Its a god-awful small affair
To the girl with the mousy hair
But her mummy is yelling, No!
And her daddy has told her to go
But her friend is nowhere to be seen
Now she walks through her sunken dream
To the seat with the clearest view
And shes hooked to the silver screen
But the film is a saddening bore
For shes lived it ten times or more
She could spit in the eyes of fools
As they ask her to focus on
Sailors fighting in the dance hall
Oh, man, look at those cavemen go
Its the freakiest show
Take a look at the lawman
Beating up the wrong guy
Oh, man, wonder if hell ever know
Hes in the best selling show
Is there life on Mars?
Its on Americas tortured brow
That Mickey Mouse has grown up a cow
Now the workers have struck for fame
Cause Lennons on sale again
See the mice in their million hordes
From Ibiza to the Norfolk Broads
Rule Britannia is out of bounds
To my mother, my dog, and clowns
But the film is a saddening bore
Because I wrote it ten times or more
Its about to be writ again
As I ask you to focus on
Sailors fighting in the dance hall
Oh, man, look at those cavemen go
Its the freakiest show
Take a look at the lawman
Beating up the wrong guy
Oh, man, wonder if hell ever know
Hes in the best selling show
Is there life on Mars?


We passed upon the stairs
We spoke of was and when
Although I wasnt there
He said I was his friend
Which came as a surprise
I spoke into his eyes
I thought you died alone
A long long time ago
Oh no, not me
We never lost control
Youre face to face
With the man who sold the world
I laughed and shook his hand
And made my way back home
I searched for foreign land
For years and years I roamed
I gazed a gazely stare
We walked a million hills
I must have died alone
A long, long time ago
Who knows? Not me
I never lost control
Youre face to face
With the man who sold the world
Who knows? Not me
We never lost control
Youre face to face
With the man who sold the world


Its Christmas time
Theres no need to be afraid
At Christmas time
We let in light and we banish shade
And in our world of plenty
We can spread a smile of joy
Throw your arms around the world
At Christmas time
But say a prayer
Pray for the other ones
At Christmas time its hard
But when youre having fun
Theres a world outside your window
And its a world of dread and fear
Where the only water flowing
Is the bitter sting of tears
And the Christmas bells that ring there
Are the clanging chimes of doom
Well tonight thank God its them
Instead of you
And there wont be snow in Africa this Christmas time
The greatest gift theyll get this year is life
Where nothing ever grows, no rain or rivers flow
Do they know its Christmas time at all?
Heres to you
Raise a glass for everyone
Heres to them
Underneath that burning sun
Do they know its Christmas time at all?
Feed the world
Feed the world
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again
Feed the world
Let them know its Christmas time again


Look up here, Im in heaven
Ive got scars that cant be seen
Ive got drama, cant be stolen
Everybody knows me now
Look up here, man, Im in danger
Ive got nothing left to lose
Im so high, it makes my brain whirl
Dropped my cell phone down below
Aint that just like me?
By the time I got to New York
I was living like a king
There I used up all my money
I was looking for your ass
This way or no way
You know Ill be free
Just like that bluebird
Now, aint that just like me?
Oh, Ill be free
Just like that bluebird
Oh, Ill be free
Aint that just like me?


Context:
(Last revised January 2, 2009)

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As of March 13th , 2014 , the booklet had been downloaded over 18,300 times and counting .


In order to help increase the booklets downloads , it would be great if all Stormfronters who had YouTube accounts , could display the following text in the description boxes of their uploaded YouTube videos .


( Simply copy and paste the following text into your YouTube videos description boxes. )


Click below for a FREE download of a colorfully illustrated 132 page e-book on the Zionist-engineered INTENTIONAL destruction of Western civilization .


Click on the `` DOWNLOAD ( 7.42 MB ) '' green banner link .


Booklet updated on Feb. 14th , 2014 .


( Now with over 18,300 Downloads. )


PDF file : http://www.mediafire.com/download/7p3p3goadvvqvsf/WNDebateBooklet_2-14-14.pdfMSWordfile:http://www.mediafire.com/download/psezkkk4d6a3wt1/WNDebateBooklet _ 2-14-14.docx Watch the 10 hour video version of `` The Zionist Attack on Western Civilization '' @ http://trutube.tv/video/14247/The-Zionist-Attack-on-Western-Civilization-Pages-1-33-Part-1-of-4-Banned-from-YouTubeNotepadPromotionalYouTubeComment:http://www.mediafire.com/download/96fg6ft02lyfruz/Booklet _ White _ YT _ Comment _ ( Hyperlinked ) .txt http://www.mediafire.com/download/zcn3wozjbwnezms/Booklet-White-YT-Comment- ( Hyperlinked-Back-Up % 5D.txt http://www.mediafire.com/download/9uyudq1yuxu1dur/Booklet+Comment+%28Firefox%29.txt2minutepromotionalBOOKLETvideo@http://www.youtube.com/watch ? v = _ 8hg254ALpM Are you interested in helping spread the booklet download link across the world ?


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Thank you in advance. : ) Download the youtube `` description box '' info text file below @ http://www.mediafire.com/download/dqhn1czprr17o21/Booklet-Description-Box _ Info.txt


The sanctions against the school were a punishing blow, and they seemed to what the efforts the school had made to change? </s> A: ignore </s> B: enforce </s> C: authoritarian </s> D: yell at </s> E: avoid </s> There is only one correct answer. Pick the best answer.


Google Maps and other highway and street GPS services have replaced what? </s> A: united states </s> B: mexico </s> C: countryside </s> D: atlas </s> E: oceans </s> There is only one correct answer. Pick the best answer.


The fox walked from the city into the forest, what was it looking for? </s> A: pretty flowers. </s> B: hen house </s> C: natural habitat </s> D: storybook </s> E: dense forest </s> There is only one correct answer. Pick the best answer.


What home entertainment equipment requires cable? </s> A: radio shack </s> B: substation </s> C: cabinet </s> D: television </s> E: desk </s> There is only one correct answer. Pick the best answer.


What do people use to absorb extra ink from a fountain pen? </s> A: shirt pocket </s> B: calligrapher's hand </s> C: inkwell </s> D: desk drawer </s> E: blotter </s> There is only one correct answer. Pick the best answer.


James was cooling off two quickly.  He would die if he didn't find some way to stop what? </s> A: loss of heat </s> B: revenge </s> C: expansion </s> D: relaxation </s> E: calm down </s> There is only one correct answer. Pick the best answer.


Of all the rooms in a house it was his favorite, the aromas always drew him to the what? </s> A: yard </s> B: basement </s> C: kitchen </s> D: living room </s> E: garden </s> There is only one correct answer. Pick the best answer.


Bill is stuck in marsh when a man comes up to him peaking Cajun, where is he? </s> A: low lands </s> B: new york </s> C: forest </s> D: louisiana </s> E: everglades </s> There is only one correct answer. Pick the best answer.


What is it called when you slowly cook using a grill? </s> A: backyard </s> B: restaurant </s> C: crockpot </s> D: neighbor's house </s> E: barbeque </s> There is only one correct answer. Pick the best answer.


What type of person typically contracts illness? </s> A: hospital </s> B: head </s> C: sick person </s> D: elderly person </s> E: doctor's office </s> There is only one correct answer. Pick the best answer.


a mom holding her babies in the middle of the picture, no other image intervenes with the image.


The image is fading between a woman holding a baby and a woman sitting with a red background. The hands of the woman sitting aren't visible.


the man on the left is walking away with his right foot lifting from the floor, the girl in green looking at her right with her mouth shut


The girl in the light blue shirt is looking down to the couch. Her left hand is open and it is blurry. Her right hand is to her side on the side of her stomach. The girl with the curly hair has her mouth slightly open and her head facing her right.


The girl in green has her knee over the back of the couch; the girl in gray's hand is pointing straight at the knee


a round china bowl filled with untouched green pepper, tomato, meat and rice


Blonde woman has cut thru to write paper and daughter looking down paying with hands.


the mom holds the paper with her left hand, and the scissor with her right hand,


The wrapping paper is not unrolled and the woman is not touching the toy


A young girl's nose is barely touching the hair on the head of a person facing them.


Why is your exchange rate so bad?

Why is your exchange rate so bad?


What do I need to do to get a card?

What do I need to do to get a card?


I transfered my balance a while back.  Why doesn't my account reflect this?


Am I able to track the card that was just sent to me?


Where can I find the auto-top option?

Where can I find the auto-top option?


Should my top up still be pending?

Should my top up still be pending?


I need to exchange a currency - can I do that here?


How do you find the exchange rate?

How do you find the exchange rate?


How long will my top-up be pending?

How long will my top-up be pending?


How do I get my virtual card?

How do I get my virtual card?


