit{Magneticum} redshift dependence \cite{Mayer2023.MNRAS.518.257} in such relativistic MOND theory.

The first direct detection of the gravitational wave signal GW150914 has marked the new era of gravitational wave astronomy \cite{Abbott2016.PRL.116.061102}. In general relativity, there exist two well-known gravitational wave polarizations (plus and cross), traveling at the speed of
light. GW170814 and GW170817 observations confirmed these predictions \cite{Abbott2017.PRL.119.141101,Takeda2021.PRD.103.064037,Abbott2017.PRL.119.161101}. In this paper, we present a gauge-invariant gravitational wave analysis for the \SZ theory, in which the polarization content and the propagation speed are determined.

This paper is organized as follows. Section \ref{sec:02} introduces the \SZ MOND theory and summarizes the cosmic background evolutions. Note that, in principle, most of the results given in this section were obtained by \cite{Skordis2021.PRL.127.161302}. This section is retained to provide a clear basis for our subsequent discussions. Section \ref{sec:03} analyzes the Newtonian and MOND approximations. Section \ref{sec:04} discusses gravitational waves in the theory. Conclusions are presented in Sec. \ref{sec:05}.

Throughout this paper, we adopt the Hubble constant $H_0=67.4\,{\rm km}/{\rm s}/{\rm Mpc}$ and denote $h$ as its reduced value \cite{Aghanim2020.AaA.641.A6}. The subscript $0$ indicates the cosmological redshift $z=0$. In order to compare with observations, we adopt the SI Units and retain all physical constants in Sec. \ref{sec:02} and Sec. \ref{sec:03}. We set the speed of light $c=1$ in Sec. \ref{sec:04} for simplicity.

\section{The theory and cosmic evolutions}\label{sec:02}
The \SZ MOND theory is constructed based on a scalar field $\phi$ and a vector field $A_\mu$ \cite{Skordis2021.PRL.127.161302}. Its action is of the form $S = \int\dx^4x\sqrt{-g}\left[R + \mathcal{L}_\mond\right]/2\kappa + S_{\rm m}$, where $\kappa=8\pi\tilde{G}/c^4$ and $\tilde{G}$ is a constant with the same dimension of the Newtonian gravitational constant $\GN$. The MOND Lagrangian reads
\begin{align}
  & \mathcal{L}_\mond = - \frac{\KB}{2}F^{\mu\nu}F_{\mu\nu} + 2(2-\KB)J^\mu\nabla_\mu\phi \nonumber\\
  & \quad  - (2-\KB)\mathcal{Y} - \mathcal{F}(\mathcal{Y},\mathcal{Q})-\lambda(A^\mu A_\mu+1),
\end{align}
where $F_{\mu\nu}=2\nabla_{[\mu}A_{\nu]}$, $J_\mu=A^\alpha\nabla_\alpha A_\mu$, $\Y=q^{\mu\nu}\nabla_\mu\phi\nabla_\nu\phi$, $q^{\mu\nu}=g^{\mu\nu}+A^\mu A^\nu$, $\Q=A^\mu\nabla_\mu\phi$, $\F(\Y,\Q)$ is an arbitrary function, $\lambda$ is the Lagrange multiplier (a scalar), $\KB$ is a dimensionless constant. In our conventions, the dimension of $A_\mu$ relates to the metric ($[A^\mu A_\mu]=1$), $\phi$ is dimensionless, and $[\Y]=[\Q^2]=[\F]=[\lambda]={\rm length}^{-2}$.

The field equations can be derived from the variational principle. Variation of the action with respect to the metric gives the gravitational field equations
\begin{subequations}\label{eq:02}
\begin{align}\label{eq:02a}
  & G_{\mu\nu}  - \KB F_{\mu}^{\ \alpha}F_{\nu\alpha} + (2-\KB)\left\{ 2J_{(\mu}\nabla_{\nu)}\phi -A_\mu A_\nu\Box\phi \right. \nonumber\\
  & \ + \left. 2[A_{(\mu}\nabla_{\nu)} A_\alpha - A_{(\mu}\nabla_{|\alpha|} A_{\nu)}]\nabla^\alpha\phi  \right\} - \F_\Q A_{(\mu}\nabla_{\nu)}\phi \nonumber\\
  & \ - (2-\KB+\F_\Y)[\nabla_\mu\phi\nabla_\nu\phi+2\Q A_{(\mu}\nabla_{\nu)}\phi] \nonumber\\
  & \ - \lambda A_\mu A_\nu - g_{\mu\nu}\mathcal{L}_\mond/2 =\kappa T_{\mu\nu},
\end{align}
where $\F_\Y=\p\F/\p\Y$ and $\F_\Q=\p\F/\p\Q$. Variation of the action with respect to $\phi$ gives the scalar field equation
\begin{equation}\label{eq:02b}
  \nabla_\mu\mathcal{I}^\mu=0,
\end{equation}
where $\I^\mu=(2-\KB)J^\mu - (2-\KB+\F_\Y) q^{\alpha\mu}\nabla_\alpha\phi - \F_\Q A^\mu/2$. Variation of the action with respect to $A_\mu$ gives the vector field equations
\begin{align}\label{eq:02c}
  & \KB\nabla_\nu F^{\nu\mu} + (2-\KB)[(\nabla^\mu A_\nu)\nabla^\nu\phi - \nabla_\nu(A^\nu\nabla^\mu\phi)] \nonumber\\
  & \quad -\left[(2-\KB+\F_\Y)\Q + \F_\Q/2\right]\nabla^\mu\phi -\lambda A^\mu = 0.
\end{align}
Variation of the action with respect to $\lambda$ gives a constraint equation for the vector field
\begin{equation}\label{eq:02d}
  A^\mu A_\mu+1=0.
\end{equation}
\end{subequations}
Energy and momentum conservation $\nabla_\nu T^{\mu\nu}=0$ can be directly derived from Eq.~(\ref{eq:02}).

