Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies
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介绍黑洞的引言英文作文Introduction to Black Holes。
Black holes, one of the most fascinating objects in the universe, have been a subject of scientific research for decades. These mysterious objects are formed when a massive star collapses under its own gravity, creating a region in space where the gravitational pull is so strong that nothing, not even light, can escape. The concept of black holes was first proposed by the physicist John Michell in 1783 and was later refined by Albert Einstein's theory of general relativity in 1915.Black holes are invisible to the naked eye, as they do not emit any light or radiation. However, their presence can be detected by observing the effects of their immense gravitational pull on nearby stars and gas. The area surrounding a black hole is known as the event horizon, which marks the point of no return. Anything that crosses the event horizon is pulled into the black hole and is lostOne of the most intriguing aspects of black holes is their ability to distort time and space. The intensegravity near a black hole causes time to slow down, and space to be warped and stretched. This phenomenon, known as gravitational time dilation, has been confirmed by observations of stars orbiting black holes.Black holes come in different sizes, ranging from a few times the mass of the sun to billions of times the mass of the sun. Supermassive black holes, found at the centers of galaxies, are thought to play a crucial role in the evolution of galaxies, as they can influence the motion of stars and gas.Despite their mysterious nature, black holes have become a topic of intense research in astrophysics and cosmology. Scientists are using a variety of techniques, such as gravitational wave detection and observations of the effects of black holes on nearby objects, to study these enigmatic objects and unlock the secrets of theIn conclusion, black holes are one of the most intriguing and mysterious objects in the universe. They are formed by the collapse of massive stars and have a gravitational pull so strong that nothing can escape. Their ability to distort time and space and influence the motion of nearby objects makes them a subject of intense research in astrophysics and cosmology.。
外研版八年级太空旅行英语作文范文My Dream of Space TravelEver since I was a little kid, I've dreamed of traveling to space. The mysteries of the cosmos have fascinated me for as long as I can remember. I've spent countless hours staring up at the night sky, trying to comprehend the vast distances between stars and planets. The idea of leaving Earth's atmosphere and venturing into the great unknown fills me with a sense of excitement and wonder.I can vividly picture the moment when I would strap into the spacecraft, my heart pounding with anticipation. The roar of the rockets would be deafening as they ignited, pushing the craft upwards with incredible force. Within minutes, I would be breaking through the clouds, gazing down at our beautiful blue planet shrinking rapidly beneath me.As the Earth receded into the distance, the blackness of space would envelop me. I imagine it would be an overwhelming sensation - the silence, the cold vacuum, the brilliant stars shining undimmed by atmospheric distortion. Floating weightless, I would turn and see the sun, its brilliant raysstretching out in all directions unfiltered. What an amazing sight that would be.My first stop would be the International Space Station, where I could visit with the astronauts living and working there. I would beg them to let me go outside on a spacewalk. Can you imagine the thrill of leaving the safety of the station, tethered only by a lifeline, and propelling yourself out into the airless void? Looking down at our entire world hanging below you, a tiny oasis of life in the vastness of space - it would be a humbling and profound experience.After visiting the space station, I dream of traveling deeper into our solar system to explore some of the other planets and moons. The rusty, crater-covered surface of Mars has always captivated me. I would give anything to be one of the first humans to walk on that alien world. With its reddish sky and rusty soil, it would be like walking on an entirely different planet.Imagine standing on one of the rocky plateaus of Mars and watching the sun rise, the light filtering through the thin atmosphere in an otherworldly way. Or better yet, visiting one of Mars' two tiny moons - Phobos or Deimos. You could simply jump off the surface and float for a while due to the low gravitational pull. That's a childhood fantasy come true!After Mars, I would set a course for the gas giants - Jupiter, Saturn, Uranus, and Neptune. These massive worlds, each with their own unique weather patterns and haunting beautfy, would be sights to behold up close. Saturn's rings, those iconic bright loops of dust and ice, would take my breath away as I approached them in my spacecraft.Jupiter's Great Red Spot, a colossal storm larger than the entire Earth, is something I've been curious about since learning about it in school. To see that raging vortex up close would be mind-blowing. And the ice giants Uranus and Neptune, their aquamarine atmospheres swirling with wind and storms, would humble me with their seeming serenity from a distance.Visiting the myriad of moons orbiting these outer planets would be a bonus adventure. Some like Enceladus, with its subsurface ocean, or Europa with its icy surface cracked like a puzzle, could potentially harbor life. How incredible would it be to be among the first explorers to find definitive proof of alien life in our solar system?Of course, no fantasy space journey would be complete without a stop at the dwarf planet Pluto. Ever since that little world was famously demoted from full planet status, I've felt a bit sorry for it. It would be wonderful to visit frigid, distant Plutoand maybe restore a little of its dignity by being among the few humans to ever see it up close.After visiting the planets, I would set my sights on destinations even farther out - deep into the galaxy and possibly beyond. Zooming past asteroids and comets, I would get a firsthand look at these ancient travellers of the solar system. Some are solid chunks of rock and metal, while others are little more than loosely bound piles of dust, gravel, and ice.Imagine coming upon one of the giant molecular clouds that fill the spaces between stars - those vast, chilly nebulas made of dust and gas, the birthplaces of new stars and planets. It would be breathtaking to see those brilliant smears of color swirling in the eyepiece, like glowing cosmic fingerpaint.Of course, it wouldn't be a proper space odyssey without visiting other star systems. Traveling at mind-boggling speeds, I could flit between the brilliant stellar cores of distant suns, each one an entire world with its own unique set of orbiting planets. Some might be burning blue giants, others cool, bloated red dwarfs, but each one a true marvel of creation.With faster-than-light travel being theoretically possible, who knows how far my journey could take me? Out of the Milky Way and into other galaxies strewn across the universe likediamond dust. I could soar between the spiral arms, taking in galaxy clusters packed with billions of stars and dark matter. Or dive into the supermassive black holes at the center of quasars and galaxies, peering into their mysterious, light-devouring maws.There's an entire universe out there waiting to be explored. And while space travel for us Earthlings is still somewhat limited for now, I have no doubt that we'll continue pushing outward, driven by our innate curiosity and desire for adventure. Perhaps within my lifetime, these childhood reveries of mine will become more of a reality.Every kid dreams of blasting off and traveling among the stars. I know I'm not alone in my fascination with the cosmos and my longing to experience its wonders firsthand. While being an astronaut takes incredible skill and dedication, a piece of me hopes that I might one day have the privilege of joining their ranks. Because the further we go, the more we'll learn about our universe and our place within it.Until that day comes, I'll have to be content gazing up at the heavens and imagining all the marvels awaiting me among the stars. The planets, moons, asteroids, nebulae, quasars, black holes, alien worlds - an entire unexplored frontier of endlesspossibilities just waiting to be discovered. To me, that boundless promise of adventure and mystery makes space travel the most captivating dream imaginable. And I'll keep reaching for the stars.。
航天解说员小练笔作文英文回答:As a space commentator, I have the privilege of witnessing and explaining the wonders of space explorationto the public. It is truly an exciting and awe-inspiring field that never fails to capture the imagination. From the moment a rocket launches into the sky to the discovery of new planets and galaxies, there is always something fascinating happening in the world of space.For instance, one of the most remarkable achievementsin recent years is the successful landing of the Mars rover. This groundbreaking mission allowed scientists to gather valuable data about the Red Planet and search for signs of life. The rover's ability to navigate the harsh Martian terrain and send back high-resolution images has providedus with a glimpse into the mysteries of our neighboring planet.中文回答:作为一名航天解说员,我有幸目睹并向公众解释太空探索的奇迹。
黑洞的由来的英语作文The Origin of Black Holes: A Journey into Cosmic Mysteries。
Introduction。
Black holes, enigmatic entities lurking in the depthsof space, have captivated the imagination of scientists and laypersons alike. Their origins, shrouded in cosmic mystery, have been the subject of intense study and speculation. In this essay, we embark on a journey to unravel the secretsof black holes, exploring their formation, properties, and significance in the universe.Formation of Black Holes。
The genesis of black holes begins with the demise of massive stars. When a massive star exhausts its nuclear fuel, it undergoes a cataclysmic event known as a supernova explosion. During this explosive phase, the outer layers ofthe star are ejected into space, while its core undergoes gravitational collapse. If the core's mass exceeds acritical threshold, it collapses into a singularity—a point of infinite density—giving birth to a black hole.The process of black hole formation can also occur through the gravitational collapse of dense stellar remnants, such as neutron stars, or through the merger of two compact objects, such as neutron stars or black holes. These pathways lead to the creation of different types of black holes, ranging from stellar-mass black holes to supermassive black holes found at the centers of galaxies.Properties of Black Holes。