Context: This is the most common method of construction procurement and is well established and recognized. In this arrangement, the architect or engineer acts as the project coordinator. His or her role is to design the works, prepare the specifications and produce construction drawings, administer the contract, tender the works, and manage the works from inception to completion. There are direct contractual links between the architect's client and the main contractor. Any subcontractor has a direct contractual relationship with the main contractor. The procedure continues until the building is ready to occupy.

Question: There are direct contractual links between who?


Context: After strengthening his government in northern China, Kublai pursued an expansionist policy in line with the tradition of Mongol and Chinese imperialism. He renewed a massive drive against the Song dynasty to the south. Kublai besieged Xiangyang between 1268 and 1273, the last obstacle in his way to capture the rich Yangzi River basin. An unsuccessful naval expedition was undertaken against Japan in 1274. Kublai captured the Song capital of Hangzhou in 1276, the wealthiest city of China. Song loyalists escaped from the capital and enthroned a young child as Emperor Bing of Song. The Mongols defeated the loyalists at the battle of Yamen in 1279. The last Song emperor drowned, bringing an end to the Song dynasty. The conquest of the Song reunited northern and southern China for the first time in three hundred years.

Question: What area was Kublai trying to capture by defending Xiangyang?


Context: The neighborhood of Sunnyside is on Fresno's far southeast side, bounded by Chestnut Avenue to the West. Its major thoroughfares are Kings Canyon Avenue and Clovis Avenue. Although parts of Sunnyside are within the City of Fresno, much of the neighborhood is a "county island" within Fresno County. Largely developed in the 1950s through the 1970s, it has recently experienced a surge in new home construction. It is also the home of the Sunnyside Country Club, which maintains a golf course designed by William P. Bell.

Question: Where is the home of the Sunnyside Country Club?


Context: The historical measure of a steam engine's energy efficiency was its "duty". The concept of duty was first introduced by Watt in order to illustrate how much more efficient his engines were over the earlier Newcomen designs. Duty is the number of foot-pounds of work delivered by burning one bushel (94 pounds) of coal. The best examples of Newcomen designs had a duty of about 7 million, but most were closer to 5 million. Watt's original low-pressure designs were able to deliver duty as high as 25 million, but averaged about 17. This was a three-fold improvement over the average Newcomen design. Early Watt engines equipped with high-pressure steam improved this to 65 million.

Question: What was the ideal duty of a concept engine?


Context: Imperialism and colonialism both dictate the political and economic advantage over a land and the indigenous populations they control, yet scholars sometimes find it difficult to illustrate the difference between the two. Although imperialism and colonialism focus on the suppression of an other, if colonialism refers to the process of a country taking physical control of another, imperialism refers to the political and monetary dominance, either formally or informally. Colonialism is seen to be the architect deciding how to start dominating areas and then imperialism can be seen as creating the idea behind conquest cooperating with colonialism. Colonialism is when the imperial nation begins a conquest over an area and then eventually is able to rule over the areas the previous nation had controlled. Colonialism's core meaning is the exploitation of the valuable assets and supplies of the nation that was conquered and the conquering nation then gaining the benefits from the spoils of the war. The meaning of imperialism is to create an empire, by conquering the other state's lands and therefore increasing its own dominance. Colonialism is the builder and preserver of the colonial possessions in an area by a population coming from a foreign region. Colonialism can completely change the existing social structure, physical structure and economics of an area; it is not unusual that the characteristics of the conquering peoples are inherited by the conquered indigenous populations.

Question: what do conquering people take away from native populations?


Context: Bills can be introduced to Parliament in a number of ways; the Scottish Government can introduce new laws or amendments to existing laws as a bill; a committee of the Parliament can present a bill in one of the areas under its remit; a member of the Scottish Parliament can introduce a bill as a private member; or a private bill can be submitted to Parliament by an outside proposer. Most draft laws are government bills introduced by ministers in the governing party. Bills pass through Parliament in a number of stages:

Question: Who may also submit private bills to Parliament?

an outside proposer
an outside proposer
an outside proposer


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Raise a cup up for all my day ones
Two middle fingers for the haters
Lifes only getting greater
Straight up from nothing we go
Higher than the highest skyscraper
No Little League, we major
The proof is in the paper
We put the good in the good in the good life
We put the good in the good in the good life
We put the bad in the past, now we alright
Eazy
Ayy, ayy, ayy, ayy
Kehlani, I got you
Ayy, yeah
And its a feelin that I cant explain
How you make it and your team still stay the same
Stay down from the jump and they never change
Man, this a moment I could never trade, yeah
I told my moms not to stress no more
Go hit the Bentley store and no credit card debts no more
I bought the crib and its in escrow now
So you dont ever have to worry about how you gon pay rent no more
I put my team in position, now they makin a killin
Stackin blue faces straight to the ceilin
Out in Vegas Im with em
Orderin bottles of that Ace when they sit em
Til there aint enough space up on the table to fit em
Go ahead and
Raise a cup up for all my day ones
Two middle fingers for the haters
Lifes only getting greater
Straight up from nothing we go
Higher than the highest skyscraper
No Little League, we major
The proof is in the paper
We put the good in the good in the good life
The good life
We put the good in the good in the good life
I said the good life
We put the bad in the past, now we alright
We alright
Ayy, ayy, ayy, ayy
Yeah, yeah
Ayy, yeah
Pour some Clicquot in the glass, have a toast to success
No lookin back from here, no more bein broke and distressed
I put my heart into this game like I opened my chest
We only pray for more Ms while you hope for the best
We make these plays, man Im finessin these checks
Times up for everybody, Im collectin on debts
And I swear this champagne just tastes better on jets
Im just out here bein great, man, this as real as it gets
I put my team in position, now they makin a killin
Stackin blue faces straight to the ceilin
Out in Vegas Im with em
Orderin bottles of that Ace when they sit em
Til there aint enough space up on the table to fit em
Go ahead and
Raise a cup up for all my day ones
Two middle fingers for the haters
Lifes only getting greater
Straight up from nothing we go
Yeah, go up
Higher than the highest skyscraper
No Little League, we major
Yeah
The proof is in the paper
You know
We put the good in the good in the good life
The good life
We put the good in the good in the good life
I said the good life
We put the bad in the past, now we alright
We alright
Ayy, ayy, ayy, ayy
Yeah, yeah
Ayy, yeah
Damn right, from the bottom we rise
So high, now we cover sky lights
Were building an empire
We owe it all to each other
Just look at us right now, destined
Were so good right now, legend
Heres to you and I
Raise em to the sky
We put the good in the good in the good life
Yeah
We put the good in the good in the good life
Yeah
We put the bad in the past, now we alright
Yeah, you know, uh
We put the good in the good in the good life
The good life
We put the good in the good in the good life
I said the good life
We put the bad in the past, now we alright
We alright
Ayy, ayy, ayy, ayy
Uh
Ayy, yeah
Uh, the good life


Ooh, ooh
Ring, ring, ring, ring
You dont hit my line no more, oh, oh
You dont make it ring, ring, ring, ring
I cant keep this on the low
I want you to make it ring, ring, ring, ring
Should I call first? I cant decide
I want to, but a bitch got pride
The switchin up shit is what I cant fuck with
Im feelin you but you hard to get in touch with
And you aint hit me up in a while
Actin like you dont know what number to dial
You quit, then thats it, Ima throw in the towel
Cause a nigga only gon do what you allow
You dont want this gun smoke
Learn to text with your nose if your thumb broke
I dont care if we get into it and I stall on your ass
Better still wake up to missed calls from your ass, nigga
You dont hit my line no more, oh, oh
You dont make it ring, ring, ring, ring
I cant keep this on the low
I want you to make it ring, ring, ring, ring
Nah, nigga, now you gon have to call me
Cause Im lookin at these messages, they on me
Actin like they aint niggas that want me
Let another nigga in your spot, and you gon be hot, nigga, coffee
You gon be sick to your, stomach
Hit me when you free, 1-800
Its emergency, call me 911
Cause right now Im out here tryna find someone
The ring on my phone, ring on my finger
You actin like you aint tryna do either
Once a good girl, watch me turn diva
Here goes my heart, I put it on speaker
You dont hit my line no more, oh, oh
You dont make it ring, ring, ring, ring
I cant keep this on the low
I want you to make it ring, ring, ring, ring
You used to be on my line
On my tick all the time, yeah
Love it when you make me feel
Like you dont mind when I aint got time for you
And no it dont go to my head, Im only arrogant in bed
I just love to know you wanna spend time with me instead
Now you all caught up, yeah
You all caught up and you done left me alone, yeah
You was all fed up
Ready for the next step, wanna be on your own
Said I just miss you, I just miss us, baby
All I know is
You dont hit my line no more, oh, oh
You dont make it ring, ring, ring, ring
I cant keep this on the low
I want you to make it ring, ring, ring, ring