As we discussed in Sec. \ref{sec:01}, one goal of this paper is to study the time evolution of the local gravitational parameters in the \SZ MOND theory. In a relativistic theory, parameters describing the local gravitational system can be time-varying due to the cosmic evolution of the relevant fields. For example, the effective Newtonian gravitational \textit{constant} is time-varying in scalar-tensor gravity \cite{Brans1961.PhysRev.124.925,Damour1990.PRL.64.123,Babichev2011.PRL.107.251102,Zhang2019.PRD.100.024038,Burrage2020.JCAP.07.060} and nonlocal gravity \cite{Barreira2014.JCAP.09.031,Belgacem2019.JCAP.02.035,Tian2019.PRD.99.064044}. Here we summarize the cosmic background evolution for the \SZ MOND theory. We assume the Universe is described by the flat Friedmann-Lema{\^i}tre-Robertson-Walker (FLRW) metric $\dx s^2=-c^2\dx t^2+a^2\dx\mathbf{x}^2$,
where $a=a(t)$. To be consistent with Eq.~(\ref{eq:02d}), we assume $A_\mu=[-c,0,0,0]$ for the vector field. The scalar field is assumed to be $\phi=\phi(t)$. For the normal matters, we adopt $T^\mu_{\ \nu}={\rm diag}\{-\rho_{\rm m}c^2,p_{\rm m},p_{\rm m},p_{\rm m}\}$ \cite{Dodelson2020.book}. Substituting Eq.~(\ref{eq:02c}) into Eq.~(\ref{eq:02a}) eliminates $\lambda$. Then, substituting the above assumptions into the result, we obtain
\begin{subequations}\label{eq:03}
\begin{gather}
  H^2=\frac{8\pi\tilde{G}}{3}\rho_{\rm m}+\frac{c^2}{6}(\mathcal{F}-\Q\F_\Q), \label{eq:03a}\\
  H^2 + 2\frac{\ddot{a}}{a}=-\frac{8\pi\tilde{G}}{c^2} p_{\rm m} + \frac{1}{2}\mathcal{F}c^2, \label{eq:03b}
\end{gather}
with the cosmic background values $\Y=0$ and $\Q=\dot{\phi}/c$. Here the Hubble parameter $H\equiv\dot{a}/a$, $\dot{}\equiv\dx/\dx t$, and $\F$~and $\F_\Q$ are evaluated at the background. Equation~(\ref{eq:02b}) gives
\begin{equation}\label{eq:03c}
  \frac{\dx\F_\Q}{\dx t}+3H\F_\Q=0.
\end{equation}
\end{subequations}
To test self-consistency, we confirm that Eq.~(\ref{eq:02c}) gives only trivial results except one constraint equation on $\lambda$. Energy conservation $\dot{\rho}_{\rm m}+3H(\rho_{\rm m}+p_{\rm m}/c^2)=0$ can be derived from Eq.~(\ref{eq:03}) for arbitrary $\F$ function. In other words, Eqs.~(\ref{eq:03a}), (\ref{eq:03c}) and the matter energy conservation equation form a complete and self-consistent set. Based on Eq.~(\ref{eq:03}), we can define the effective MOND (dark matter) mass density and pressure as
\begin{equation}
  \rho_\mond = \frac{c^2}{16\pi\tilde{G}}(\mathcal{F}-\Q\F_\Q), \
  p_\mond = -\frac{\F c^4}{16\pi\tilde{G}}.
\end{equation}
Then Eq.~(\ref{eq:03}) can be rewritten as the two conventional Friedmann equations and one effective MOND energy conservation equation. The MOND relative mass density is defined as $\Omega_\mond\equiv8\pi\tilde{G}\rho_\mond/(3H^2)$.