黑洞介绍英语作文初一Title: Exploring the Mysteries of Black Holes。
Black holes are fascinating objects in the universethat have captured the imagination of scientists and the public alike. These enigmatic entities are characterized by their immense gravitational pull, which is so strong that nothing, not even light, can escape from them. In this essay, we will delve into the intriguing world of black holes and explore their properties, formation, and significance in astrophysics.To begin with, let's discuss the nature of black holes.A black hole is formed when a massive star collapses under its own gravity at the end of its life cycle. As the star's core runs out of nuclear fuel, it can no longer support its own weight, leading to a catastrophic collapse. This collapse causes the star to shrink to a point of infinite density called a singularity, surrounded by an event horizon, which marks the boundary beyond which nothing canescape.The concept of the event horizon is crucial to understanding the behavior of black holes. It represents the point of no return, beyond which the gravitational pull is so strong that even light cannot break free. This phenomenon makes black holes invisible to direct observation, as they do not emit any light themselves. Instead, scientists infer their presence through theeffects they have on surrounding matter and light.Despite their invisibility, black holes can have a profound impact on their surroundings. For example, when matter gets too close to a black hole, it is drawn into a swirling disk of gas and dust called an accretion disk. The intense friction and gravitational forces within the accretion disk cause it to heat up and emit high-energy radiation, such as X-rays, which can be detected by telescopes.Another fascinating aspect of black holes is their role in the evolution of galaxies. Supermassive black holes,which can contain the mass of millions or even billions of suns, are thought to reside at the centers of most galaxies, including our own Milky Way. These behemoths exert a powerful influence on their host galaxies, regulating the formation of stars and influencing the dynamics of galactic structures.In recent years, scientists have made significantstrides in our understanding of black holes, thanks to advances in observational techniques and theoretical modeling. For example, the Event Horizon Telescope collaboration made headlines in 2019 with the first-ever image of a black hole's silhouette, providing direct evidence of their existence.Moreover, theoretical frameworks such as Einstein's theory of general relativity have provided a mathematical description of black holes' behavior, allowing scientiststo make predictions and test them against observational data. However, many mysteries surrounding black holes remain, such as the nature of the singularity at their core and the possibility of wormholes connecting distant regionsof space-time.In conclusion, black holes are among the mostintriguing phenomena in the universe, challenging our understanding of physics and the nature of reality itself. While much progress has been made in unraveling their mysteries, there is still much we have yet to learn about these enigmatic objects. Continued research and exploration are essential if we are to unlock the secrets of black holes and expand our knowledge of the cosmos.。
重庆市第八中学校2024届高三下学期高考适应性月考(五)英语试卷学校:___________姓名:___________班级:___________考号:___________一、阅读理解DAY TRIP ITINERARY (行程)After a warm reception from your tour manager at your dedicated pick-up point in London, settle in your comfortable coach as we set off on our journey towards Stonehenge. The world's most famous prehistoric monument has inspired people to study and interpret it for centuries, yet many questions remain to be answered-about who built it, when, and why.After visiting Stonehenge, we drive to Windsor Castle, which is home to royalty and 1,000 years of royal history. The stunning 13-acre site is the largest and oldest occupied, working castle in the world. There are many famous, must-see moments within these spectacular rooms in the castle, like the grand Waterloo Chamber and the magnificent Crimson Drawing Room.In the early evening, we make our way towards London and proceed towards your respective drop off points and bid farewell to all friends you have made on the tour. ESSENTIALS TO CARRY WITH YOUWe recommend you wear comfortable clothing and carry essentials such as a jacket or jumper, dry snacks, water, tissues, chargers, power bank, ete., in your handbag as access to the luggage hold is only possible until a comfort stop or arrival at your destination. Hot foods are not allowed to be carried or consumed inside the coach.PICK-UP POINTSand travelling.1.How many tourist spots will the participants visit?A.Two.B.Three.C.Four.D.Five.2.It is advised to put your essentials in the handbag because _______.A.the luggage hold is inaccessible when the bus is in motionB.they are not allowed to be carried inside the coachC.it's convenient for you to enjoy hot foodsD.drivers are likely to access them3.Where is the text most probably taken from?A.A journal.B.A webpage.C.A travel brochure.D.A magazine.It all started with a simple question:"Can I paint your portrait? "One day in the summer of 2015, Peterson was relaxing in his living room, reading the book Love Does, about the power of love in action, when his quiet was disturbed by a homeless man outside his apartment. Inspired by the book's compassionate message, Peterson made a decision:He was going to go outside and introduce himself.In that first conversation, Peterson learned that the man's name was Matt Faris. He'd moved to Southern California from Kentucky to pursue a career in music, but he soon fell on hard times and ended up living on the street for more than a decade. "I saw beauty on the face of a man who hadn't shaved in probably a year, because his story, the life inside of him, inspired me," Peterson recalled. Therefore, Peterson asked if he could paint Faris's portrait. Faris agreed.Peterson's connection with Faris led him to form Faces of Santa Ana, a nonprofit organization focused on befriending and painting portraits of members of the community who are unhoused. Peterson sells the paintings for money, splitting the proceeds and putting half into a "love account" for his model. He then helps people use the money to get back on their feet.Many of Peterson's new friends use the donations to secure immediate necessities medical care, hotel rooms, food. Faris used the funds from his portrait to record an album, fulfilling his musical dreams. Another subject, Kimberly Sondoval, had never been able to financially support her daughter. She asked, "Can I use the money to pay my daughter's rent? " When the check was delivered, "They both wept in my arms, "Peterson recalls.Peterson has painted 41 of these portraits himself. But there's more to the finished products than the money they bring to someone who's down and out. He's discovered that the buyers tend to connect to the story of the person in the painting, finding similarities and often friendship with someone they might have otherwise overlooked or stereotyped."People often tell me, 'I was the one that would cross the street, but I see homeless people differently now, ' " Peterson says. "I didn't know that would happen."4.What made Peterson start a conversation?A.The curiosity about strangers.B.The touching story of Matt Faris.C.The disturbance by a homeless man.D.The sympathetic message in Love Does.5.What do we know about Faces of Santa Ana?A.It pays the homeless salaries.B.It is an official nonprofit organization.C.It tries to restore the lives of Peterson's models.D.It spends all the money on helping the unhoused.6.After buying a portrait, a buyer might view the homeless as ______?zy and poorB.odd but inspiringC.disturbing and untidyD.pitiful but respectable7.Which of the following is the best title of this text?A.Art with Purpose: Love Account MattersB.Hope in Paintings: Help Knows No RaceC.Faces of Compassion: Painting a New PerspectiveD.Encounter with Strangers: Embracing New FriendsFilm Puts Justifiable Defense in SpotlightThe film, Article 20, directed by Zhang Yimou, draws its name from Article 20 of the Criminal Law, which focuses on the sometimes controversial legal concept of justifiable defense. Drawing inspiration from real-life cases of justifiable defense, the film gained widespread attention and struck a chord with the public during the Spring Festival holiday. The movie calls for a detailed interpretation of legal terms and urges against compromising on unlawful conduct.According to the Criminal Law, when a person, faced with an unlawful attack, takes action to protect his or her own rights or interests or those of others, and the attacker is thereby harmed, the defender will be considered to have acted in justifiable defense and will not bear criminal responsibility. For some time, justifiable defense has been regarded as a "dormant clause" (沉寂条款) , due to the influence of misconceptions, such as "whoever is injured or killed is right".But the true meaning of the law should be to increase the responsibility for wrongdoers, rather than burdening good people. Recent cases have shown that, for ordinary citizens, justifiable defense is no longer a pipe dream. A high-profile case in Kunshan, Jiangsu province, in 2018 served as a wake-up call and caught the attention of authorities regarding such cases. In that case, a traffic argument led to a motorist who took a knife with him confronting another man.The motorist was killed, and police and judges determined that the defender's actions constituted justifiable defense. Since then, the justifiable defense clause has been applied in several places across the nation. The concern over justifiable defense reflects the public's demand for fairness, justice, security and rule of law.Luo Xiang, a renowned professor of criminal law at China University of Political Science and Law, said in a recent comment about the film Article20 that the public and judges should avoid taking a "godlike" perspective. Instead, they should consider the situation in which the defender was involved, empathize with the defender's position, and stop themselves from making excessive demands on the defender, Luo said.8.Why did the film Article 20 attract the audience's attention?A.It was released during the Spring Festival holiday.B.It is named after one article in the Criminal Law.C.It explores real-life cases of justifiable defense.D.It was directed by Zhang Yimou.9.According to the Criminal Law, the victim will be free from criminal responsibility when ______.A.the victim