I like my girls just like I like my honey; sweet
A little selfish
I like my women like I like my money; green
A little jealous
Cause Im a beautiful wreck
A colorful mess, but Im funny
Oh, Im a heartbreak vet
With a stone-cold neck, yeah, Im charming
All the pretty girls in the world
But Im in this space with you
Colored out the lines
I came to find, my fire was fate with you
Heartache would stay with you
Fly great escapes with you
I countdown to the clock, saw you awake
Dont walk away, or would you wait for me?
I go out to the bar, fuck hangin with the stars
Dont even have a car, but you would wait for me
All, all, all, all the pretty girls in the world
But Im in this space with you
Colored out the lines
I came to find, my fire was fate with you
My heartache would stay with you
Escape with you
I like my girls just like I like my honey; sweet
A little selfish, huh
I like my women like I like my money; green
A little jealous
Oh, Im a beautiful wreck
A colorful mess, but Im funny
Oh, Im a heartbreak vet
With a stone-cold neck, Im so charming, oh, oh
La-la-la-la-la-la-la
Do-do-do do-do
Do-do-do do-do
Do-do-do do-do
Da-da-da da-da
Do-do-do do-do
Isnt love all we need? Is it love?
Do-do-do do-do
The Beatles say prophecy is love
Do-do-do do-do
Do-re-mi-fa-so-la-ti, is it love?
Do-do-do do-do
Love, do-do-do do-do


You act like you need remindin
Tryna do it over, bring it back and rewind it
But all that glitters isnt gold, I was blinded
Should have never gave you my heart on consignment
And I cant believe the lies that I went for
Thought you was mine, but you decided to be with him though
You took my feelings and just threw em out the window
Feel like its too hard to fall in love again, no
On some nights like this, shawty, I cant help but think of us
Ive been reminiscin, sippin, missin ya
Can you tell me whats with all this distant love?
If I called, would you pick it up?
On some nights like this, I just wanna text you, but for what?
You gon say you want me, then go switch it up
Just gon play with my emotions just because, no
All them times I played the fool for you
Thinkin we could put it back together, thought we had forever
You never see my point of view
Our connection is so severed, you dont show no effort
And I cant believe the lies that I went for
Thought you was mine, but you decided to be with him though
Took my feelings and just threw em out the window
Feel like its too hard to fall in love again, no
On some nights like this, shawty, I cant help but think of us
Ive been reminiscin, sippin, missin ya
Can you tell me whats with all this distant love?
If I called, would you pick it up?
On some nights like this, I just wanna text you, but for what?
You gon say you want me, then go switch it up
Just gon play with my emotions just because, no
You gon get my hopes high, girl
You gon get my hopes high, girl
Just gon tell me more lies, girl
Just gon get my hopes high, girl
Ive been way too good to you, you take me for granted
You was my day one since back at Big Bs house on Adams
First day that we met, I flagged you down, I told you, Hit my line
Used to promise me youd never switch on me like Gemini
You think Im a fool, aint nobody stupid
I see all the signs, I see all the clues
Yeah, sometimes I reminisce bout that shit when Im bingin
Cant believe its been a whole year, yeah, but...
On some nights like this, shawty, I cant help but think of us
Ive been reminiscin, sippin, missin ya
Can you tell me whats with all this distant love?
If I called, would you pick it up?
On some nights like this, I just wanna text you, but for what?
You gon say you want me, then go switch it up
Just gon play with my emotions just because, no
You gon get my hopes high, girl
You gon get my hopes high, girl
Just gon tell me more lies, girl
Just gon get my hopes high, girl


Pray to God, but Im feeling like hes going deaf
Now when I lean on you and I got nothing left
Hey, Ive been wanting to call ya, tell you that Im sorry
Same old fucking story everybody sing
And I say Im okay, but I guess Im a liar
You say youre okay, but I saw that you liked it
2 AM and faded, I know thats when you like it
Know thats when you miss me, know thats when you crying
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Nowadays, Im just a bitch to everybody else
I dont need no shoulders, Im good crying by myself
Moving ons a chore, cause you know I still adore ya
An unrequited love is just a lovers hell
And I say Im okay, but I guess Im a liar
You say youre okay, but I saw that you liked it
2 AM and faded, I know thats when you like it
Know thats when you miss me, know thats when you crying
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Im not gonna act like I dont love ya baby
Cause deep in my mind, girl, I know I do
Tried to search all through the world and not well
But I cant find a girl who looks close like you
I done made millions of dollars
But Im still alone until I come home back to you
I remember all of the times we were parked by your house
And laughed all on your avenue
Whoa, you cant front, youre a stone cold diva
I had to get counseling from my moms
Shes a heartbreak teacher
Remember that time I put those pepperonis on your face
Made you a creature
Now I think about you every single time I eat pizza, ohh
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Why you, why you, why you checking if youre over it?
Why you, why you say Let go if youre still holding it?
Just a little bit better at faking it than me, baby
Just a little bit better at faking it than me, baby
Why you holding me?
Why you holding me?
Oh, she killed that shit
She was killing it, that was hard, bruh
I didnt know she could get that high but she killed that
Go Lani, go Lani


Yeah, yeah, yeah-eah-eah-eah, yeah-eah, yeah-eah
Yeah, yeah, yeah, yeah, yeah, yeah, yeah-eah
She talkin that noise, take her lovin with the dawn, all while I talk on the phone
After we fuck in the morn, she wake up, she wearin my clothes
She always be callin my phone, she always be stealin my clothes, ayy
Askin me, How does it feel when you know you could buy out the store?, ayy
Im Bathin Ape down to the floor, ayy, Im droppin the four in the foreign, ayy
I came a long way on my own, ayy, Im doin this shit on my own, ayy
I dont give a fuck what Im told, ayy, I came a long way on my own, ayy
Now her pussy made out of gold, ayy, I swear her pussy ownin my soul
She got that sauce, yeah, four days a hundred thousand
Forever like a diamond, she bring me back to life, yeah
Im so fly, Im martian, quit talkin all that nonsense
Im just tryna fuck you til you dont know nothin, oh-oh-oh
I cross my Ts and dot my Is, yeah, Im for real
He hold me down , thats my shield
He buy whatever, he know the drill , dont need no pill
He whispered in my ear and told me
Feel
Fee-eee-eee-eel
Fee-eee-eee-eee-eel
Oh-oh, oh-oh
He love that I say what I feel, he feel what I say cause its real
You couldnt forget, I never changed up on my set, and I only make calls to collect, thats why we connect
We can go half on a jet, baby, we on to the next, fuck all the stress
Fuckin with bitches whos new to the game when you got you a vet
I know you like it when I act like Im still shy
Then turn around and put that thing in overdrive, Im down to ride
Ima keep you on my shoulder
Cause every cold nigga need a bae thats ten times colder, no
I cross my Ts and dot my Is, yeah, Im for real
He hold me down , thats my shield
He buy whatever, he know the drill , dont need no pill
He whispered in my ear and told me
Feel
Fee-eee-eee-eel, ayy
Fee-eee-eee-eee-eel , oh
Oh-oh, oh-oh
Hey, fuck me til I cant see straight
Make me think that ho was a mistake
I just need to feel you all the time
Ride, ho, ride, ho, alright