In order to reveal the key properties of the cosmic background evolution, and to be consistent with the conventions adopted in \cite{Skordis2021.PRL.127.161302}, we rewrite the function
\begin{equation}
  \F(\Y,\Q) = (2-\KB)\J(\Y,\Q) - 2\K(\Q).
\end{equation}
Here the first term satisfies $\J(0,\Q)=0$, and is used to produce the MOND behavior (see Sec. \ref{sec:03}). For the second term, we adopt the Higgs-like function $\K(\Q)=(\K_2/4\Q_c^2)(\Q^2-\Q_c^2)^2$, where $\K_2$ and $\Q_c$ are constant parameters \cite{Skordis2021.PRL.127.161302,Note1}.
The $\Q$ approaches to $\Q_c$ in the infinite future. In the late-time Universe, we can adopt $\rho_{\rm m}=\rho_{\rm baryon}\propto a^{-3}$. Meanwhile we add the cosmological constant $\Lambda$ to Eq.~(\ref{eq:03a}). Then Eq.~(\ref{eq:03c}) completely determines the cosmological evolution of $\Q$. The solid lines in Fig.~\ref{fig:01} show the numerical results for this ordinary differential system. The initial condition of $\Q$ and parameters of baryon and $\Lambda$ are set so that $\Omega_{\rm Baryon}h^2=0.0224$ and $\Omega_\mond h^2=0.120$ at today \cite{Aghanim2020.AaA.641.A6}. The MOND parameters are $\K_2=8.5\times10^8$ and $\Q_c=1\,{\rm Mpc}^{-1}$, which guarantee good fits to the \textit{Planck} CMB measurements and SDSS matter power spectra results \cite{Skordis2021.PRL.127.161302}. We set $\tilde{G}=\GN$, which corresponds to a special kind of $\J$ function (see Sec. \ref{sec:03}). Note that the cosmic background evolutions are independent of $\J$. We emphasize that high precision calculations are required to suppress numerical errors. The bottom part plots the relative energy density $\Omega_i$ of each component together with the result of dark matter in the standard $\Lambda$CDM model \cite{Aghanim2020.AaA.641.A6}. The coincidence between MOND and CDM indicates that such MOND can behave as cold as the CDM in the expanding Universe. The top part plots the evolution of $\Q$. Considering the extremely small value of the dimensionless $y$-axis, we conclude that, during the late-time era, $\Q$ keeps almost constant while the variation of $\Q-\Q_c$ is considerable. Generalizing the Taylor expansion discussed in \cite{Skordis2021.PRL.127.161302}, we obtain
\begin{subequations}\label{eq:06}
\begin{gather}
  \frac{\Q-\Q_c}{\Q_c} = \frac{1}{2}\beta-\frac{3}{8}\beta^2+\mathcal{O}(\beta^3), \label{eq:06a}\\
  \rho_\mond = \frac{\K_2c^2\Q_c^2}{8\pi\tilde{G}}\left[\beta+\frac{1}{4}\beta^2+\mathcal{O}(\beta^3)\right], \\
  p_\mond = \frac{\K_2c^4\Q_c^2}{32\pi\tilde{G}}\beta^2+\mathcal{O}(\beta^3), \\
  w_\mond = \frac{\beta}{4}+\mathcal{O}(\beta^2),
\end{gather}
where
\begin{equation}
  \beta=\frac{3\Omega_{\mond,0}H_0^2}{\K_2c^2\Q_c^2}\left(\frac{a_0}{a}\right)^3 \ll 1. \label{eq:06e}
\end{equation}
\end{subequations}
Note that $1+z=a_0/a$, where $z$ is the cosmological redshift. The $\Omega_{\mond,0}$ appearing in Eq.~(\ref{eq:06e}) can be regarded as a boundary condition of the differential equation (\ref{eq:03}). The above result confirms that the MOND is cold for the previous parameter settings. In the top part of Fig.~\ref{fig:01}, we also plot the leading term of Eq.~(\ref{eq:06a}), and the result shows it is a good approximation. Especially, the leading terms of Eq.~(\ref{eq:06}) are valid for a general $\K(\Q)$ once it satisfies $\K\approx\K_2(\Q-\Q_c)^2$ when $\Q\rightarrow\Q_c$.

\begin{figure}[!t]
  \centering
  \includegraphics[width=0.95\linewidth]{Fig01.pdf}
  \caption{The cosmic background evolutions for the \SZ MOND theory (see the main text).}
  \label{fig:01}
\end{figure}