gave up his legal rightsB.the robber kept silent about the robberyC.the robber was hurt worse than the victimD.the victim knifed the armed robber to stop the ongoing crime10.What is the function of the case in Kunshan in Paragraph 3?A.Making comparisons.B.Listing reasons.C.Explaining misconceptions.D.Providing evidence.11.What does Luo Xiang suggest judges do?A.Take a “godlike” viewpoint with the public.B.Put oneself in the defender's shoes.C.Demand more from the defender.D.Side with the attacker.Researchers have discovered the oldest black hole ever observed, dating from the dawn of the universe, and found that it is "eating" its host galaxy to death.The international team, led by the University of Cambridge, used the James Webb Space Telescope (JWST) to detect the black hole, which dates from 400 million years after the big bang. The results, which lead author Professor Roberto Maiolino says are "a giant leap forward", are reported in the journal Nature.This surprisingly massive black hole even exists so early in the universe challenges our assumptions about how black holes form and grow. The size of this newly-discovered black hole suggests that they might form in other ways: they might be 'born big' or they can eat matter at a rate that's five times higher than had been thought possible. Like all black holes,According to standard models, supermassive black holes form from the remains of dead stars, which collapse and may form a black hole about a hundred times the mass of the Sun. If it grew in an expected way, this newly-detected black hole would take about a billion years to grow to its observed size. However, the universe was not yet a billion years old when this black hole was detected.The young host galaxy, called GN-z11, is a compact galaxy, about one hundred times smaller than the Milky Way, but the black hole is likely harming its development. When black holes consume too much gas, it pushes the gas away like an ultra-fast wind. This "wind" could stop the process of star formation, slowly killing the galaxy, but it will also kill the black hole itself, as it would cut off the black hole's source of "food".Maiolino says that the gigantic leap forward provided by JWST makes this the most exciting time in his career. "It's a new era: the giant leap is like upgrading from Galileo's telescope to a modern telescope overnight," he said. "The universe has been quite generous in what it's showing us, and this is just the beginning."12.What does the underlined word "devours" mean in Paragraph 3?A.Changes.B.Swallows.C.Observes.D.Forms.13.According to Paragraph 5, why is GN-z11 likely to be harmed?A.Because the host galaxy is too small.B.Because the black hole is killing itself.C.Because the “wind” ceases star formation.D.Because black holes produce too much gas.14.What is Maiolino's attitude to the new discovery about the black hole?A.Favorable.B.Intolerant.C.Doubtful.D.Ambiguous.15.What can we learn from this passage?A.The black hole took a billion years to achieve its size.B.Supermassive black holes are assumed to form overnight.C.The new discovery of the host galaxy is a giant leap forward.D.The host galaxy and the black hole can be destroyed by the "wind".二、七选五16.The Failed New Year's Resolution: Three Tips to Get on Track January is officially over, and many people are taking stock of their progress towards New Year's resolutions. The fact is that you probably haven't kept up with them as much as you hoped. But that's not your fault. ①______.If you feel like you have already failed, here are three tips before you let go.Practice self-compassionMany people talk to themselves in harsh ways when struggling with new habits, believing self-criticism will help them reach their goals. Research shows, however, that the opposite is true. Self-compassion is more effective for personal improvement, especially when facing failure. ②______, try to be kind and gentle with yourself, just as you would with a loved one.③______Resolutions are often phrased as definitive goals. I will exercise daily. I will kick desserts. ④______. But setting all-or-nothing goals can lead to all-or-nothing decisions that one gives up when faced with challenges. In contrast, intentions focus more on your values than specific actions. For example, the resolution "I will exercise daily" may become an intention of "I want to move my body because it feels good." This approach allows for more flexibility when unexpected stress arises.Solve problems by overcoming barriersIf you are struggling to maintain your desired habits, there are evidence-based techniques available to help you. ⑤______. This involves identifying the specific barriers that lead to your quitting something that you want to do. Perhaps you keep forgetting the new habit, or perhaps you don't understand how to do it. Whatever it is, identify the barrier and cope with it specifically.A. Set all-or-nothing goalsB. Change your resolutions into intentionsC. One such skill is called missing links analysisD. Setting specific behavioral goals can be effectiveE. If you're persuaded to give up on your resolutionsF. Old habits tend to die hard, and new habits tend to die easyG. When you are upset about yourself for not keeping resolutions三、完形填空(15空)My son asked me months ago if he could switch from his mainstream high school to aanother learning environment to complete his study. But my heart hurt a little that he wouldThen, we decided the vocational school (职业学校) was an option with the same generalcarry over, and he could graduate early.17.pulsory B.technical C.unprofessional D.academic18.A.heartbroken B.nervous C.angry D.confused19.A.apply B.adapt C.transfer D.talk20.A.ceremony B.moment C.dilemma D.stage21.A.curriculum B.wellbeing C.friendship D.decision22.A.bald B.generous C.straightforward D.shy23.A.anxiety B.conduct C.responsibility D.awareness24.A.studied B.canceled C.required D.banned25.A.credits B.subjects C.medals D.reputations26.A.graduate B.worsen C.thrive D.suffer27.A.formed B.understood C.abandoned D.remembered28.A.got away B.made up C.lined up D.got along29.A.crying B.murmuring plaining D.smiling30.A.oversell B.learn C.share D.predict31.A.affordable B.suitable C.available D.sensible四、短文填空32.While there is growing consumer ①______ (realize) of the environmental impact of fast fashion, can the same be said about fast furniture? The chairs and tables that fill many of our homes and everyday spaces are manufactured on a mass scale, and the cheaper items often end up ②______ landfills.According to the Environmental Protection Agency (EPA) , in 2020 over 12 million tons of furniture ③______ (throw) out in America and some into the forest illegally. Buying furniture can be ④______ (incredible) expensive. Many of us switch over to cheaper, instant brands like IKEA, ⑤______ manufacturers use materials harder to recycle, which is likely to damage the environment.With growing calls for sustainability, many brands are announcing to change though it remains ⑥______ (see) whether they will keep these promises. In ⑦______ (it) current sustainability strategy, IKEA commits itself to using only recyclable materials in all its products in an effort to practice "circular" design and cut emissions to net-zero. The concept of circular design ⑧______ (win) increasing concern up to now. In ⑨______ circular system, furniture products would be designed to last longer and be fully recyclable, thus forming a ⑩______ (close) loop (环) .五、书面表达33.假定你是高三学生李华。
2024年04版小学4年级英语第三单元真题(含答案)考试时间:100分钟(总分:140)B卷考试人:_________题号一二三四五总分得分一、综合题(共计100题)1、听力题:The chemical symbol for cobalt is _____.2、听力题:We will _______ (have) a picnic today.3、填空题:I have a robot _______ that can dance and sing.4、填空题:There are many ________ (树木) in the forest.5、填空题:The _______ (青蛙) can live both in water and on land.6、What color do you get when you mix blue and yellow?A. PurpleB. GreenC. OrangeD. Brown7、What is the name of the famous ancient city in Italy known for its ruins?A. RomeB. PompeiiC. FlorenceD. Venice答案:B8、填空题:The ________ was a famous leader in the fight for justice.9、 (11) is home to many unique species. 填空题:The ____10、填空题:The ________ (养分) in the soil is important for growth.11、填空题:A ______ (蜗牛) carries its home with it wherever it goes.12、听力题:The capital city of Australia is __________.13、选择题:Which instrument has strings?A. PianoB. DrumC. ViolinD. Flute14、听力题:My dad drives a ______ (car).15、填空题:A ________ (植物遗传多样性保护) ensures survival.16、听力题:A stable isotope has the same number of ______.17、听力题:Many galaxies have supermassive black holes at their _______.18、听力题:The chemical formula for sodium thiosulfate is __________.19、听力题:The chemical formula for bismuth(III) oxide is __________.20、填空题:The ancient Romans are known for their ________ and culture.21、What is the opposite of 'fast'?A. SlowB. QuickC. SpeedyD. Rapid答案:A22、听力题:A chemical that aids in digestion is called a ______.23、听力题:A _______ is a measure of how much matter is in an object.24、Which instrument has keys and is played with fingers?A. GuitarB. DrumsC. PianoD. Violin答案:C25、填空题:The __________ is a large lake located in North America. (五大湖)26、听力题:The dog is _____ (barking/sleeping) in the yard.27、听力题:A __________ reaction releases energy in the form of heat.28、听力题:The cat is ______ with a string. (playing)29、听力题:The chocolate is ___ (sweet/sour).30、What is the capital of Spain?A. BarcelonaB. MadridC. SevilleD. Valencia答案:B31、soil) is crucial for agriculture. 填空题:The ____32、填空题:Dolphins are very _______ (聪明的).33、填空题:My friend is very __________ (独特的) in her style.34、What do we call the study of heredity and variation?A. GeneticsB. EvolutionC. BiologyD. Ecology35、填空题:My favorite animal at the zoo is a _______ (大象).36、选择题:What do we call the time of day when the sun sets?A. SunriseB. NoonC. SunsetD. Midnight37、填空题:Gardening can provide a sense of accomplishment and ______. (园艺可以带来成就感和快乐。
黑洞介绍英语作文带翻译Title: Exploring the Enigma of Black Holes。
Introduction。
Black holes have long captured the imagination of scientists and the public alike. These enigmatic cosmic entities, formed from the collapse of massive stars, possess gravitational forces so intense that not even light can escape their grasp. In this essay, we will delve into the fascinating world of black holes, exploring their properties, formation, and the profound implications they hold for our understanding of the universe.Properties of Black Holes。
At the heart of every black hole lies a singularity, a point of infinite density where the laws of physics, as we currently understand them, break down. Surrounding this singularity is the event horizon, the boundary beyond whichnothing can escape the black hole's gravitational pull. It is this event horizon that gives black holes their name, as it appears "black" to outside observers.Formation of Black Holes。