the study of the equation of state ( eos ) , transport properties , and mixing rules of hydrogen ( h ) and helium ( he ) under extreme condition of high pressure and temperature is not only of fundamental interest but also of essential practical applications for astrophysics @xcite .
for instance , giant planets such as jupiter and saturn require accurate eos as the basic input into the respective interior models in order to solve hydrostatic equation and investigate the solubility of the rocky core @xcite . on the other side , the evolution of stars and the design of thermal protection system is assisted by high precision transport coefficients of h - he mixtures at high pressure @xcite . in addition ,
the viscosity and mutual diffusion coefficients are also important input properties for hydrodynamic simulations in modelling the stability of the hot spot - fuel interfaces and the degree of fuel contamination in inertial confinement fusion ( icf ) @xcite .    since direct experimental access such as shock wave experiments
is limited in the mbar regime @xcite , the states deep in the interior of jupiter ( @xmath2 mbar ) and saturn ( @xmath3 mbar ) @xcite can not be duplicated in the laboratory . as a consequence ,
theoretical modelling provides most of the insight into the internal structure of giant planets .
the eos of h - he mixtures have been treated by a linear mixing ( lm ) of the individual eos via fluid perturbation theory @xcite and monte carlo simulations @xcite . recently , several attempts have been made to calculate eos of h - he mixtures by means of quantum molecular dynamic ( qmd ) simulations .
@xcite applied local density approximation of density functional theory ( lda - dft ) calculations for solid h - he mixtures , implying demixing for jupiter and saturn at 15000 k for a he fraction of @xmath4 .
@xcite , lorenzen _ et al . _
@xcite , and militzer @xcite performed qmd simulations by using generalized gradient expansion ( gga ) instead of the lda in order to evaluate the accuracy of the lm approximation and study the demixing of h - he at mbar pressures .
@xcite introduced car - parrinello molecular dynamics ( cpmd ) simulations to calculate the excess gibbs free energy of mixing at a lower temperature compared to that set in the work of lorenzen _ et al .
_ @xcite and militzer @xcite .    considering the transport properties , qmd @xcite and orbital - free molecular dynamics ( ofmd ) @xcite simulations
have been introduced to study hydrogen and its isotropic deuterium ( d ) and tritium ( t ) .
self - diffusion coefficients in the pure h system and mutual diffusion for d - t mixtures were determined for temperatures @xmath51 to 10 ev and equivalent h mass densities 0.1 to 8.0 g / cm@xmath1 @xcite .
qmd and ofmd simulations of self - diffusion , mutual diffusion , and viscosity have recently been performed on heavier elements ( fe , au , be ) @xcite and on mixtures of li and h @xcite .
the present work selects h - he mixture as a representative system and examines some of the standard mixing rules with respect to the eos and transport properties ( viscosity , self and mutual diffusion coefficients ) in the warm dense regime that covers standard extreme condition as reached in the interiors of jupiter and saturn .
the thermophysical properties of the full mixture and the individual species have been derived from qmd simulations , where the electrons are quantum mechanically treated through finite - temperature ( ft ) dft and ions move classically . in the next section , we present the formalism for qmd and for determining the static and transport properties .
then , eos , viscosity , and diffusion coefficients for h - he mixtures are presented , and the qmd results are compared with the results from reduced models and qmd based linear mixing models . finally , concluding remarks are given .
in this section , a brief description of the fundamental formalism employed to investigate h - he mixtures is introduced .
the basic quantum mechanical density functional theory forms the basis of our simulations .
the implementation of schemes in determining diffusion and viscosity is discussed . mixing rules that combine pure species quantities to form composite properties
is also presented .
qmd simulations have been performed for h - he mixtures by using vienna _
ab initio _ simulation package ( vasp ) @xcite . in these simulations , the electrons are treated fully quantum mechanically by employing a plane - wave ft - dft description , where the electronic states follow the fermi - dirac distribution .
the ions move classically according to the forces from the electron density and the ion - ion repulsion .
simulations have been performed in the nvt ( canonical ) ensemble where the number of particles @xmath7 and the volume are fixed .
the system was assumed to be in local thermodynamic equilibrium with the electron and ion temperatures being equal ( @xmath8 ) . in these calculations ,
the electronic temperature has been kept constant according to fermi - dirac distribution , and ion temperature is controlled by noe thermostat @xcite .    at each step during md simulations , a set of electronic state functions [ @xmath9 for each * k*-point
are determined within kohn - sham construction by @xmath10 with @xmath11 in which the four terms respectively represent the kinetic contribution , the electron - ion interaction , the hartree contribution and the exchange - correlation term . the electronic density is obtained by @xmath12 then by applying the velocity verlet algorithm , based on the force from interactions between ions and electrons , a new set of positions and velocities are obtained for ions .
all simulations are performed with 256 atoms and 128 atoms for pure species of h and he , and as for the case of the h - he mixture , a total number of 245 atoms ( 234 h atoms and 11 he atoms ) for a mixing ratio @xmath13 ( corresponding to the h - he immiscibility region determined in the work of morales _ et al . _
@xcite ) has been adopted , where a cubic cell of length @xmath14 ( volume @xmath15 ) is periodically repeated .
the simulated densities range from 1.0 to 4.0 g / cm@xmath1 for pure h system . as for pure
he and h - he mixture , the size of the supercell is chosen to be the same as that for pure h to secure a constant electron number density ( in the range @xmath0/m@xmath1 ) . the temperature from 4000 k to 20000 k
has been selected to highlight the conditions in the interiors of jupiter and saturn .
the convergence of the thermodynamic quantities plays an important role in the accuracy of qmd simulations . in the present work ,
a plane - wave cutoff energy of 1200 ev is employed in all simulations so that the pressure is converged within 2% .
we have also checked out the convergence with respect to a systematic enlargement of the * k*-point set in the representation of the brillouin zone . in the molecular dynamic simulations ,
only the @xmath16 point of brillouin zone is included .
the dynamic simulation is lasted 20000 steps with time steps of 0.2 @xmath17 0.7 fs according to different densities and temperatures . for each pressure and temperature ,
the system is equilibrated within 0.5 @xmath17 1 ps .
the eos data are obtained by averaging over the final 1 @xmath17 3 ps molecular dynamic simulations .
the self - diffusion coefficient @xmath18 can either be calculated from the trajectory by the mean - square displacement @xmath19 or by the velocity autocorrelation function @xmath20 where @xmath21 is the position and @xmath22 is the velocity of the @xmath23th nucleus . only in the long - time limit , these two formulas of @xmath18 are formally equivalent .
sufficient lengths of the trajectories have been generated to secure contributions from the velocity autocorrelation function to the integral is zero , and the mean mean - square displacement away from the origin consistently fits to a straight line .
the diffusion coefficient obtained from these two approaches lie within 1 % accuracy of each other .
here , we report the results from velocity autocorrelation function .
we have also computed the mutual - diffusion coefficient @xmath24 from the autocorrelation function @xmath25 with @xmath26 where the concentration and particle number of species @xmath27 are denoted by @xmath28 and @xmath29 , respectively , and the total number of particles in the simulation box @xmath30 .
the quantity @xmath31 is the thermodynamic factor related to the second derivation of the gibbs free energy with respect to concentrations @xcite . in the present simulations ,
@xmath31 value has been adopted equal to unity since studies with leonard - jones and other model potentials have shown that for dissimilar constituents the @xmath31-factor departs from unity by about 10% @xcite .
the viscosity @xmath32 has been computed from the autocorrelation function of the off - diagonal component of the stress tensor @xcite @xmath33 the results are averaged from the five independent off - diagonal components of the stress tensor @xmath34 , @xmath35 , @xmath36 , @xmath37 , and @xmath38 .