\section{Newtonian and MOND analysis}\label{sec:03}
In the \SZ theory, the form of $\J(\Y,\Q)$ determines the local gravitational behaviors. \citet{Skordis2021.PRL.127.161302} pointed out two key properties. For physically acceptable scenarios, in the strong field region~\footnote{Here \textit{strong} means the acceleration is much larger than $a_\mond$. The latter \textit{weak} indicates the opposite case.}, the scalar field is described by the tracking or screening solution, which corresponds to the strong asymptotic expression $\J\rightarrow\Y$ or $\J\rightarrow\Y^p$ with $p\geq3/2$, respectively. The strong field solution determines the relation between $\tilde{G}$ and $\GN$. In the weak field region \cite{Note2}, MOND appears if $\J\rightarrow\Y^{3/2}$. These analyzes assumed that $\Q$ appearing in $\J$ reaches its cosmological minimum $\Q_c$. However, this may be invalid if variables such as $\Q-\Q_c$ appear in $\J$ (see Fig.~\ref{fig:01} for the evolutions). Similar to the time-varying $\GN$ in the scalar-tensor theory \cite{Brans1961.PhysRev.124.925,Damour1990.PRL.64.123,Babichev2011.PRL.107.251102,Zhang2019.PRD.100.024038,Burrage2020.JCAP.07.060}, relaxing this static assumption may make the local MOND parameters time-varying.

Considering the great success of the $\Lambda$CDM model in both theories and observations \cite{Ostriker1993.ARAA.31.689,Frieman2008.ARAA.46.385,Bertone2018.RMP.90.045002}, we wish to answer what kind of $\J(\Y,\Q)$ can reproduce the redshift dependence found in the \textit{Magneticum} $\Lambda$CDM simulations \cite{Mayer2023.MNRAS.518.257}. However, we emphasize that the \textit{Magneticum} trend has not been confirmed by observations. The difference between the MOND predictions and the \textit{Magneticum} trend does not mean the failure of either theory. Instead, this possible difference provides an indicator to distinguish between MOND and $\Lambda$CDM observationally in the future. Besides MOND, dark sector models beyond $\Lambda$CDM, such as dynamical dark energy and ultralight dark matter, might also predict a different $a_\mond$--$z$ relation. This is due to the fact that these models could affect galaxy formation \cite{Penzo2014.MNRAS.442.176,Schive2014.NatPhys.10.496}. A complete model dictionary of $a_\mond(z)$ is useful for future observational tests. The present paper only focuses on the part about the \SZ MOND theory.

Following \cite{Skordis2021.PRL.127.161302}, we adopt the perturbed metric $\dx s^2=-c^2(1+2\Phi/c^2)\dx t^2+(1-2\Phi/c^2)\dx\mathbf{x}^2$, where the first-order infinitesimal $\Phi=\Phi(\mathbf{x})$. The vector field is assumed to be $A_\mu=[-c(1+\Phi/c^2),0,0,0]$, which is consistent with Eq.~(\ref{eq:02d}). The scalar field is assumed to be $\phi=\bar{\phi}(t)+\varphi$, where the bar means cosmic background value and the first-order infinitesimal $\varphi=\varphi(\mathbf{x})$. The time derivative of the first-order infinitesimal is ignored because it is much smaller than the corresponding space derivative \cite{Skordis2021.PRL.127.161302,Tian2019.PRD.99.064044}. The possible time dependence of the local MOND parameters is encoded in $\bar{\phi}(t)$, or strictly $\bar{\Q}(t)$. Note that we no longer assume $\bar{\Q}=\Q_c$. Calculating the quadratic terms in the action with the above perturbations, we obtain
\begin{subequations}\label{eq:07}
\begin{align}\label{eq:07a}
  S^{(2)} &= -\int c\dx t\,\dx^3\mathbf{x}\left\{\frac{2-\KB}{16\pi\tilde{G}}\left[|\nabla\hat{\Phi}|^2 \right.\right. \nonumber\\
    &  \quad \left.\left. + c^4\J(\Y,\bar{\Q}) + \mathrm{mass\ terms}\right] + \rho\Phi\right\},
\end{align}
where
\begin{equation}
  \Y = |\nabla\varphi|^2+\mathrm{mass\ terms}, \label{eq:07b}
\end{equation}
\end{subequations}
and $\hat{\Phi}=\Phi-\varphi c^2$, $\rho$ is the local baryon mass density, and the mass terms indicate terms like ${\rm const.}\times\Phi^n$. The $\K(\Q)$ only contributes to the mass terms because $\Q=\bar{\Q}\cdot(1-\Phi/c^2+2\Phi^2/c^4)$. For the same reason, we can rewrite $\bar{\Q}$ as $\Q$ in Eq. (\ref{eq:07a}), and only consider the perturbation of $\Y$ in the following discussions. Hereafter we ignore the mass terms. This is reasonable because suitable parameters can indeed suppress the corresponding influences on the Newtonian and MOND dynamics \cite{Skordis2021.PRL.127.161302}. Integration by parts is used to eliminate the second derivative terms (e.g., $\Phi\nabla^2\Phi$) and obtain the above results.  Equation~(\ref{eq:07}) recovers Eq.~(6) in \cite{Skordis2021.PRL.127.161302} when $\bar{\Q}=\Q_c$. Hereafter we omit the bar in $\bar{\Q}$ and adopt $\J_\Y=\p\J(\Y,\Q)/\p\Y$. Variation of $S^{(2)}$ with respect to $\hat{\Phi}$ and $\varphi$, we obtain
\begin{subequations}\label{eq:08}
\begin{gather}
  \nabla^2\hat{\Phi}=\frac{8\pi\tilde{G}}{2-\KB}\rho, \\
  \nabla[\J_\Y\nabla\varphi]=\frac{8\pi\tilde{G}}{(2-\KB)c^2}\rho, \label{eq:08b}
\end{gather}
\end{subequations}
respectively. The \SZ theory is written in the Einstein frame with minimally coupling between matter and other fields. Therefore, $\Phi=\hat{\Phi}+\varphi c^2$ is the physical gravitational potential. In the weak field region, if $\J\propto\Y^{3/2}$, i.e., $\J_\Y\propto|\nabla\varphi|$, then $\varphi$ dominates $\Phi$ and produces the MOND behavior \cite{Bekenstein1984.ApJ.286.7,Skordis2021.PRL.127.161302}.