介绍宇宙的英语作文100字初中全文共6篇示例,供读者参考篇1The Vast Expanse of the UniverseEver since I was a little kid, I've been fascinated by the night sky. Gazing up at the twinkling stars, I often found myself lost in thought, pondering the mysteries that lie beyond our tiny blue planet. The universe is a vast expanse, a boundless sea of galaxies, stars, and celestial wonders that have captivated humankind for centuries.In school, we learned about the basic structure of the universe. At the center of our solar system is the Sun, a massive ball of hot plasma that provides us with light and warmth. Orbiting around the Sun are the planets, each with its unique characteristics and moons. Our planet, Earth, is a beautiful blue and green oasis, teeming with life and surrounded by a thin veil of atmosphere.But the universe extends far beyond our solar system. It is estimated that there are billions of galaxies in the observable universe, each containing millions or billions of stars. Our galaxy,the Milky Way, is a vast spiral of stars, gas, and dust, with a supermassive black hole at its center. It's mind-boggling to think that our Sun is just one of countless stars in this cosmic ocean.As I delve deeper into the study of the universe, I'm constantly amazed by the sheer scale and complexity of it all. Galaxies are not randomly scattered throughout space; they are organized into clusters and superclusters, forming an intricate cosmic web that stretches across billions of light-years. And between these luminous islands of stars lie vast stretches of darkness, punctuated by clouds of gas and dust that serve as the nurseries for new stars and planets.One of the most captivating aspects of the universe is its origins. According to the Big Bang theory, the universe began as an incredibly hot and dense singularity, which expanded rapidly in a colossal explosion around 13.8 billion years ago. This cosmic event scattered the fundamental particles of matter across the nascent universe, setting the stage for the formation of the first stars and galaxies.As the universe cooled and evolved, it gave rise to an astonishing array of celestial phenomena. Black holes, those insatiable gravitational monsters, warp the very fabric of space and time, devouring anything that strays too close. Pulsars, thedense remnants of exploded stars, spin rapidly and emit beams of radiation like cosmic lighthouses. And quasars, powered by supermassive black holes at the hearts of distant galaxies, shine with the brilliance of billions of suns.But perhaps the most profound question of all is whether we are alone in this vast cosmic expanse. The sheer enormity of the universe and the countless stars and planets it harbors have led many scientists to speculate that life may exist elsewhere. The search for extraterrestrial intelligence, or SETI, has become a major focus of modern astronomy, with powerful telescopes and radio receivers scanning the skies for any signs of intelligent life beyond our planet.As I continue to learn about the universe, I'm constantly reminded of how small and insignificant we are in the grand scheme of things. Yet, at the same time, I'm filled with a sense of wonder and awe at the grandeur and beauty of the cosmos. The universe is a place of infinite mysteries, and every new discovery only seems to unravel more questions.Perhaps one day, humanity will unlock the secrets of the universe, unraveling the mysteries of dark matter, black holes, and the very nature of space and time itself. Or perhaps the universe will forever remain a vast, unknowable expanse, itsdeepest secrets forever beyond our grasp. Either way, the journey of exploration and discovery is one that fills me with excitement and curiosity.As I gaze up at the night sky, I'm reminded of the words of the great cosmologist Carl Sagan: "We are a way for the universe to know itself." And in that profound statement, I find solace and inspiration, for it reminds me that we are not mere spectators in this cosmic drama, but active participants in the unfolding of the universe's grand story.篇2The Vast Wonder of the UniverseThe universe is a mind-bogglingly vast expanse that has captivated humans for millennia. As I gaze up at the twinkling stars on a clear night, I can't help but feel a sense of awe and wonder. The cosmos is home to countless celestial bodies, from sizzling stars to ghostly nebulae to gargantuan galaxies. And at the heart of it all lies one of the greatest mysteries in existence –the origins of the universe itself.According to the widely accepted Big Bang theory, the universe began as an infinitely hot and dense singularity around 13.8 billion years ago. In the first few fractions of a second afterthe Big Bang, the universe underwent a period of rapid expansion and cooling, forming the fundamental particles that would eventually coalesce into the stars, galaxies, and other celestial wonders we observe today.One of the most remarkable features of the cosmos is the sheer scale involved. Our own Milky Way galaxy, for example, is a vast spiral of stars, gas, and dust measuring around 100,000 light-years in diameter. Yet the Milky Way is just one of billions of galaxies scattered throughout the observable universe, which spans an incredible 93 billion light-years in diameter. It's a staggering distance that's almost impossible for the human mind to fully comprehend.Within this colossal expanse, we find a diverse array of celestial objects, each with its own unique characteristics and mysteries. Stars, the building blocks of galaxies, come in a wide range of sizes, colors, and temperatures, from the cool, dim red dwarfs to the scorching blue giants. Some stars even exhibit bizarre behavior, such as pulsars, which emit beams of radiation at regular intervals, or quasars, which are incredibly bright and energetic objects powered by supermassive black holes.Speaking of black holes, these enigmatic regions ofspace-time are among the most fascinating and perplexingobjects in the universe. With gravitational fields so intense that not even light can escape their grasp, black holes represent the ultimate paradox – regions of space where the laws of physics as we know them break down. Yet they play a crucial role in the evolution of galaxies and the distribution of matter throughout the cosmos.Beyond the boundaries of our own galaxy, the universe is home to a dazzling array of celestial phenomena. Nebulae, vast clouds of gas and dust, serve as the birthplaces of new stars and planets. Supernovae, the explosive deaths of massive stars, briefly outshine entire galaxies and seed the cosmos with heavy elements essential for life. And dark matter, an invisible and mysterious substance that makes up around 27% of the universe, exerts a gravitational influence on the largest structures in the cosmos, shaping the very fabric of the universe itself.As our understanding of the universe continues to grow, new and exciting frontiers of exploration emerge. The search for exoplanets, worlds orbiting distant stars, has yielded thousands of candidates, some of which may even harbor conditions suitable for life. The study of gravitational waves, ripples in the fabric of space-time predicted by Einstein's theory of generalrelativity, promises to unlock new insights into the most extreme events in the cosmos, such as the collision of black holes.And then there are the grand unanswered questions that continue to tantalize and intrigue us: What lies beyond the observable universe? What is the nature of dark matter and dark energy, the enigmatic forces that seem to drive the expansion of the cosmos? And perhaps the greatest mystery of all – are we alone in this vast expanse, or is there intelligent life elsewhere in the universe?As a student captivated by the wonders of the cosmos, I find myself constantly in awe of the universe's grandeur and complexity. From the familiar stars twinkling overhead to the mind-bending concepts of black holes and quantum mechanics, the universe is a boundless realm of exploration and discovery. And while we may never fully unravel all of its mysteries, the journey of understanding this vast cosmic tapestry is a profoundly enriching and humbling experience.篇3The Universe: A Vast and Wondrous ExpanseHave you ever gazed up at the night sky, mesmerized by the twinkling stars and the luminous moon? If so, you've caught aglimpse of the extraordinary universe that surrounds us. The universe is a boundless realm of mysteries and wonders, and the more we learn about it, the more awe-inspiring it becomes.To begin with, the sheer size of the universe ismind-boggling. It's a vast expanse that stretches far beyond our wildest imaginations. Astronomers estimate that the observable universe, which is the portion we can detect with our current instruments, spans a staggering 93 billion light-years in diameter! That's an inconceivable distance, and it's believed that the actual size of the entire universe is even greater.Within this immense cosmos, countless celestial objects populate the celestial canvas. From the blazing stars that illuminate the night sky to the enigmatic black holes that warp the fabric of space-time, the universe is teeming with phenomena that challenge our comprehension. And at the heart of it all lies our home, the Milky Way galaxy – a colossal pinwheel of stars, gas, and dust, containing billions of stars, including our life-giving Sun.One of the most captivating aspects of the universe is its origin and evolution. According to the widely accepted Big Bang theory, the universe began as an infinitely dense and hot singularity, which expanded rapidly in a colossal explosionapproximately 13.8 billion years ago. From this initial cosmic event, the universe has been continuously expanding and cooling, giving rise to the vast array of galaxies, stars, and other celestial bodies we observe today.The study of the universe is an ongoing pursuit, and scientists are constantly making new discoveries that reshape our understanding of the cosmos. For instance, the recent detection of gravitational waves, ripples in the fabric ofspace-time predicted by Einstein's theory of general relativity, has opened up a new window into the universe, allowing us to observe cataclysmic events like the collision of black holes.Another fascinating aspect of the universe is the search for extraterrestrial life. With the vast number of galaxies and planetary systems out there, the possibility of life existing elsewhere in the universe seems increasingly plausible. Scientists are actively exploring this tantalizing prospect, studying exoplanets (planets orbiting other stars) and searching for biosignatures that could indicate the presence of life beyond our own planet.As we delve deeper into the mysteries of the universe, we are reminded of our humble place in this grand cosmic tapestry. We are but a speck in the vastness of the cosmos, yet our curiosityand scientific endeavors have allowed us to unravel some of the universe's most profound secrets.In conclusion, the universe is a realm of boundless wonders and endless possibilities. From the birth of galaxies to the potential existence of alien civilizations, the cosmos never ceases to captivate and inspire us. As we continue to explore and unravel its mysteries, we embark on a journey of discovery that not only expands our knowledge but also ignites our imaginations and reminds us of our insignificance and yet our significance in the grand scheme of the cosmos.