different from the self - diffusion coefficient , which involves single - particle correlations and attains significant statistical improvement from averaging over the particles , the viscosity depends on the entire system and thus needs very long trajectories so as to gain statistical accuracy . to shorten the length of the trajectory , we use empirical fits @xcite to the integrals of the autocorrelation functions .
thus , extrapolation of the fits to @xmath39 can more effectively determine the basic dynamical properties .
both of the @xmath18 and @xmath40 have been fit to the functional in the form of @xmath41 $ ] , where @xmath42 and @xmath43 are free parameters .
reasonable approximation to the viscosity can be produced from the finite time fitting procedure , which also serves to damp the long - time fluctuations .
the fractional statistical error in calculating a correlation function @xmath44 for molecular - dynamics trajectories @xcite can be given by @xmath45 where @xmath43 is the correlation time of the function , and @xmath46 is the length of the trajectory .
in the present work , we generally fitted over a time interval of [ 0 , @xmath47 .      here
, we examine two representative mixing rules .
the first , termed density - matching rule ( mrd ) with the inspiration of a two - species ideal gas .
the second , termed pressure - matching rule ( mrp ) , which follows from two interacting immiscible fluids .    in the mrd
, the volume of the individual species is set equal to that of the mixture ( @xmath48 ) , and qmd simulations are performed for h at a density of @xmath49 and he at @xmath50 at a temperature @xmath51 .
then , pressure predicted by mrd is determined by simply adding the individual pressures from the pure species h and he simulations .
other transport coefficients , such as mutual diffusion and viscosity , follow the same prescription and are summarized as @xmath52 the superscript is used to denote values predicted from mrd .
the derived pressure based on density mixing rule generally follows from the ideal noninteracting h and he gas in a volume @xmath53 .
the mrp has a more complicated construction compared to mrd .
mrp can be characterized as the following prescription : @xmath54 in this case , we have performed a series of qmd simulations on the individual species h and he , where the volumes change under a constraint @xmath55 until the individual pressures equal to each other @xmath56 .
the total pressure becomes the predicted value .
here , we use the excess or electronic pressure @xmath57 to evaluate this mrp mixing rule .
composite properties such as mutual diffusion and viscosity are evaluated by combining the individual species results via volume fractions @xmath58 .
finally , we also derive properties of the mixture from a slightly more complex mixing rule @xcite , as so - called binary ionic mixture ( bim ) : @xmath59 with @xmath60 the predicted mutual - diffusion coefficient or the viscosity .
the subscript @xmath61 denotes the mixture and @xmath23 the pure species .
in this section , the wealth of information derived from qmd calculations are mainly presented through figures , and the general trends of the eos as well as transport coefficients are concentrated in the text .
it is , therefore , interesting to explore not only to get insight into the interior physical properties of giant gas planets but also to examine a series of mixing rules for hydrogen and helium .
additionally , one can consider the influence of helium on the eos and transport coefficients of mixing .
high precision eos data of hydrogen and helium are essential for understanding the evolution of jupiter and target implosion in icf .
experimentally , the eos of hydrogen and helium in the fluid regime have been studied through gas gun @xcite , chemical explosive @xcite , magnetic driven plate flyer @xcite , and high power laser @xcite . since these experiments were limited by the conservation of mass , momentum , and energy , the explored density of warm dense matter
were limited within @xmath62 times of the initial density .
recently , a new technique combined diamond anvil cell ( dac ) and high intensity laser pulse has successfully been proved to provide visible ways to generate shock huguniot data of hydrogen over a significantly broader density - temperature regime than previous experiments @xcite
. however , the density therein was still restricted within 1 g / cm@xmath1 .        in our simulations , wide range eos for h
, he , and h - he mixtures have been determined according to qmd method .
the eos can be divided into two parts that is , contributions from the noninteracting motion of ions ( @xmath63 ) and the electronic term ( @xmath64 ) , @xmath65 where @xmath64 is calculated directly through dft . in fig .
[ fig_eos1 ] ( a ) , we have compared our results of @xmath64 with that of holst _ et al . _
@xcite , where the electronic pressure is expressed as a smooth function in terms of density and temperature , and the results agree with each other with a very slight difference ( accuracy within 5% ) . in the simulated density and temperature regime
, we do not find any signs indicating a liquid - liquid phase transition ( @xmath66 ) or plasma phase transition ( @xmath67 ) , which are characterized by molecular dissociation and ionization of electrons , respectively . with considering the mixing of he into h ,
the electronic pressure is effectively reduced , as has been shown in fig .
[ fig_eos1 ] ( b ) .
mrd accounts for contribution from noninteracting h and he subsystems in the volume of the mixtures . in mrd ,
the pressure contributed from noninteracting ions is the same as that of the mixture , but the electronic pressure is much lower due to the low electronic density in the pure species simulations .
it is indicated that the electronic pressure is underestimated by mrd model at about 8% @xmath17 9% ( see fig .
[ fig_eos2 ] ) . for mrp model
, we have firstly performed a series of pure species simulations at a wider density ( temperature ) regime compared to h - he mixtures .
then , the simulated eos data are fitted into smooth functions in terms of density and temperature . under the constraint of @xmath68
, we have predicted the electronic pressures @xmath69 according to mrp model by solving pure species eos function at certain densities and temperatures , as shown in fig .
[ fig_eos2 ] .
it is indicated that the mrp model agrees better with direct qmd simulations ( accuracy within 3% ) , the difference mainly come from the ionic interactions between h and he species after mixing .       and 8 g / cm@xmath1 , respectively .
( a ) self - diffusion coefficient ; ( b ) viscosity .
the direct qmd simulated results are presented by black crosses , while the fitted results are denoted by blue dashed lines . ]
qmd simulations have been performed within the framework of ft - dft to benchmark the dynamic properties of h , he , and h - he mixture in the wdm regime .
illustrations for the self - diffusion coefficients and viscosity ( for h and he at densities of 2.0 g / cm@xmath1 and 8.0 g / cm@xmath1 , respectively ) at a temperature 12000 k , as well as their fits are shown in fig . [ fig_dandeta ] .
the trajectory of the present simulations lasts 4.0 @xmath17 14.0 ps , and correlation times between 1.0 and 15.0 fs . as a consequence ,
the computational error for the viscosity lies within 10% .
after accounting for the fitting error and extrapolation to infinite time , a total uncertainty of @xmath17 20% can be estimated .
the uncertainty in the self - diffusion coefficients is smaller than 1% , due to the additional @xmath70 advantage given by particle average .    .
for helium , the density is 8 g / cm@xmath1 .
the electron number density for pure species ( h and he ) is @xmath71/m@xmath1 .
]    dynamic properties of wdm are generally governed by two dimensionless quantities , namely , ionic coupling ( @xmath16 ) and electronic degenerate ( @xmath72 ) parameter .
the former one is defined by the ratio of the potential to kinetic energy @xmath73 , with @xmath74 the ionic charge , and @xmath75 the ion - sphere radius ( @xmath76 is the number density ) . the latter one @xmath77 , where @xmath78 is fermi temperature .
it has been reported that dynamic properties such as diffusion coefficients and viscosity can be represented purely in terms of ionic coupling parameter @xmath16 according to molecular dynamics or monte carlo simulations based on one component plasma ( ocp ) model @xcite , where ions move classically in a neutralizing background of electrons .
for instance , hansen _
@xcite introduced a memory function to analyze the velocity autocorrelation function , and obtain the diffusion coefficient in terms of @xmath79 with the plasma frequency @xmath80 .
based on classical molecular dynamic simulations , bastea @xcite has fitted the viscosity into the following form @xmath81 with @xmath82 , @xmath83 , @xmath84 , and @xmath85 .