Here we discuss the possible time evolution of $\GN$ and $a_\mond$. Comparison of Eq.~(\ref{eq:08}) and Poisson equation in strong field region determines $\GN$. In the scaling case \cite{Skordis2021.PRL.127.161302}, we assume $\J\rightarrow\lambda_s\Y$, where the dimensionless variable $\lambda_s=\lambda_s(\Q)$. Then Eq.~(\ref{eq:08}) gives $\varphi c^2\rightarrow\hat{\Phi}/\lambda_s$ and
\begin{equation}\label{eq:09}
  \GN = \frac{2\tilde{G}}{2-\KB}(1+\frac{1}{\lambda_s}).
\end{equation}
Note that $\tilde{G}$ is a constant introduced in the action, and $\GN$ could be time-varying because of its dependence on $\lambda_s$. Considering $(\Q-\Q_c)/\Q_c\ll1$ (see Fig.~\ref{fig:01}), if $\lambda_s\propto\Q^p$, where $p$ is a constant, then the time evolution of $\GN$ is unobservable. However, if $\lambda_s\propto(\Q-\Q_c)^p\propto a^{-3p}$, then Eq.~(\ref{eq:09}) gives
\begin{equation}
  \frac{\dot{G}_\textsc{n}}{\GN} \approx -\frac{\dot{\lambda}_s}{\lambda_s^2}
  \approx\frac{3pH_0}{\lambda_{s,0}}.
\end{equation}
in which we assumed $\lambda_s\gg1$ and the last equality is valid at the low redshift Universe. Current observations give $|\dot{G}_\textsc{n}/\GN|\lesssim10^{-12}\,{\rm yr}^{-1}\approx0.01H_0$ \cite{Williams2004.PRL.93.261101,Hofmann2010.AaA.522.L5,Zhu2015.ApJ.809.41}. Therefore we require $\lambda_{s,0}\gtrsim100$ for this case. The screening case \cite{Skordis2021.PRL.127.161302} corresponds to $\lambda_s=\infty$, and results in an exactly constant $\GN$. This requires $\J\propto\Y^p$, where $p\geq3/2$ \cite{Skordis2021.PRL.127.161302}.

\begin{table*}[!t]
  \centering
  \tabcolsep=0cm
  \rowcolors{3}{lightgray!40}{}
  \begin{minipage}{0.77\textwidth}
  \caption{Models discussing the possible cosmological evolution of $a_\mond$. Note that Eqs. (\ref{eq:12}) and (\ref{eq:13}) are extensions of the original \SZ theory.}
  \label{tab:01}
  \begin{tabular}{@{\,}p{2.13cm}p{3.5cm}p{8.1cm}@{\,}}
    \hline
    \multicolumn{3}{c}{
    \footnotetext{Most of the existing relativistic MOND theories give constant $a_\mond$. Here we only consider the models that the constant $a_\mond$ can still be obtained after analyzing the relevant cosmic background evolutions.}
    \footnotetext{Here $l_\textsc{de}$ is the characteristic length scale of dark energy, which is of the order of $\Lambda^{-1/2}$, i.e., $c/H_0$, at today and could be time-varying in the dynamical models. }}