篇4The Vast and Wondrous UniverseHave you ever gazed up at the night sky and felt completely mesmerized by the twinkling stars? I know I have, more times than I can count. The universe is an endlessly fascinating place, full of mysteries and marvels that spark my curiosity and imagination. Let me tell you about some of the mostmind-blowing aspects of the cosmos we call home.To start, the sheer scale of the universe is almost too immense to wrap our minds around. The galaxy we inhabit, the Milky Way, is just one of billions of galaxies out there, each onean island of stars in the dark sea of space. Our solar system is a tiny speck within the Milky Way. And the distances between stars and galaxies are so stupendously vast that it boggles the mind. It would take light, the fastest thing there is, over 100,000 years to travel across our galaxy! The cosmic distances are so extreme they make the size of our planet or even our whole solar system seem almost insignificant.Speaking of stars, these brilliant beacons of light are true cosmic wonders. Stars are massive spheres of superhot gas that generate tremendous amounts of energy through the process of nuclear fusion in their cores. Our sun is a fairly average-sized star, but some stars out there are millions of times larger and brighter. The sheer amount of energy produced by these stellar giants is unimaginable to our human-sized senses. Yet for all their might, even the mightiest stars have a finite lifespan. They burn through their nuclear fuel over billions of years until they eventually run out and die spectacular explosive deaths as supernovas, seeding the universe with heavy elements that went on to form new generations of stars, planets, and even the building blocks of life itself.Our beautiful blue-green world is just one of potentially trillions of planets spinning through the cosmos. In recentdecades, astronomers have discovered thousands of exoplanets circling distant stars using powerful telescopes. Some of these alien worlds are rocky and Earth-like, while others are frozen ice balls or searing gas giants. Many orbit in the "Goldilocks zone" around their parent stars - the perfect distance for conditions that could allow liquid water and maybe even life to exist. The sheer diversity and possibility of habitable worlds out there waiting to be uncovered is a thrilling prospect for future generations of explorers and scientists.As amazing as the wonders listed above may be, they represent just a tiny fraction of the breadth and majesty of the universe. We're talking about a place so vast, so ancient, so filled with wonders that our minds struggle to make sense of it all. And that's what makes it so endlessly thrilling for stargazers, dreamers, thinkers, and explorers like me. There's always a new cosmic marvel waiting to awe and inspire us, fueling our drive to push the boundaries of our knowledge and understanding ever further.The universe is the ultimate arena of the unknown, a canvas of mysteries just begging to be unraveled and turned into adventures of discovery. Who knows what secrets, revelations, or paradigm-shifting truths lie awaiting humankind amongst thestars and galaxies? What we do know is that the more we learn, the more wonders seem to emerge ripe for exploration. Perhaps one day we'll develop the warp drives or wormhole gateways of science fiction and sail the interstellar seas in search of distant worlds and cosmic wonders not yet even imagined. Or perhaps we'll make contact and gain insight from civilizations far more advanced than our own. Anything seems possible when we contemplate the boundless majesty and potential of the universe.I could go on and on about exploding stars, stellar nurseries, rogue planets roaming the cold depths between galaxies, cosmic tsunamis generated by colliding black holes, strange theoretical realms like dark matter and dark energy, and all the other wild, wonderful celestial phenomena out there. But I think you get the idea - the universe is a sublime arena of awe, mystery, and endless opportunity for discovery, an infinite frontier that inspires the explorer within us all. As long as humans gaze outwards with starry eyes full of questions, there's no limit to what we may achieve or篇5The Vast Wonders of the UniverseEver since I was a little kid, I've always been fascinated by the night sky. Gazing up at the twinkling stars and the luminous moon never fails to fill me with a sense of wonder and curiosity. What lies beyond our tiny planet Earth? What mysteries does the universe hold? These are the kinds of questions that have fueled my passion for learning about the cosmos.From what I've studied so far, the universe is amind-bogglingly vast place. It's difficult to wrap my head around just how big it truly is. The universe contains billions upon billions of galaxies, each one a colossal system made up of billions of stars, planets, gas, and dust. Our own galaxy, the Milky Way, is just one tiny speck in this unfathomable vastness.Within our galaxy alone, there are estimated to be over 100 billion stars! The sun, which seems so large and powerful from our vantage point on Earth, is just an average-sized star among this multitude. Many of the other stars out there are much larger than our sun, while some are smaller and cooler. Stars are constantly being born from massive clouds of gas and dust, while older stars eventually run out of fuel and die, sometimes explosively as supernovas.The universe doesn't just contain stars and galaxies though. It's also filled with other bizarre and fascinating phenomena.Black holes, for instance, are incredibly dense objects with gravitational pulls so strong that not even light can escape their grasp. Then there are quasars, which are intensely bright galactic nuclei that can outshine entire galaxies. Pulsars are rapidly spinning neutron stars that emit precise beams of radiation. The more I learn, the more I'm amazed by the variety and strangeness of cosmic objects.While the universe is vast beyond imagination, it all began from an infinitely small, dense point around 13.8 billion years ago in an event known as the Big Bang. All of the matter and energy that now fills the observable universe was once compacted into that single, mind-bogglingly hot and dense point. In the first few fractions of a second after the Big Bang, the fundamental forces of nature began to separate out and the basic building blocks of matter started to form.From those first few particles in the extreme heat and density of the Big Bang, the universe rapidly inflated and cooled, allowing atoms to form after about 380,000 years. These atoms eventually coalesced through gravity into the first stars and galaxies we see today. Incredibly, we can still detect the faint glow of that primordial radiation from nearly 14 billion years ago, which provides evidence for the Big Bang theory.As amazing as it is to ponder the origins and immense scale of the cosmos, what really boggles my mind is the possibility that life may exist elsewhere in the universe. With billions of galaxies out there, each containing billions of stars with their own planetary systems, the odds seem pretty good that at least some of those planets could have developed life, perhaps even intelligent life.While concrete proof remains elusive, I can't help but wonder – what would alien life be like if we encountered it? Would their biology and chemistry be similar to life as we know it on Earth? Or could life take on radically different forms on other worlds? Would alien intelligence be more advanced than ours, or less so? The possibilities are tantalizing to consider.In the meantime, we'll have to be content with exploring our own solar system and the other planets within it. Unmanned robotic probes have already visited every major planet and returned incredible images and data. We've discovered geological and atmospheric conditions unlike anything on Earth. Who knows what other surprises may lie in store as we continue to explore?Personally, I can't get enough of learning about space and our place in this mind-bendingly enormous universe. Every newdiscovery seems to raise more fascinating questions. How did all of this complexity arise from the hot dense state of the early universe? What fundamental laws and forces shape the cosmos on the largest scales? Are there other universes beyond our own?The quest to understand the true nature of the universe is one of humanity's greatest challenges. While we've come a long way in unraveling some of its mysteries through science, logic, and observation, the universe still holds infinite depths of secrets left to explore. Just contemplating its immensity fills me with a sense of humility and excitement. I can't wait to see what amazing revelations the future will bring as our knowledge of the cosmos continues to expand. The universe is a limitless frontier, filled with wonders and possibilities beyond our wildest imaginings.篇6The Vast and Wondrous UniverseEver since I was a little kid, I've been fascinated by the night sky. Staring up at the twinkling stars and the brilliant moon, I couldn't help but wonder what else was out there, waiting to be discovered. As I grew older and learned more about the universe, my sense of awe and curiosity only grew stronger.The universe is a vast, ever-expanding realm that stretches far beyond our comprehension. It's a canvas of galaxies, nebulae, and celestial bodies, each one more mesmerizing than the last. Imagine this – our own Milky Way galaxy, a spiral of stars numbering in the hundreds of billions, is just one tiny speck in the grand scheme of things.Beyond our galaxy lies a realm of unimaginable vastness, filled with countless other galaxies, each one a。