since ocp model is restricted to a fully ionized plasma , we use @xmath74=1.0 ( or 2.0 ) for hydrogen ( or helium ) to compute the self - diffusion coefficient and viscosity . in fig .
[ fig_qmd_ocp ] ( a ) , we show comparison between qmd and ocp model @xcite for hydrogen and helium at densities of 2 g / cm@xmath1 and 8 g / cm@xmath1 .
the general tendency for the self - diffusion coefficient with respect to temperature is similar for qmd and ocp model , however , the difference up to @xmath1760 % is observed between the two results . for the viscosity [ fig .
[ fig_qmd_ocp ] ( b ) ] , ocp @xcite predicts smaller ( larger ) values for hydrogen ( helium ) compared to qmd simulations .
the viscosity is governed by interactions between particles and ionic motions , contribution from the former one decrease with the increase of temperature , while , it increases for the latter one . as a consequence
, the viscosity may have local minimum along temperature . for hydrogen
, the local minimum locates around 10000 k and 14000 k indicated by qmd and ocp model , respectively . while in the case of helium
, we do not observe any signs for the local minimum in the simulated regime .
/m@xmath1 and temperature from 4000 @xmath17 20000 k. ]    in fig .
[ fig_mix ] , we have shown the mutual diffusion coefficient @xmath86 and viscosity @xmath87 for h - he mixture with an electron number density of @xmath88/m@xmath1 , and results from mixing models are also provided .
the transport coefficients predicted by mrd can be directly evaluated through eq .
( [ eq_mrd ] ) . for mrp model ,
we have firstly fitted the self - diffusion coefficients and viscosity in terms of density and temperature , after determining the volume for each species under the constraint of @xmath89 , the transport coefficients are then obtained . in bim model , we have used @xmath90 and @xmath91 , then , the transport coefficients are determined by eq .
( [ eq_bim ] ) . here
we would like to stress that in some mixture studies based on average atom models , the properties of pure species are derived from perturbed - atom models , where boundary conditions are introduced from the surrounding medium by treating a single atom within a cell . in the present work ,
the dynamic properties of different mixing rules originate from qmd calculations of the individual species . despite divorced of the h -
he interactions , the pure species calculations still contain complex intra - atomic interactions based on large samples of atoms .
the mutual diffusion coefficient of h - he mixture shows a linear increase with respect of temperature , as indicated in fig .
[ fig_mix](a ) .
the data from mrp and bim models have a better agreement with qmd simulations compared with that of the mrd model , where ion densities are reduced and results in a larger diffusion coefficient .
the viscosity of h - he mixture has a more complex behavior than pure species under extreme condition . as shown in fig .
[ fig_mix ] ( b ) , mrd is valid at low temperature , while mrp works at higher temperature .
bim rule moves the results into better agreement with the h - he mixture , leaving within 30% or better for the simulated conditions .
in summary , we have performed systematic qmd simulations of h , he , and h - he mixture in the warm dense regime for electron number density ranging from @xmath0/m@xmath1 and for temperatures from 4000 to 20000 k. the present study concentrated on thermophysical properties such as the eos , diffusion coefficient , and viscosity , which are of crucial interest in astrophysics and icf .
various mixing rules have been introduced to predict dynamical properties from qmd simulations of the pure species and compare with direct calculations on the fully interacting mixture .
we have shown that mrd and mrp rules produce pressures within about 10 % of the h - he mixture , however , the mutual diffusion coefficients are as different as 75 % and it is 50 % for the viscosity .
bim rule generally gives better agreement with the mixture results .
we have also compared our qmd results with ocp model for the pure species .
this work was supported by nsfc under grants no .
11275032 , no . 11005012 and no . 51071032 , by the national basic security research program of china , and by the national high - tech icf committee of china .
99 w. b. hubbard , science * 214 * , 145 ( 1981 ) . h. f. wilson and b. militzer , astrophys .
j. * 745 * , 54 ( 2012 ) .
h. f. wilson and b. militzer , phys .
lett . * 108 * , 111101 ( 2012 ) .
d. bruno , c. catalfamo , m. capitelli , g. colonna , o. de pascale , p. diomede , c. gorse , a. laricchiuta , s. longo , d. giordano , and f. pirani , phys .
plasmas * 17 * , 112315 ( 2010 ) . s. atzeni and j. meyer - ter - vehn , _ the physics of inertial fusion : beam plasma interaction , hydrodynamics , hot dense matter _ , international series of monographs on physics ( clarendon press , oxford , 2004 ) .    j. d. lindl , _ inertial confinement fusion : the quest for ignition and energy gain using indirect drive _ , ( springer - verlag , new york , 1998 ) .
m. d. knudson and m. p. desjarlais , phys .
lett . * 103 * , 225501 ( 2009 ) .
w. lorenzen , b. holst , and r. redmer , phys .
lett . * 102 * , 115701 ( 2009 ) .
d. j. stevenson , phys .
b * 12 * , 3999 ( 1975 ) .
w. b. hubbard and h. e. dewitt , astrophys .
j. * 290 * , 388 ( 1985 ) .
j. e. klepeis , k. j. schafer , t. w. barbee iii , and m. ross , science * 254 * , 986 ( 1991 ) .
j. vorberger , i. tamblyn , b. militzer , and s. a. bonev , phys .
b * 75 * , 024206 ( 2007 ) .
b. militzer , phys .
b * 87 * , 014202 ( 2013 ) .
o. pfaffenzeller , d. hohl , and p. ballone , phys .
lett . * 74 * , 2599 ( 1995 ) .
l. a. collins , j. d. kress , d. l. lynch , and n. troullier , j. quant .
transf . * 51 * , 65 ( 1994 ) .
i. kwon , j. d. kress , and l. a. collins , phys .
b * 50 * , 9118 ( 1994 ) .
l. collins , i. kwon , j. kress , n. troullier , and d. lynch , phys .
e * 52 * , 6202 ( 1995 ) .
j. clrouin and s. bernard , phys .
e * 56 * , 3534 ( 1997 ) .
i. kwon , l. collins , j. kress , and n. troullier , epl * 29 * , 537 ( 1995 ) .
j. clrouin and j .- f .
dufrche , phys .
e * 64 * , 066406 ( 2001 ) .
j. d. kress , j. s. cohen , d. a. horner , f. lambert , and l. a. collins , phys .
e * 82 * , 036404 ( 2010 ) .
f. lambert , j. clouin , and s. mazevet , epl * 75 * , 681 ( 2006 ) .
f. lambert , j. clouin , and g. zrah , phys .
e * 73 * , 016403 ( 2006 ) . c. wang , y. long , x .-
he , and p. zhang , phys .
e * 87 * , 043105 ( 2013 ) .
d. a. horner , f. lambert , j. d. kress , and l. a. collins , phys .
b * 80 * , 024305 ( 2009 ) .
m. a. morales , c. pierleoni , e. schwegler , and d. m. ceperley , proc .
* 106 * , 1324 ( 2009 ) .
j. p. hansen and i. r. mcdonald , _ the theory of simple liquids _ , 2nd ed .
( academic press , new york , 1986 ) , chap . 8 .
m. schoen and c. hoheisel , mol.phys .
* 52 * , 33 ( 1984 ) ; * 52 * , 1029 ( 1984 ) .
m. p. allen and d. j. tildesley , _ computer simulation of liquids _
( oxford university press , new york , 1987 ) . j. d. kress , james s. cohen , d. p. kilcrease , d. a. horner , and l. a. collins , phys .
e * 83 * , 026404 ( 2011 ) .
r. zwanzig and n. k. ailawadi , phys . rev . * 182 * , 280 ( 1969 ) .
s. bastea , phys .
e * 71 * , 056405 ( 2005 ) . w. j. nellis , rep .
* 69 * , 1479 ( 2006 ) .
g. v. boriskov , a. i. bykov , r. ilkaev , v. d. selemir , g. v. simakov , r. f. trunin , v. d. urlin , a. n. shuikin , and w. j. nellis , phys .
b * 71 * , 092104 ( 2005 )
. m. d. knudson , d. l. hanson , j. e. bailey , c. a. hall , j. r. asay , and c. deeney , phys .
b * 69 * , 144209 ( 2004 ) .
g. w. collins , l. b. da silva , p. celliers , d. m. gold , m. e. foord , r. j. wallace , a. ng , s. v. weber , k. s. budil , and r. cauble , science * 281 * , 1178 ( 1998 ) .
t. r. boehly , d. g. hicks , p. m. celliers , t. j. b. collins , r. earley , j. h. eggert , d. jacobs - perkins , s. j. moon , e. vianello , d. d. meyerhofer , and g. w. collins , phys .
plasmas * 11 * , l49 ( 2004 ) .
d. g. hicks , t. r. boehly , p. m. celliers , j. h. eggert , s. j. moon , d. d. meyerhofer , and g. w. collins , phys .
b * 79 * , 014112 ( 2009 ) .
p. loubeyre , s. btygoo , j. eggert , p. m. celliers , d. k. spaulding , j. r. rygg , t. r. boehly , g. w. collins , and r. jeanloz , phys .
b * 86 * , 144115 ( 2012 ) .
b. holst , r. redmer , and m. p. desjarlais , phys .
b * 77 * , 184201 ( 2008 ) .
f. lambert , ph.d .
thesis , universit paris xi .
commissariat l nergie atomique , 2007 .
b. bernu and p. vieillefosse , phys .
a * 18 * , 2345 ( 1978 ) .
z. donk , b. nyri , l. szalai , and s. holl , phys .
lett . * 81 * , 1622 ( 1998 ) ; z. donk and b. nyri , phys .
plasmas * 7 * , 45 ( 2000 ) .
j. daligault , phys .
lett . * 96 * , 065003 ( 2006 ) ; * 103 * , 029901(e ) ( 2009 ) . j. p. hansen , i. r. mcdonald , and e. l. pollock , phys
a * 11 * , 1025 ( 1975 ) .
r. m. more , adv . at .
* 21 * , 305 ( 1985 ) .