    \\[-11pt]
    \hline
    $a_\textsc{mond}(z)$                       & \SZ theory                                       & Other theories \& Phenomenological motivations \\
    \hline
    \vspace{-3.6pt}$\sim{\rm const.}$\footnotemark[1] & \vspace{-3.6pt}$\J=c_1\Y^{3/2}/\Q$        & T\textit{e}V\textit{e}S
                                                                                theory~\cite{Famaey2007.PRD.75.063002,Bekenstein2008.PRD.77.103512}
                                                                                $\qquad$ $\qquad$ $\qquad$ $\qquad$ $\qquad$ $\qquad$ $\quad$
                                                                                a subclass of nonlocal MOND models \cite{Deffayet2014.PRD.90.064038} \\
    $\propto(1+z)^3$                           & $\J=c_1\Y^{3/2}/(\Q-\Q_c)$                       &  --- \\
    \vspace{-3.6pt}$\propto cH(z)$             & \vspace{-3.6pt}$\J=c_1\Y^{3/2}/\nabla_\mu A^\mu$ & the numerical coincidence between $a_{\textsc{mond},0}$ and $cH_0$
                                                                                \cite{Milgrom1983.ApJ.270.365,Milgrom2015.PRD.91.044009}
                                                                                a subclass of nonlocal MOND models~\cite{Deffayet2014.PRD.90.064038} \\
    \vspace{-3.6pt}$\propto c^2/l_\textsc{de}$\footnotemark[2] & \vspace{-3.6pt}$\J=c_1\Y^{3/2}/\sqrt{V_\textsc{de}}$ & the numerical coincidence between $a_{\textsc{mond},0}$ and
                                                                                $c^2/l_{\textsc{de},0}$~\cite{Milgrom2015.PRD.91.044009}
                                                                                relativistic theories linking MOND to dark energy
                                                                                \cite{Zhao2007.ApJL.671.L1,Blanchet2008.PRD.78.024031} \\
    \textit{Magneticum}                        & Eq.~(\ref{eq:11})                                & --- \\
    \hline
    \hline
  \end{tabular}
  \end{minipage}
\end{table*}

The parameter $a_\mond$ is determined in the weak field region, in which $\varphi$ dominates $\Phi$. Hereafter, for simplicity, we adopt $\J\propto\Y^{3/2}$ throughout the MOND region to the Newtonian region. Considering Eqs.~(\ref{eq:07b}), (\ref{eq:08b}), (\ref{eq:09}) with $\lambda_s=\infty$, and Eq.~(3) in \cite{Bekenstein1984.ApJ.286.7}, we see that the coefficient of $\J\propto\Y^{3/2}$ equals to $2c^2/(3a_\mond)$. On the other hand, the coefficient can be written as a function of $\Q$. Theoretically, $a_\mond$ could be redshift-dependent. Here we discuss several explicit cases. Considering the dimensions of the variables, one of the simplest cases is $\J=c_1\Y^{3/2}/\Q$, where $c_i$ ($i=1,2,3\cdots$) is dimensionless constants. This case gives nearly constant $a_\mond$ in the late-time Universe (see Fig. \ref{fig:01}). Replacing $\Q$ with $\Q-\Q_c$ in the denominator, we obtain $a_\mond\propto(1+z)^3$ based on Eq.~(\ref{eq:06a}). Figure \ref{fig:02} depicts this result together with the \textit{Magneticum} result \cite{Mayer2023.MNRAS.518.257}. We see that this simple case fails to accurately describe the \textit{Magneticum} trend. The best polynomial fit of the \textit{Magneticum} result is $a_\mond=[0.9+0.2(1+z)^2]\times10^{-10}\,{\rm m}/{\rm s}^2$~\footnote{We first fit the \textit{Magneticum} RAR result~\cite{Mayer2023.MNRAS.518.257} with a second order polynomial $c_0+c_1(1+z)+c_2(1+z)^2$. The result shows $c_1$ is an order of magnitude smaller than $c_0$ and $c_2$. Hence the $c_1$ term is negligible. The final polynomial $c_0+c_2(1+z)^2$ is just for mathematical convenience.}. Therefore, in the \SZ MOND theory, the \textit{Magneticum} trend could be reproduced by
\begin{equation}\label{eq:11}
  \J(\Y,\Q)=\frac{\Y^{3/2}}{c_1\Q_c+c_2\Q_c^{1/3}(\Q-\Q_c)^{2/3}}.
\end{equation}
For the parameters used in Sec. \ref{sec:02}, we obtain $c_1=4.6\times10^{-5}$ and $c_2=1.3\times10^6$ for the best fit. Note that Eq.~(\ref{eq:11}) gives an exactly constant $\GN$. Furthermore, if $\J\propto\Y^{3/2}$, then its specific form does not affect the cosmological linear perturbation analysis of the theory. The reason is that an equation similar to Eq.~(\ref{eq:07b}) can be obtained in the case of expanding Universe.

\begin{figure}[!b]
  \centering
  \includegraphics[width=0.95\linewidth]{Fig02.pdf}
  \caption{Four theoretical and \textit{Magneticum} simulated $a_\mond$ as a function of redshift. All results are calibrated at $z=0$.}
  \label{fig:02}
\end{figure}