天体英语知识点总结The study of celestial bodies, or what we commonly refer to as heavenly bodies, holds a significant place in the field of astronomy. As humans, we have always been fascinated by the stars, planets, moons, and other celestial objects that exist beyond our planet Earth. In this article, we will explore and summarize some important knowledge points in the study of celestial bodies, their characteristics, and their role in the universe.The Solar SystemThe solar system is a collection of celestial bodies that are gravitationally bound to the sun, which includes eight planets, their moons, dwarf planets, asteroids, and comets. The eight planets in the solar system, in order of their distance from the sun, are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune. Each planet has its own unique characteristics, such as size, composition, and atmosphere, which sets it apart from the others.The sun, at the center of the solar system, is a star that provides heat, light, and energy to all the other celestial bodies within the solar system. It is a massive, spherical body composed mainly of hydrogen and helium, and it is the most significant source of energy for life on Earth.The Oort CloudThe Oort Cloud is a theoretical and hypothetical region of space that is believed to be the source of long-period comets. It is thought to be a shell of icy bodies that surrounds the solar system at a very large distance, extending nearly a light-year from the sun. The Oort Cloud is named after Dutch astronomer Jan Oort, who first proposed its existence in 1950.The Oort Cloud is important in the study of celestial bodies as it provides insight into the origin and evolution of the solar system. It is believed that the comets originating from the Oort Cloud may have played a role in the delivery of water and organic materials to the early Earth, which could have contributed to the development of life on our planet.Stars and GalaxiesStars are massive, luminous spheres of plasma that emit light and heat due to nuclear reactions occurring at their cores. They are the fundamental building blocks of galaxies and play a crucial role in the dynamics of the universe. Stars vary in size, temperature, and luminosity, and they can be classified into different spectral types based on their temperature and color.Galaxies are vast systems of stars, gas, dust, and dark matter that are bound together by gravitational forces. They come in different shapes and sizes, such as spiral, elliptical, and irregular galaxies. The Milky Way, our galaxy, is a barred spiral galaxy that contains hundreds of billions of stars, as well as planets, asteroids, and other celestial objects.Black HolesBlack holes are regions of space where the gravitational pull is so strong that nothing, not even light, can escape from it. They are formed when massive stars collapse under their own gravity at the end of their life cycle. Black holes come in different sizes, ranging from stellar black holes, which are a few times the mass of the sun, to supermassive black holes, which can be millions or even billions of times the mass of the sun.The study of black holes has revolutionized our understanding of the universe, as they are thought to play a crucial role in the evolution and dynamics of galaxies. Black holes have also been the subject of intense research and observation in recent years, with the detection of gravitational waves from the merger of black holes being a significant milestone in our quest to understand these enigmatic celestial bodies.ConclusionThe study of celestial bodies is a fascinating and ever-evolving field that continues to unravel the mysteries of the universe. From the solar system to stars, galaxies, and black holes, each celestial body offers unique insights into the nature of the cosmos and our place within it. As we continue to explore and understand these celestial bodies, we gain a deeper appreciation for the beauty and complexity of the universe in which we live.。
a rXiv:084.3141v2[astro-ph]9J ul28Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies ?K.Omukai 1,R.Schneider 2and Z.Haiman 3ABSTRACT Primordial gas in protogalactic dark matter (DM)halos with virial temper-atures T vir ∼>104K begins to cool and condense via atomic hydrogen.Provided this gas is irradiated by a strong ultraviolet (UV)flux and remains free of H 2and other molecules,it has been proposed that the halo with T vir ∼104K may avoid fragmentation,and lead to the rapid formation of a supermassive black hole (SMBH)as massive as M ≈105−106M ⊙.This “head–start”would help explain the presence of SMBHs with inferred masses of several ×109M ⊙,powering the bright quasars discovered in the Sloan Digital Sky Survey at redshift z ∼>6.However,high–redshift DM halos with T vir ∼104K are likely already enriched with at least trace amounts of metals and dust produced by prior star–formation in their progenitors.Here we study the thermal and chemical evolution of low–metallicity gas exposed to extremely strong UV radiation fields.Our results,obtained in one–zone models,suggest that gas fragmentation is inevitable above a critical metallicity,whose value is between Z cr ≈3×10−4Z ⊙(in the absence of dust)and as low as Z cr ≈5×10−6Z ⊙(with a dust-to-gas mass ratio of about 0.01Z/Z ⊙).We propose that when the metallicity exceeds these critical values,dense clusters of low–mass stars may form at the halo nucleus.Relatively mas-sive stars in such a cluster can then rapidly coalesce into a single more massive object,which may produce an intermediate–mass BH remnant with a mass up to M ∼<102−103M ⊙.Subject headings:cosmology:theory —galaxies:formation —stars:formation1.IntroductionThe discovery of bright quasars at redshifts z∼>6in the Sloan Digital Sky Survey (SDSS)implies that BHs as massive as several×109M⊙were already assembled when the age of the universe was less than≈1Gyr(see the recent review by Fan2006).The BH masses are inferred from the quasars’luminosities,assuming these sources shine near their Eddington limit.Strong gravitational lensing or beaming could,in principle,mean that the inferred BH masses are overestimated;however,there is no obvious sign of either effect in the images and spectra of these quasars(Willott et al.2003;Richards et al.2004).Indeed, their relatively“normal”line–to–continuum ratio,consistent with those in lower–redshift quasars,makes it unlikely that the apparentflux of these sources was significantly boosted by beaming(Haiman&Cen2002).Likewise,the lack of a second detectable image on Hubble Space Telescope images(Richards et al.2004)essentially rules out the hypothesis that most of the sources experienced strong magnification by lensing(Comerford et al.2002;Keeton et al.2005).Relatively little time is available for the growth of several×109M⊙SMBHs prior to z∼6,and their seed BHs must be present as early as z∼10(e.g.Haiman&Loeb 2001).As the SMBHs grow from high–redshift seed BHs by accretion,they are expected to encounter frequent mergers.A coalescing BH binary experiences a strong recoil due to gravitational waves(GWs)emitted during thefinal stages of their merger.The typical recoil speed is expected to be v recoil∼>100km s−1(and may be as large as4,000km s−1for special BH spin configurations;see,e.g.Campanelli et al.2007and references therein),significantly exceeding the escape velocity(∼<10km s−1)from typical DM halos that exist at z∼10.As a result,SMBHs are often ejected from their host halos at high redshift.The repeated loss of the growing seeds makes it especially challenging to account for the several×109M⊙SMBHs at z∼>6without at least a brief phase of super–Eddington accretion,or some equivalent “head–start”(Haiman2004;Yoo&Miralda-Escud´e2005;Shapiro2005;Volonteri&Rees 2006).There have been several recent proposals that such a“head–start”may occur in metal–free gas in high–redshift DM halos with virial temperatures exceeding T vir∼>104K,leading to the rapid formation of SMBHs with a mass of M≈105−106M⊙.As primordial gas falls into these halos,it initially cools via the emission of hydrogen Lyαphotons.Provided the gas is free of H2molecules,its temperature will remain near T vir∼104K.Bromm&Loeb(2003, hereafter BL03)performed hydrodynamical simulations of a metal–and H2–free halo,with a mass of∼108M⊙collapsing at z∼10,corresponding to a2σGaussian overdensity and to T vir∼104K.Under these conditions,which may apply to some dwarf galaxies collapsing close to the epoch of reionization,the primordial gas is marginally able to collapse and remainsnearly isothermal.BL03found that during the evolution,fragmentation of the gas cloudis very inefficient,leading at most to binary formation even with some degree of rotation.Thus,a super–massive star is expected to form,and evolve into a SMBH with a mass ashigh as M≈105−106M⊙.Oh&Haiman(2002)and Lodato&Natarajan(2006)have also showed that if H2formation is inhibited,a primordial-gas disk is stable to fragmentation anda single massive object is formed in accordance with BL03’s conclusion.Volonteri&Rees(2005)arrived at similar conclusions,by considering Bondi accretion onto a stellar seed BH,which can significantly exceed the Eddington rate at the gas density and temperature in asimilar halo.Finally,Begelman et al.(2006)and Spaans&Silk(2006)proposed differentmechanisms to form similarly massive BHs by the direct collapse of primordial,atomic gas.For reference,we note that the total(DM+gas)mass of halos with T vir=(1−5)×104K atz=10is M tot≈108−9M⊙,so that such SMBHs would represent≈0.2−20%of the gas mass in these halos.We also note that in the WMAP5cosmology,the age of the universe at z=10and z=6.5is∼0.5Gyr and∼0.9Gyr,respectively.At the e–folding time–scale of4×107years(assuming Eddington accretion,and a radiative efficiency of10%;see,e.g., Haiman&Loeb2001),a seed BH of M≈105M⊙at z∼10could easily grow to a super massive BH of M≈2×109M⊙at z∼6.5,if fed uninterruptedly.A crucial assumption in all of the above proposals is that H2molecules cannot form as the gas cools and condenses in the DM halo.This assumption can be justified in the presence of a sufficiently strong far ultraviolet(FUV)radiation,so that molecular hydrogen(or the intermediary H−necessary to form H2)is photodissociated.The relevant criterion is that the photodissociation timescale is shorter than the H2–formation timescale;since generically, t diss∝J and t form∝ρ,the condition t diss=t form yields a criticalflux J∝ρ.In DM halos with T vir∼<104K,whose gas can not cool in the absence of H2,the densities remain low and H2can be dissociated even when backgroundflux is as low as J−21∼10−2(e.g.Haiman, Rees&Loeb1997;Mesinger et al.2006;here J−21is theflux just below13.6eV,in the usual units of10−21erg cm−2sr−1s−1Hz−1).However,if a gas cloud is massive enough and has a virial temperature higher than≈8000K,it is able to cool and start its collapse via atomic hydrogen Ly-αcooling.Even if the FUVfield is initially above the critical value,molecular hydrogen can form,and dominate the gas cooling at a later stage during the