 thermophysical properties of hydrogen , helium , and hydrogen - helium mixtures have been investigated in the warm dense matter regime at electron number densities ranging from @xmath0/m@xmath1 and temperatures from 4000 to 20000 k via quantum molecular dynamics simulations .
 we focus on the dynamical properties such as the equation of states , diffusion coefficients , and viscosity . mixing rules ( density matching , pressure matching , and binary ionic mixing rules )
 have been validated by checking composite properties of pure species against that of the fully interacting mixture derived from qmd simulations .
 these mixing rules reproduce pressures within 10% accuracy , while it is 75 % and 50 % for the diffusion and viscosity , respectively .
 binary ionic mixing rule moves the results into better agreement .
 predictions from one component plasma model are also provided and discussed .


kouveliotou ( 1993 ) showed that the durations of gamma ray bursts ( grbs ) have a bimodal distribution , with roughly a third of the observed bursts corresponding to a short duration ( @xmath6 s ) population , and the remaining two - thirds belonging to a long duration ( @xmath7 s ) population .
searches for transient x - ray , optical and radio afterglow emission have so far been largely limited to long duration bursts .
this is because the italian - dutch bepposax satellite and other presently active instruments , which have been used to obtain well - determined grb coordinates , are sensitive only to bursts longer than a few seconds .
most of the x - ray follow - ups of long grbs have been successful , and 35 x - ray afterglows have been detected so far ( mid-2001 ) .
the success rate of optical searches has been somewhat less ( lazzati , covino & ghisellini 2001 ; fynbo 2001 ) , and 23 optical afterglows have been detected ; the majority of optical afterglows have yielded redshifts .
the success rate in radio has been comparable to that in the optical .    among short grbs , optical and radio searches for afterglows
have so far been carried out for only four sources that happened to be well localized by the interplanetary network ( hurley 2001 ) .
no afterglow emission was detected , but the sensitivity of the searches was not very high .
more searches will be carried out in the future when rapid arc - minute localizations of short grbs become routinely available from the upcoming hete ii and swift satellites .    in this _
, we make reasonable assumptions about the physical parameters of short grbs and estimate the broadband afterglow emission to be expected from these bursts .
the results may be useful for designing search strategies for afterglows of short grbs .
the predictions for the light - curves of the afterglows depend on some key parameters .
we attempt to estimate the relative magnitudes of these parameters in short and long grbs using observational data and some theoretical ideas .
studies of the temporal and spectral properties of short and long grbs have revealed that the burst duration is anticorrelated with the spectral hardness ( kouveliotou 1993 ) .
the peak frequency of the @xmath8 spectrum increases with the bulk lorentz factor of the grb in the external shock model for producing @xmath0-ray emission ( rees & mszros 1992 ; piran , shemi & narayan 1993 ; katz 1994 ) , however the relationship is complicated in the internal shock model ( see piran 1999 for a review ) .
fortunately , the lorentz factor ( lf ) of the late - time grb remnant which produces the afterglow is practically independent of the lf during the early grb phase , and so it is unlikely that any difference in the initial lf for the long and the short duration grbs will have any effect on the afterglow flux .
we note , however , that if the initial jet opening angle @xmath9 for short duration grbs were larger than longer lasting grbs , it will cause the afterglows of short grbs to become considerably dimmer since the jet transition time ( see  3 ) varies as @xmath10 .    by analysing a sample of over 400 grbs , and allowing for observational bias against detecting weak and long bursts with peak fluxes below the detection threshold ,
lee & petrosian ( 1997 ) showed that there is a highly significant positive correlation between the burst fluence and duration . in another study ,
mukherjee ( 1998 ) used two multivariate clustering methods to show that most of the structure in the multidimensional space of burst observations is contained in three fundamental quantities : duration , fluence , and spectral hardness . according to their analysis , short / hard grbs have a 25 kev1 mev fluence @xmath11 ( in cgs units ) of approximately @xmath12 , while long / soft grbs have @xmath13 .
short bursts thus have about 20 times less fluence than long bursts ( see also mao et al . 1994 , piran 1996 ) .
figure 1 shows the 25 kev1mev fluences @xmath11 and the durations @xmath14 of 34 long grbs for which afterglows have been observed .
the average duration for these grbs is @xmath15 , similar to that of the 486 long bursts analyzed by mukherjee ( 1998 ) from the third batse catalog ( meegan 1996 ) .
the average fluence of long grbs with afterglows is @xmath16 , implying that these bursts are , on average , approximately twice as bright as the long bursts analyzed by mukherjee et al .
( 1998 ) and 40 times more energetic than the 203 short bursts analyzed by them .
the grb energy output is determined by the kinetic energy of the relativistic outflow and the efficiency with which dissipative and radiative mechanisms convert some of the energy into @xmath0-ray emission . assuming that grbs arise from internal shocks in unsteady winds , the dissipation efficiency is determined by the magnitude of the fluctuations in the ejection lorentz factors of various parts of the outflow .
our present understanding of the properties of grb progenitors does not allow us to establish a correlation between the grb duration and efficiency .
it is possible that short grbs are somewhat less efficient than long grbs because the radius at which internal shocks occur in short grbs is closer to the photospheric radius ( kumar 1999 ) , so that some of the emission may be degraded by multiple scattering . ignoring this effect
, we expect the ratio of the kinetic energies of short and long grbs to be the ratio of their fluences , i.e. , a factor of about 20 .
we finally discuss the environments in which short and long bursts take place .
the existence of these two clearly distinct populations of grbs probably implies different physical origins .
most models of grbs  mergers of binary neutron stars ( ns  ns ) , black hole ( bh)ns , or bh  white dwarf ( wd ) , and failed supernovae / collapsars  involve the formation of a bh surrounded by a disk of debris .
the spin energy of the hole and the gravitational , thermal , and rotational energy of the disk represent the available reservoirs to power the @xmath17 ergs required for the grb .
the bh spin may be tapped by the blandford - znajek process ( 1977 ) , and the disk energy may be extracted either via neutrino annihilation ( eichler et al . 1989 ) or via magnetic fields / flares ( narayan , paczyski & piran 1992 ; see mszros , rees & wijers 1999 for a review ) .    the burst duration is determined both by the timescale for ejecting the relativistic outflow , and by the processes that @xmath18 shape the outflow dynamics until the gas reaches the region where the @xmath0-ray photons are emitted , such as the penetration of the grb jet through the envelope of a collapsed star , and @xmath19 convert the outflow kinetic energy into @xmath0-rays . in those bursts where the high energy emission arises as the outflow energy is dissipated through interaction with the circumburst medium , grbs of long duration can be obtained even if the initial ejection is impulsive .
however , the general absence of signatures of an external shock in the temporal structure of grbs ( sari & piran 1997 ; ramirez - ruiz & fenimore 2000 ) indicates that the grb emission is produced in internal shocks over a small range of distances . if this is the case , then the grb duration is a direct measure of the time interval during which the `` central engine '' is active .    if grbs originate in ns
ns or ns - bh mergers ( goodman 1986 ; eichler 1989 ; paczyski 1991 ; narayan 1992 ; mszros & rees 1992 ; katz & canel 1996 ) , enough mass reaches the resulting bh to power the grb , provided the disk is sufficiently small and accretion is driven by neutrino cooling ( narayan , piran & kumar 2001 ) .
the expected duration of the relativistic wind ( and thus the grb ) is under 1 s. thus these progenitors can naturally produce short grbs .
the collapse of the iron core of a massive star ( collapsar model : woosley 1993 ; paczyski 1998 ) with intermediate angular momentum leads to the formation of a disk with a sufficient accretion rate to power a relativistic outflow lasting for 1020 s ( macfadyen & woosley 1999 ) .
the collapsar model is thus more appropriate for long grbs .
if the core collapse produces a ns and an out - going shock , the bh and the torus form when the ejected matter , lacking sufficient momentum , falls back ( macfadyen , woosley & heger 2001 ) . in this model
the grb duration is set by the dynamics of the fallback , and most likely would accommodate only the longest grbs , lasting for more than 100 s. long grbs could also arise from wd  bh ( fryer 1999 ) or helium star  bh mergers ( zhang & fryer 2001 ) , which lead to the formation of larger disks with accretion times above 10 s. however , it is likely that the gas will accrete via a convection - dominated accretion flow in these systems , in which case the flow is likely to be rather inefficient at extracting the disk energy ( narayan 2001 ) .    according to these ideas ,
then , there is a clear association between the type of grb progenitor and the burst duration .
short grbs are likely to involve merging ns binaries ( ns  ns or ns  bh ) , which should occur predominantly in the low density halo of the host galaxy , given the velocities of a few hundred @xmath20 acquired by the ns at birth and the binary coalescence time of about 100 myr .
long grbs , on the other hand , are likely to be associated with massive stars that at the end of their evolution ( a few myr ) are still within the cloud where they formed .
we note that bloom , kulkarni & djorgovski ( 2001 ) have identified the host galaxies of 20 afterglows of long duration grbs and have found grb  host offsets lower than those expected for merging ns binaries ( bloom , sigurdsson & pols 1999 ; bulik , belczyski & zbijewski 1999 ; fryer , woosley & hartmann 1999 ) .