Equation (\ref{eq:11}) could reproduce the \textit{Magneticum} trend, but may not be the most natural way --- the functional form and relevant parameters require slight fine-tuning. Figure \ref{fig:02} also plots the case of $a_\mond\propto cH$, which is pretty close to the \textit{Magneticum} result. Inspired by the numerical coincidence between $a_{\mond,0}$ and $cH_0$, \citet{Milgrom1983.ApJ.270.365} firstly conjectured this relation. A theory that $a_\mond$ is controlled by $cH$ multiplied by a $\mathcal{O}(1)$-valued redshift-dependent function seems more natural. The \SZ theory may not be able to realize $a_\mond\propto cH$. The reason is that the explicit time-dependent variable that exists here is $\Q-\Q_c\propto(1+z)^3$, rather than an explicit $H$-dependent expression. Luckily, a minor extension of the \SZ theory can achieve the desired scenario. Considering $\nabla_\mu A^\mu=3H/c$ \cite{Deffayet2014.PRD.90.064038} (see also the Acknowledgements), we see that replacing $\J(\Y,\Q)$ with
\begin{equation}\label{eq:12}
  \J(\Y,\nabla_\mu A^\mu)=c_1\Y^{3/2}/\nabla_\mu A^\mu
\end{equation}
gives $a_\mond=2cH/c_1$, where the dimensionless constant $c_1\approx4\pi$ \cite{Milgrom2015.PRD.91.044009}. Note that, in the MOND analysis, we only need to consider the background value of $\nabla_\mu A^\mu$ because $\Y^{3/2}$ is a high-order infinitesimal. In addition, this extension does not destroy the success of the original \SZ theory in fitting the cosmological observations \cite{Skordis2021.PRL.127.161302}. This is due to the facts that $\Y=0$ in the cosmological background and $\Y^{3/2}$ only contributes the high-order terms in the cosmological linear perturbation analysis. For the same reason, in the framework of the \SZ theory with minor extension, we can link MOND to dark energy with
\begin{equation}\label{eq:13}
  \J=c_1\Y^{3/2}/\sqrt{V_\textsc{de}},
\end{equation}
where $V_\textsc{de}$ is the field potential of dark energy. Following the conventions in \cite{Tian2020.PRD.101.063531}, we know $c_1$ is dimensionless and $[V_\textsc{de}]={\rm length}^{-2}$. There are some work in the literature discussing possible links between MOND and dark energy \cite{Milgrom2015.PRD.91.044009,Zhao2007.ApJL.671.L1,Blanchet2008.PRD.78.024031}. Here Eq. (\ref{eq:13}) provides a new example. If dark energy is the cosmological constant, then this case gives constant $a_\mond$. However, if dark energy is dynamical, then $a_\mond$ could be redshift-dependent. In Fig.~\ref{fig:02}, the green line plots an illustration for the power-law potential with the index $p=1$ \cite{Peebles1988.ApJL.325.L17,Steinhardt1999.PRD.59.123504}. Detailed evolution of dark energy can be found in Appendix \ref{app:A}. We emphasize that current observations require $p<0.06$ \cite{Xu2022.PhysDarkUniverse.36.101023}, which in turn gives a flatter $a_\mond(z)$. Therefore, relativistic theory linking MOND to dark energy is not a good option to reproduce the \textit{Magneticum} trend.

Table \ref{tab:01} summarizes the models mentioned above. One thing is worth mentioning here. Generally, in the T\textit{e}V\textit{e}S theory \cite{Bekenstein2004.PRD.70.083509}, the $a_\mond$ changes much more slowly than $cH$ \cite{Bekenstein2008.PRD.77.103512}. To our knowledge, no specific T\textit{e}V\textit{e}S theory has been confirmed that can realize $a_\mond\propto cH$.