collapse(Oh& Haiman2002);the H2–formation rate is furthermore strongly boosted by the large out–of–equilibrium abundance of free electrons in the collisionally ionized gas in these halos(Shapiro &Kang1987;Susa et al.1998;Oh&Haiman2002).The criticalflux required to keep the gas H2–free as it collapses by several orders of magnitude therefore increases significantly; for halos with T vir∼104K the value has been found to be J−21≈103−105,depending on the assumed spectral shape(Omukai2001,hereafter O2001;BL03).In halos exposed to such extremely intense UVfields,the gas cloud is still able to collapse only via atomic hydrogenline cooling,namely Lyαand H−free–bound(f-b)emission(O2001).One possible source of such an intense UVfield is the intergalactic UV background just before the epoch of cosmic reionization(BL03).The ionizing photonflux J+21can be evaluated from the number density of hydrogen atoms in the intergalactic medium(IGM) and the average number of photons needed to ionize a hydrogen atom Nγ,which,in general, is>1,owing to recombinations in an inhomogeneous ing the escape fraction of ionizing radiation f esc,theflux J−21just below the Lyman limit is given byJ−21=J+21f eschcm H≃4×103Nγ0.01 −1 1+zIn the present paper,our goal is to answer the following question:can cooling and fragmentation be avoided in metal–enriched T vir∼>104K halos,irradiated by a strong FUV flux?If so,this would suggest that supermassive black holes may form,similar to the metal–free case,in the more likely case of metal–enriched high–redshift protogalaxies.To investigate this possibility,we here study the thermal and chemical evolution of low–metallicity gas, exposed to extremely strong UV radiationfields.We will evaluate the critical metallicity, above which fragmentation becomes unavoidable in the presence of a strong FUVflux.In§2,we describe our one–zone modeling procedure.Our results are presented and discussed in§3,first for the metal–free(§3.1),and then for the metal–enriched case(§3.2). The fragmentation and subsequent evolution of the metal–enriched clouds are then discussed in§3.3and3.4,respectively.In§4,we summarize our results and offer our conclusions.2.Model2.1.BasicsWe use the one–zone model described in Omukai(2001)to follow the gravitational collapse of gas clouds.The model includes a detailed description of gas–phase chemistry and radiative processes,and the effect of dark matter on the dynamics in a simplified fashion.In addition,in the present version of the model we have implemented the contribution of metal lines and dust to gas cooling.In what follows,all physical quantities are evaluated at the center of the cloud.The gas density increases asdρgast col.(2) where the collapse timescale,t col,is taken to be equal to the free-fall time,t col=tff≡ 32Gρ,(3) andρis the sum of the gas and dark matter density.The dark matter density follows the evolution of a top–hat overdensity,ρDM=9π21−cosθ 3ΩDMρcrit(4)with1+z=(1+z ta) θ−sinθ(e.g.,Chapter8.2of Padmanabhan1993),where the turn-around and the virialization cor-respond toθ=πand2π,respectively.Although,strictly speaking,this is correct only inthe Einstein-de Sitter universe(Ω0=1),it does not cause a significant error in the high-zuniverse(z 10)we consider.The initial epoch of calculation is taken at the turn–around at redshift z ta=17.Fromequation5,the virialization and turn-around redshifts have the relation1+z vir=2−2/3(1+z ta);thus z vir≃10.In our calculation,the dark matter density is kept constant after reaching its virialization value8ρDM(z ta).The initial values of the gas number density,temperature,ionization degree,and H2fraction have been assumed to be n H=4.5×10−3cm−3,T=21K,y(e)=3.7×10−4and y(H2)=2×10−6,respectively,to reflect conditions at the turn–aroundat z ta=17.Some runs with initial temperature ten times higher(210K)are also performedto confirm independence of our main results from the initial temperature.The cosmologicalparameters areΩDM=0.24,Ωb=0.04,and h=0.7.Our calculation does not include the virialization shock.Owing to fast cooling by Lyαemission,the central region whose evolution we intend to follow does not experience thevirialization shock in the spherically symmetric case(Birnboim&Dekel2003).In more real-istic calculations,the outer regions can experience shocks and the temperature and electronfraction become higher than in our case.In addition,recent numerical calculations(e.g.Kereˇs et al.2005)show that low-mass galaxies,especially at high-redshifts,obtain their gasthrough accretion predominantly along the large-scalefilaments.Three-dimensional effectssuch as asymmetric accretion might affect the evolution at low densities.However,since weare considering halos with T vir≃104K,which can marginally collapse by Lyαcooling,the shock is not strong:the temperature increase is modest and the electron fraction reaches at most 10−2(see Figures5a and5c in BL03).This additional electrons alter the early evolution for the J=0case.However,in the irradiated clouds,where H2formation is suppressed,during the collapse by the Lyαcooling recombination proceeds until the free electron fraction reaches x e≃1.2×10−3n−1/2H,the value set by the balance between the recombination and the collapse time t rec∼t col at8000K.Thus,our results for molecule formation and cooling are hardly affected.We adopt tffas the collapse time scale just because it has been widely used in otherstudies(e.g.,Palla et al.1983).Note that the free–fall time(3)is the time for density of aninitially static cloud to reach infinity,while the dynamical timescale t col=ρ/(dρ/dt)in thefree–fall collapse ist col,ff=124πGρ(6)in the limit where the density has become sufficiently larger than the initial value.Thus the rate we adopted(3)is3π/2=4.7times slower collapse than the genuine free–fall one.Infact,pressure gradients oppose gravity and the collapse becomes slower than the free–fall one within a factor of a few(e.g.,Foster&Chevalier1993).Adoption of tffas the e–folding time for density increase mimics the pressure effect.The assumption of nearly free-fall collapse is invalidated,and the collapse is slowed down,once the cloud becomes optically thick to continuum radiation.However,our result on the thermal evolution is not altered:with little radiative cooling,the temperature is now determined by the adiabatic compression and the chemical cooling by dissociation and ionization,both of which are independent of the collapse timescale.Moreover,the evolution after the cloud becomes optically thick is not relevant to our argument on fragmentation,which occurs at much lower density,in the optically thin regime.The overall size of the collapsing gas cloud(or of the roughly uniform density central region)determines its optical depth,and is therefore important for its thermal evolution. Here we assume the size equals the Jeans length,λJ= Gρgasµm H,(7)where T gas is the gas temperature,µis the mean molecular weight.Similarly,its mass is given by the Jeans massM J=ρgasλ3J.(8) Specifically,we assume that the radius of the cloud is R c=λJ/2and the optical depth isτν=κνR c=κν λJdt =−pdρgas −Λnet γad−1kT gascontinuum emission,as well as emission by H and H2lines,and chemical heating/cooling, the net cooling rate includes emission by C and Ofine–structure linesΛmetal,by dust grains Λgr,and heating by photoelectric emission of dust grainsΓpe.Cooling byfine–structure lines of[CII]and[OI]is included as in Omukai(2000).Dust processes are described below in §2.2.Primordial–gas chemical reactions are solved for the nine species of H,H2,e,H+,H+2, H−,He,He+,and He++.We do not explicitly include the chemical reactions involving metals. Instead,all the carbon and oxygen is assumed to be in the form of CII and OI,respectively. Having a lower ionization energy(11.26eV)than hydrogen,carbon remains in the form of CII in the atomic medium owing to photoionization by the background radiation.We maintained this assumption even in J=0runs,although carbon is expected to recombine and become neutral in these cases.The cooling rates by CII and CIfine–structure lines are within a factor of≃2difference for T 30K,and therefore this assumption does not significantly affect the results.On the other hand,the ionization potential of oxygen (13.61eV)is very similar to that of hydrogen(13.60eV)and the charge exchange reactionO++H↔H++O,(12) keeps its ionization degree equal to that of hydrogen.In fact,the coefficient of the rightwardyr. reaction being6.8×10−10cm3/sec,these reactions reach equilibrium only in∼50n−1H In a cold( a few100K)and dense( 103−4cm−3)environment,molecular coolants such as CO and H2O may become important(Omukai et al.2005).Since we are interested here in metal effects on warm( a few1000K)atomic clouds,we neglect the contribution to cooling of metals in molecules.This simplification does not affect the early evolution of gas clouds,when the effects of metals induce a deviation from the primordial evolutionary track at several1000K.It is true that it may alter the predicted thermal behavior at later stages, when the gas has cooled significantly( 1000K).However,even in such cold environments, the error in the temperature caused by neglect of metal molecular coolants is very small(see Figure10of Omukai et al.2005)and the thermal evolution is well reproduced when only dust processes andfine–structure line cooling of C and O are considered.2.2.Dust ProcessesDust in the local interstellar medium(ISM)originates mainly from the asymptotic giant–branch(AGB)stars,whose age is 1Gyr,longer than the Hubble time at z 6.At higher redshifts,supernovae(SNe)are considered to be the major dust factories.Indeed, the observed extinction law of high–z quasars and gamma–ray bursts can be well reproducedby this scenario(Maiolino et al.2004,Stratta et al.2007).Dust grains produced in SN ejecta are more effective in cooling and H2formation because of their smaller size and larger area per unit mass(Schneider et al.2006).However,their composition and size distribution are still affected by many uncertainties,such as the degree of mixing in the ejecta and the efficiency of grain condensation and their destruction by the reverse shock(Nozawa et al. 2007,Bianchi&Schneider2007).To be conservative,in this work the properties of dust,such as grain composition and size distribution,are assumed to be similar to those in the solar neighborhood and its amount is reduced in proportion to the assumed metallicity of the gas clouds.Specifically,we adopt the dust opacity model developed by Semenov et al.(2003).This model partly follows the scheme proposed by Pollack et al.(1994),which was used in Omukai et al.