furthermore , the high column densities identified by owens ( 1998 ) and galama & wijers ( 2001 ) from the absorption of the x - ray afterglow emission indicate that long - duration grbs occur in giant molecular clouds , yielding further support for the massive star collapse model for long bursts .
if the above arguments are correct , we expect the afterglows of short grbs to occur in a more tenuous medium compared to the afterglows of long - duration grbs .
the difference in the density of the medium is likely to be a few orders of magnitude .
given the kinetic energy @xmath21 of the relativistic outflow and the number density @xmath22 of the ambient external medium , plus a few other dimensionless parameters described below , the afterglow light - curves in various bands may be theoretically estimated ( e.g. , sari , piran & narayan 1998 ; panaitescu & kumar 2001a , and references therein ) . if we consider early times , when the radio emission is below the peak frequency @xmath23 of the afterglow spectrum , and if we assume that the cooling frequency @xmath24 is between the optical and x - ray bands , then the analysis of panaitescu & kumar ( 2001a ) shows that f_radio ^-2/3 ^1/3 e^5/6 n^1/2 , [ radio ] f_optical ^p-1 ^(p+1)/4 e^(p+3)/4 n^1/2 , [ optic ] f_x - ray ^p-1 ^(p-2)/4 e^(p+2)/4 .
[ xray ] here , @xmath21 is the isotropic equivalent kinetic energy of the outflow , @xmath25 is the fractional energy in electrons , @xmath26 is the index of the power - law distribution of the electron lorentz factor @xmath27 , and @xmath28 is the fraction of the post - shock thermal energy in magnetic field ( see panaitescu & kumar 2001a for details ) .
the break frequencies satisfy @xmath29 , @xmath30 for synchrotron - dominated electron cooling , and @xmath31^{1/(4-p)}$ ] when inverse compton losses exceed synchrotron cooling .
the above equations show that for @xmath32 , which is the average value for this parameter determined by panaitescu & kumar ( 2001b ) from numerical modeling of eight grb afterglows , the afterglow flux is roughly proportional to the kinetic energy @xmath21 .
since short grbs have a fluence on average @xmath2 times smaller than that of long grbs , other parameters being equal , we expect the afterglows of short grbs to be @xmath2 times dimmer than the afterglows of long grbs .
the equations show that the afterglow flux in short bursts would be further suppressed if these bursts occur in a lower density medium compared to long bursts .
the expressions for the radio and optical flux have an explicit dependence on @xmath22 .
even though the formula for the x - ray flux does not have an explicit dependence , this flux is also suppressed since , for low @xmath22 , the cooling frequency @xmath24 moves above the x - ray band and so the x - ray afterglow light - curve is described by equation ( [ optic ] ) rather than equation ( [ xray ] ) .    finally , if the breaks observed at one to a few days in the optical emission of several grb afterglows are due to collimation of the outflow ( rhoads 1999 ; sari et al .
1999 ; kumar & panaitescu 2000 ) , then the @xmath2 times smaller kinetic energy of the jets in short grbs will cause the jet break time @xmath33 to occur @xmath34 times earlier in these bursts compared to long grbs .
this will further diminish the brightness of short - grb afterglows ( at a fixed observing time ) by a factor of about @xmath35 .
these conclusions are illustrated in figure 2 , which compares the radio , optical , and x - ray emission of a typical long - grb afterglow with that predicted for short - grb afterglows with lower values of @xmath21 and @xmath22 .
the numerical calculations of the afterglow dynamics and emission of radiation were done by the methods described in panaitescu & kumar ( 2000 ) .
the parameters for the long - grb afterglow were chosen such that at one day after the burst the model yields a radio flux of @xmath36 mjy , an optical brightness of @xmath37 and a 210 kev x - ray flux of @xmath38 , in rough agreement with observations .
we see from fig .
2 that the radio emission from a typical short - grb afterglow will most likely be very difficult to detect . the same is true also for the optical emission , where only early ( @xmath39 day ) observations as deep as the measurements made by groot ( 1998 ) for grb 970828 and by fynbo ( 2001 ) for grb 000630 are likely to be successful . the best chance for detecting the afterglow of a short grb is with x - ray observations .
bepposax will need to observe earlier than @xmath40 day , and cxo , hete ii and swift earlier than @xmath41 days .
such observations are quite feasible .    because of the roughly linear dependence of the afterglow brightness on the kinetic energy @xmath21 , any difference in the average redshifts of short and long grbs will not alter the above conclusions .
the redshift enters into the estimate of @xmath21 , and through it in the estimate of the afterglow luminosity , but it factors out when the luminosity is converted to the observed flux .
the fluences above 25 kev of grbs detected by batse are positively correlated with the durations of these bursts ; long bursts ( durations longer than a few seconds ) are on average 20 times more energetic than short bursts .
moreover , the @xmath42 three dozen long grbs for which afterglows have been detected so far ( following their accurate localization by bepposax and the interplanetary network ) are on average 40 times brighter ( in fluence ) than typical short grbs .
thus we expect the relativistic outflow of a long grb to have about 20 times the kinetic energy of the outflow from a short grb .
if the other parameters that influence the dynamics of the grb remnant and the emission of radiation are roughly the same , we predict that the afterglows of short grbs should be a factor of 10 or more dimmer than the afterglows of long grbs .    if short grbs arise from merging ns  ns or ns  bh binaries which may have traveled upto or beyond the very tenuous outskirts of their host galaxies , and if long grbs are due to the core collapse of massive stars which die in the dense molecular clouds where they were formed , then the densities @xmath22 of the media surrounding these two types of grbs may differ by a few orders of magnitude .
this could further seriously diminish the prospects of detecting radio and optical afterglows of short grbs since the afterglow brightness in these bands is proportional to @xmath43 .
we conclude that the best chance of detecting afterglows of short grbs is with early x - ray observations within 1 day after the grb .
rapid and deep optical follow - up within a few hours after the main event may also lead to a detection .
radio observations appear the least promising ( fig .
2 ) .    of course
, short grbs significantly brighter than average could be as energetic as some of the long grbs for which afterglows have been seen ( fig .
the afterglows of such unusually bright short grbs could be detected even beyond a day , particularly if the magnetic field strength is close to equipartition ( @xmath44 ) .
but such bursts should be in the minority .
on the other hand , if future observations indicate that the afterglows of most short grbs are as bright as those of long grbs , it would imply that one or more of the assumptions we have made in our analysis is invalid .
one possibility is that the @xmath0-efficiency is significantly lower in short bursts than in long bursts , as disussed in kumar ( 1999 ) , and another is that the efficiency spans a wide range in both types of bursts , indicating a highly inhomogeneous outflow ( kumar & piran 2000 ) .
eichler , d. 1989 , nature , 340 , 126 fryer , c. , woosley , s. , herant , m & davies , m. 1999 , apj , 520 , 650 fynbo , j. 2001 , a&a 369 , 373 goodman , j. 1986 , apj , 308 , l17 groot , p. 1998 , apj , 493 , l27 hurley , k. 2001 , apj , submitted ( astro - ph/0107188 ) katz , j. 1994 , apj , 422 , 248 katz , j. & canel , l. 1996 , apj , 471 , 915 kouveliotou , c. 1993 , apj , 413 , l101 kumar , p. 1999
, apj , 523 , l113 kumar , p. & piran , t. 2000 , apj , 535 , 152 kumar , p. & panaitescu , a. 2000 , apj , 541 , l9 lazzati , d. , covino , s. & ghisellini , g. 2001 , a&a , submitted ( astro - ph/0011443 ) lee , t. & petrosian , v. 1997 , apj , 474 , 37 macfadyen , a. & woosley , s. 1999 , apj , 524 , 262 macfadyen , a. , woosley , s. & heger , a. 2001 , apj , 550 , 410 mao , s. , narayan , r. , and piran , t. , 1994 , apj , 420 , 171 meegan , c. 1996 , apj , s106 mszros , p. & rees , m. 1992 , apj , 397 , 570 mszros , p. , rees , m.j . & wijers , r. 1999 , new ast , 4 , 303 mukherjee , s. 1998 , apj , 508 , 314 narayan , r. , paczyski , b. & piran , t. 1992 , apj , 395 , l83 narayan , r. , piran , t. & kumar , p. 2001 , apj , in press ( astro - ph/0103360 ) paczyski , b. 1991 , acta ast , 41 , 257 paczyski , b. 1998 , apj , 494 , l45 panaitescu , a. & kumar , p. 2000 , apj , 543 , 66 panaitescu , a. & kumar , p. 2001a
, apj , 554 , 667 panaitescu , a. & kumar , p. 2001b
, apj , submitted piran , t. 1996 , in `` compact stars in binaries '' , proceedings from iau symposium 165 , eds j. van paradijs , e. p. j. van den heuvel , e. kuulkers .
kluwer academic publishers , dordrecht , p.489 piran , t. 1999 , phys . rep .
, 314 , 575 piran , t. , shemi , a. & narayan , r. 1993 , mnras , 263 , 861 ramirez - ruiz , e. & fenimore , e. 2000 , apj , 539 , 712 rees , m.j . & mszros , p. 1992 , mnras , 258 , 41p rhoads , j. 1999 , apj , 525 , 737 sari , r. , piran , t. 1997 , apj , 485 , 270 sari , r. , piran , t. , & halpern , j. 1999 , apj , 519 , l17 sari , r. , piran , t. , & narayan , r. 1998 , apj , 497 , l17 tavani , m. 1998 , apj , 497 , l21 woosley , s. 1993 , apj , 405 , 273 zhang , w. & fryer , c. 2001 , apj , 550 , 357

 if the efficiency for producing @xmath0-rays is the same in short duration ( @xmath1 s ) gamma - ray bursts ( grbs ) as in long duration grbs , then the average kinetic energy of short grbs must be @xmath2 times less than that of long grbs .
 assuming further that the relativistic shocks in short and long duration grbs have similar parameters , we show that the afterglows of short grbs will be on average 1040 times dimmer than those of long grbs .
 we find that the afterglow of a typical short grb will be below the detection limit ( @xmath3 ) of searches at radio frequencies
 . the afterglow would be difficult to observe also in the optical , where we predict @xmath4 a few hours after the burst
 . the radio and optical afterglow would be even fainter if short grbs occur in a low - density medium , as expected in ns  ns and ns  bh merger models .
 the best prospects for detecting short - grb afterglows are with early ( @xmath5 day ) observations in x - rays .    3