\section{Gravitational wave analysis}\label{sec:04}
Gravitational wave properties in the \SZ theory can be determined by solving the linearized equations of motion about the Minkowski spacetime defined by $\bar g_{\mu\nu}=\eta_{\mu\nu}$, $\bar A^\mu=\delta^\mu_0$, and $\bar\phi={\rm const.}$. This background solution requires that $\bar{\mathcal F}=\bar{\mathcal F}(\bar g_{\mu\nu}, \bar A^\mu,\bar\phi)=0$. The perturbed solutions are $g_{\mu\nu}=\eta_{\mu\nu}+h_{\mu\nu}$, $A^\mu=\delta^\mu_0+a^\mu$, and $\phi=\bar\phi+\varphi$. Since the linearized equations of motion are very complicated and coupled together, it is easier to use the gauge-invariant formalism to decouple the equations \cite{Flanagan:2005yc,Gong:2018cgj}. Following \citet{Gong:2018cgj}, one can decompose the components of $h_{\mu\nu}$ and $a^\mu$ as
\begin{subequations}
\begin{gather}
  h_{tt} = 2\phi, \label{httdec}\\
  h_{tj} = \beta_j+\partial_j\gamma, \label{htjdec}\\
  h_{jk} = h_{jk}^\mathrm{TT}+\frac{1}{3}H\delta_{jk}+\partial_{(j}\epsilon_{k)}+\left(\partial_j\partial_k-\frac{1}{3}\delta_{jk}\nabla^2\right)\rho,\label{hjkdec}\\
  a^t=\frac{1}{2}h_{tt}=\phi,\label{v0dec}\\
   a^j=\mu^j+\partial^j\omega.\label{vjdec}
\end{gather}
\end{subequations}
Here, $\partial^kh_{jk}^\mathrm{TT}=0$, $\eta^{jk}h_{jk}^\mathrm{TT}=0$, and $\partial_j\beta^j=\partial_j\epsilon^j=\partial_j\mu^j=0$.
Under the infinitesimal coordinate transformation parameterized by $\xi^\mu=(\xi^t,\xi^j)=(A,B^j+\partial^jC)$ with $\partial_jB^j=0$, one knows that
\begin{subequations}
\begin{gather}\label{eq-gt}
  h_{\mu\nu}\rightarrow h_{\mu\nu}-\partial_\mu\xi_\nu-\partial_\nu\xi_\mu,\\
  a^\mu\rightarrow a^\mu+\bar A^\nu\partial_\nu\xi^\mu,\\
  \varphi\rightarrow\varphi.
\end{gather}
\end{subequations}
Therefore, one determines the following gauge-invariant variables,
\begin{subequations}
\begin{gather}
    \varphi,\quad h^\mathrm{TT}_{jk},\\
  \Phi = -\phi+\dot\gamma-\frac{1}{2}\ddot\rho, \\
  \Theta = \frac{1}{3}(H-\nabla^2\rho), \\
  \Xi_j = \beta_j-\frac{1}{2}\dot\epsilon_j,\\
  \Sigma_j=\beta_j+\mu_j,\\
   \Omega=\omega+\frac{1}{2}\dot\rho.
\end{gather}
\end{subequations}
Then, one can try to reexpress the linearized equations of motion to conclude that
\begin{subequations}
\begin{gather}
    \ddot h_{jk}^\mathrm{TT}-\nabla^2h_{jk}^\mathrm{TT}=0,\\
    \ddot \Sigma_j-\nabla^2\Sigma_j=0,\\
    \frac{\partial^2\bar{\mathcal F}}{\partial\mathcal Q^2}\ddot\varphi+2\left[ \frac{2(2-\KB)}{\KB}+\frac{\partial\bar{\mathcal F}}{\partial\mathcal Y} \right]\nabla^2\varphi=0,\\
    \Xi_j=0,\\
    \Theta=\Phi=0,\\
    \dot\Omega=\frac{\KB-2}{\KB}\varphi,
\end{gather}
\end{subequations}
assuming $\partial\bar{\mathcal F}/\partial\mathcal Q=0$, where barred quantities are to be evaluated at the flat spacetime background. The above equations show that the tensor and vector modes are propagating at the speed of light, while $\varphi$ generally travels at a different speed, which is smaller than the speed of light for the parameter values adopted in Sec. \ref{sec:02}. This result reconfirmed the conclusion presented in \cite{Skordis2021.PRL.127.161302}.

Provided that the ordinary matter couples with the metric minimally, one can calculate the geodesic deviation equation, $\ddot x^j=-R_{tjtk}x^k$, to determine the polarizations of gravitational waves \cite{Misner:1974qy}. It turns of that
\begin{equation}
    \label{eq-relc}
    R_{tjtk}=-\frac{1}{2}h_{jk}^\mathrm{TT}.
\end{equation}
Therefore, there are only two polarizations (plus and cross), like in general relativity.

\section{Conclusions}\label{sec:05}
In this paper, we discuss the Newtonian, MOND and gravitational wave analyses for the \SZ theory \cite{Skordis2021.PRL.127.161302}. In the first two cases, after abandoning the static assumption adopted in \cite{Skordis2021.PRL.127.161302}, we find that whether $\GN$ and $a_\mond$ are time-varying depends on the specific form of the $\J$ function of the theory. Screening the scalar field in strong field region is a sufficient condition to give a constant $\GN$, and this scenario may be a preferred choice in both theory and observations. For the $a_\mond$, we highlight that the theory with Eq.~(\ref{eq:11}) could reproduce the $a_\mond$--$z$ dependence observed in the \textit{Magneticum} simulations \cite{Mayer2023.MNRAS.518.257}. Minor extension of the original \SZ theory with Eq. (\ref{eq:12}) gives $a_\mond\propto cH$. For the gravitational wave analysis, we show that there are only two tensor polarizations, which is preferred by the GW170814 observations \cite{Abbott2017.PRL.119.141101,Takeda2021.PRD.103.064037}.

\section*{Acknowledgements}
We especially thank the referee for pointing out $\nabla_\mu A^\mu\propto H(z)$ and suggesting that we discuss the model described by Eq. (\ref{eq:12}). This work was supported by the National Natural Science Foundation of China under Grants No. 11633001, No. 11920101003, No. 12021003 and No. 11690023, and the Strategic Priority Research Program of the Chinese Academy of Sciences, Grant No. XDB23000000. S. T. was supported by the Initiative Postdocs Supporting Program under Grant No. BX20200065 and China Postdoctoral Science Foundation under Grant No. 2021M700481. S. H. was supported by the National Natural Science Foundation of China under Grant No. 12205222.

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