(2005),assuming the same dust composition,size distribution and evaporation temperatures,but uses a new set of dust optical constants.Overall,the opacity curves of the two models are in good agreement,the largest difference being at most a factor of two(see Semenov et al.2003 for a thorough discussion).The main dust constituents include amorphous pyroxene([Fe, Mg]SiO3),olivine([Fe,Mg]2SiO4),volatile and refractory organics,amorphous water ice, troilite(FeS)and iron.The grains are assumed to follow a size distribution modified from that by Mathis,Rumpl,&Nordsieck(1977)with the inclusion of large(0.5-5)µm grains.At each density and gas temperature,the dust is assumed to be in thermal equilibrium, and its temperature T gr,which is followed separately from the gas temperature,is determined by the energy balance equation4π κa,νBν(T gr)dν=Λgas→dust+4π κa,νJ inνdν.(13) HereΛgas→dust is the energy transfer rate per unit mass from gas to dust due to gas–dust collisions,which we take from Hollenbach&McKee(1979),κa,νis the absorption opacity of dust,and J inνis the mean intensity of the radiationfield inside the cloud.Note that Λgas→dust also represents the net cooling rate of the gas,caused by the presence of dust grains at temperature T gr.We model the external radiationfield assuming a diluted thermal spectrum(i.e.a blackbody spectrum,scaled by an overall constant representing a mean geometrical dilution).Its shape is then fully described by only two free parameters,J21,the mean intensity at the Lyman limit(νH)and T∗,the color temperature,(T∗)]erg cm−2sr−1s−1Hz−1.(14) J exν=J2110−21[Bν(T∗)/BνHIn the following,we will consider two possible values for the radiation color temperature,T∗= 104K and105K,representing“standard”Population II stars and very massive Population III stars,respectively.Given the mean intensity of the external radiationfield J exν,thefieldinside the gas cloud is obtained as(see O2001),J inν=J exν+ξνxνS a,ν[1+4×10−3(G0T1/2/n(e))0.73]+3.7×10−2(T/10−4)0.71+4.0×10−2(T+T gr)1/2+2.0×10−3T+8.0×10−6T2(21) wheref a=[1+exp(7.5×102(1/75−1/T gr))]−1.(22)3.ResultsIn what follows,we willfirst discuss the results obtained for the thermal evolution of metal–free gas clouds,and then describe the effects induced by the presence of metals and dust grains.3.1.Metal–free CloudsThe thermal evolution of metal–free clouds irradiated by a FUV radiation backgroundis expected to change with radiation temperature T∗and intensity J21.The models witha radiation temperature of T∗=104K(105K)are shown in Figure1(2,respectively)fordifferent values of intensity J21.Initially,i.e.at low densities,the temperature increases adiabatically,because there isnot enough H2to activate cooling.In the no radiation case,when the density is∼1cm−3and the temperature is∼1000K,sufficient H2is formed and,as a result,the temperaturedecreases.It is to be noted that the relatively low temperature where this condition is metdoes not contradict previous results(BL03).In fact,the predicted temperature of eachfluidelement in the simulation of BL03shows a large scatter at low densities.This scatter reflectsthe radial temperature gradient,and the central value,which we calculate here,correspondsto the lower boundary of the scattered points and it is in agreement with our result.Weexpect that the central temperature of the gas cloud does not reach the virial temperatureof the host dark matter halo since the innermost region starts to cool and collapse duringthe adiabatic compression and does not experience the virialization shock.As the external radiation intensity J21increases,the onset of H2cooling is delayedbecause higher densities and temperatures are required for H2formation to compensate forthe photodissociation.If the UV intensity is below a threshold value,J21,thr,which wefindto be in the range102−103for T∗=104K and(1−3)×105for T∗=105K,there is always a density at which H2cooling starts to become effective.The temperature then decreasesand eventually reaches the no–radiation evolutionary track,along which it evolves thereafter.On the other hand,if the radiation is stronger than the threshold value,H2cooling neverbecomes important.In this case,atomic hydrogen cooling by H excitation(for 107cm−3)and H−free-bound(f-b)emission(for 107cm−3),are the main cooling channels(see Figure3).In Figure1,runs with higher initial temperature(210K)are also shown(dotted lines).During the initial adiabatic phase,the temperature at a given density is proportional to itsinitial value,and thus higher in runs with higher initial temperature.However,after theonset of efficient radiative cooling,these initially different thermal evolutionary tracks soonconverge.At higher densities,the results are independent of the initial temperature(seeFigure1).As it can be inferred from Figs.1and2,wefind that the threshold value,J21,thr,islower for a radiation temperature of T∗=104K than for T∗=105K.Thus,for comparableradiation intensities,J21,the lower T∗radiation has a stronger impact on the cloud evolution.To understand why this is the case,in Figure4we show the H2and H−photodissociation rates,for the same intensity J21=1.The dilution factor W,defined by Jν≡W Bν(T∗), which was used in Omukai&Yoshii(2003),is also shown for reference.As thefigure shows, the H−photodissociation rate decreases steeply with T∗,while the H2photodissociation rate remains nearly constant.The H2and H−photodissociation rate coefficients arek H=1.4×109Jν(12.4eV)(23)2phin the unattenuated case andk H−ph= 0.755eV4πJνSince the compressional heating rate−p dρgas =pβ−1.(30)Both the H line and H−f-b emissions are very sensitive to temperature,and thusβ>1.For those collisional processes,α=2forfixed chemical abundances.With chemical evolution, it deviates from2,but remains>3/2.Therefore,the exponent in equation(30)is negative for the atomic-cooling track as long as the cloud is optically thin:the temperature decreases with density as observed in Figures1and2.On the other hand,on the molecular-cooling track,α=1for densities higher than the critical value for the LTE.Thus,the temperature increases with density for n H 104cm−3.The existence of a threshold UV background and the discontinuity of thermal evolution at this value are due to the presence of non-local thermodynamic equilibrium(non-LTE)to LTE transition of H2ro–vibrational level population at∼104cm−3.When the gas density is higher than this value,the cooling rate saturates and more H2is needed to compensate for compressional heating.In addition,after the LTE is reached,collisional dissociation rate is enhanced owing to a large H2level population in the excited levels.Thus,if a strong FUV radiation delays H2formation and cooling until the critical density for LTE is reached,a fraction of the remaining H2is collisionally dissociated.Thus the gas cloud is no longer able to cool by H2even at a later phase of the evolution.On the other hand,if the UV background is slightly smaller than the threshold,the cloud begins to cool by H2and the temperature begins to fall before the collisional dissociation effect becomes significant(see Figure5b in Omukai2001for cooling rates by each process in such a case).The lower temperature allows further H2formation and resultant cooling.The cooling proceeds in this accerelated fashion and the temperature eventually reaches the molecular cooling track.This is the origin of the dichotomy between the atomic and molecular cooling tracks.To summarize,the main effect of the FUV radiation is to photodissociate H2directly and to decrease the H2formation rate through photodissociating H−.If these two processes inhibit H2formation and cooling until the critical density for LTE is reached,the gas remains warm( several thousands K) and H2is collisionally dissociated at higher densities.Thus the high density evolution is not affected by the presence of the FUVfield and depends only on the temperature at the H2 critical density.3.2.Metallicity Effects on Irradiated CloudsIn this section,we show the effects induced by the presence of metals and dust grains on the thermal evolution of gas clouds irradiated by a FUVfield with a mean intensity larger than J21,thr.In what follows,the total metallicity is expressed relative to the solar value, as[M/H]≡log(Z/Z⊙).Unless specified otherwise,the fractions of metals in the gas phase and in dust grains are assumed to be the same as in the interstellar medium(ISM)of the Galaxy.Specifically,the number fractions of C and O nuclei in the gas phase with respect to H nuclei are y C,gas=0.927×10−4Z/Z⊙and y O,gas=3.568×10−4Z/Z⊙.The mass fraction of dust grains relative to the mass in gas is0.939×10−2Z/Z⊙below the ice-vaporization temperature(T gr 100K).In Figure5we present the thermal evolution of clouds with metallicity in the range −6≤[M/H]≤−3irradiated by extremely strong FUV radiationfields.The parameters of the radiationfields are(a)T∗=104K,J21=103and(b)T∗=105K,J21=3×105, respectively.Under these conditions,the clouds would collapse only via atomic cooling in the absence of metals or dust grains(see Figs.1and2).For a metallicity as low as [M/H] −6,the predicted thermal evolution follows the metal–free track.In both panels of Figure5,deviations from the metal–free tracks start to appear at a density∼1011cm−3 when the metallicity is[M/H]≃−5.3.For the sake of comparison,thin lines show the expected evolution in the absence of radiation for the same initial values of metallicity. At metallicity[M/H]=−5.3,although the temperature drops and eventually reaches the molecular-cooling track at∼1016cm−3,this arrival is after the minimum in the molecular cooling at∼1014cm−3.With a slightly higer metallicity of[M/H]=−5,this arrival takes place at∼1011−12cm−3,and the temperature subsequently decreases to the minimum in the no-radiation case.For higher metallicities,the temperature drop occurs at lower density and the temperature minima becomes lower.In Figure6we show the cooling and heating rates contributed by each process during the evolution of the cloud with T∗=104K,J21=103 and[M/H]=-5.Up to1010cm−3,cooling is dominated by the H line emission(denoted as “H”in the Figure; 107cm−3)and H−f-b emission(“H−f-b”; 107cm−3),and the cloud collapses along the atomic cooling track(see Fig.5a).However,at a density∼1010cm−3, cooling by the dust grain(“grain”)becomes dominant and causes the sudden temperature drop.Now the temperature is lower than that in the atomic cooling track,the H2collisional dissociation rate is also reduced,which causes a high equilibrium value of the H2fraction. As a result of H2cooling,the temperature decreases further,although this effect is almost completely balanced by heating due to H2formation(“H2form”).Note thatfine-structure line cooling(“CII,OI”)is not important at such low metallicities(see the discussion below). Eventually,the thermal evolutionary tracks reach those of the corresponding metallicity in the no–radiation case(shown as thin curves in Fig.5)and evolve along them thereafter.。