Investigating the nature of absorption lines in the Chandra X-ray spectra of the neutron st
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Investigating the properties oforganic compoundsOrganic chemistry is the study of compounds that contain carbon. Organic compounds are found in living organisms, as well as in man-made products such as plastics and fuels. Investigating the properties of organic compounds is essential for understanding their behavior and potential applications.One important property of organic compounds is their molecular structure. Organic molecules come in many shapes and sizes, and their structure often determines their chemical and physical properties. For example, the structure of a molecule can affect its polarity, which in turn can affect its solubility in water or other solvents. Molecular structure can also affect reactivity, with some molecules being more prone to chemical reactions than others.Another important property of organic compounds is their functional groups. A functional group is a group of atoms that confers specific chemical properties to a molecule. For example, the carboxyl group (-COOH) is found in organic acids and is responsible for their acidic properties. The hydroxyl group (-OH) is found in alcohols and is responsible for their ability to form hydrogen bonds and dissolve in water.The physical properties of organic compounds are also important to investigate. These properties include melting and boiling points, density, and refractive index. The physical properties of a compound depend on the intermolecular forces between its molecules. For example, compounds with strong intermolecular forces tend to have higher boiling and melting points and are often solids at room temperature. Compounds with weaker intermolecular forces tend to have lower boiling and melting points and tend to be gases or liquids at room temperature.Chemical properties are also crucial in understanding the behavior of organic compounds. Chemical properties describe how a compound reacts chemically with other substances. Organic compounds can undergo a wide variety of chemical reactions, suchas combustion, oxidation, reduction, substitution, elimination, and addition. Understanding these reactions is important for developing new organic compounds and for understanding the behavior of existing ones.In addition to the properties themselves, the methods used to investigate the properties of organic compounds are also important. Several experimental techniques are commonly used to study the properties of organic compounds, including infrared spectroscopy, nuclear magnetic resonance (NMR) spectroscopy, and mass spectrometry. These techniques allow scientists to observe the vibrations, magnetic fields, and masses of molecules, respectively, and can provide valuable information about a compound's structure and properties.In summary, investigating the properties of organic compounds is crucial for understanding their behavior and potential applications. The properties of organic compounds include molecular structure, functional groups, physical properties, and chemical properties. Experimental techniques such as spectroscopy and mass spectrometry are commonly used to investigate these properties. By understanding these properties, scientists and engineers can design new organic compounds with specific properties and applications.。
Investigating the Nature of DarkMatterThe phrase “dark matter” has become a buzzword in modern astrophysics as well as popular culture, and yet we still know very little about what dark matter really is. It is a mysterious substance that makes up 27% of the universe and that cannot be observed directly, but can only be inferred from the gravitational effects it has on visible matter. Therefore, dark matter is a topic of intense research and debate in the scientific community. In this article, we will explore the key aspects of dark matter and the different ways scientists are working to uncover its nature.What is Dark Matter?As mentioned, dark matter is a substance that does not emit, absorb or reflect light, hence its name. It does not interact strongly with electromagnetic forces, but it does with gravity, which is why its presence can be inferred from the gravitational effects it has on visible matter. One of the most well-known examples of this is the rotation curve of spiral galaxies. According to the laws of classical mechanics, the velocity of stars and gas in a galaxy should decrease as one moves away from the center, as the gravitational attraction of the visible matter decreases. However, observations have shown that the velocity remains constant or even increases, suggesting that there is an invisible mass that is causing this anomaly. This invisible mass is the dark matter.Another piece of evidence for the existence of dark matter is the distribution of matter in the universe as revealed by the cosmic microwave background radiation, which is the afterglow of the Big Bang. The pattern of temperature fluctuations in this radiation shows that the matter in the universe is not distributed evenly, but is rather clumped up in large structures such as galaxies and clusters of galaxies. However, this clumping up cannot be explained solely by the gravitational influence of visible matter; there must be an additional source of gravity, i.e. dark matter, to explain the observed distribution.Moreover, measurements of the large-scale structure of the universe, such as the distribution of galaxies and galaxy clusters, also point to the existence of dark matter.What is Dark Matter Made of?Despite its importance in shaping the structure of the universe, the identity of dark matter remains unknown. There are several hypotheses about what dark matter might be made of, but none of them has been conclusively proven yet. One popular hypothesis is that dark matter is composed of weakly interacting massive particles (WIMPs), which are hypothetical particles that would interact with normal matter only through the weak nuclear force and gravity. The idea is that WIMPs were produced in the early universe when it was hot and dense, and have been moving around freely ever since. If they collide with normal matter, they would transfer some of their energy and momentum, producing detectable signals. In fact, several experiments have been designed to detect WIMP interactions, such as the Large Underground Xenon (LUX) experiment and the Super Cryogenic Dark Matter Search (SuperCDMS).Another hypothesis is that dark matter is made of axions, which are theoretical particles that were originally proposed to explain a different problem in physics, the strong CP problem. The idea is that axions would be very light and weakly interacting, making them difficult to detect, but would still affect the motion of galaxies and other cosmic structures. The Axion Dark Matter eXperiment (ADMX) is currently searching for evidence of axions in a laboratory at the University of Washington.A third hypothesis is that dark matter is composed of primordial black holes, which are black holes that were formed by the collapse of a density fluctuation in the early universe. The idea is that these black holes could have a mass range that would make them more likely to be dark matter, and that their interactions with normal matter could produce observable effects. However, this hypothesis is less favored by most researchers, as the formation and stability of such black holes would require very specific conditions.ConclusionDespite decades of research, the nature of dark matter remains one of the most intriguing and elusive topics in astrophysics. It remains a theoretical construct that cannot be directly observed, but its effects on the motion and structure of the cosmos are undeniable. Researchers are continuing to study dark matter using a variety of tools and techniques, from telescopes that measure gravitational lensing to underground experiments that look for WIMP interactions. The hope is that someday we will finally be able to unravel the mystery of what dark matter is made of, and in doing so, gain a better understanding of the universe and our place in it.。
光不能穿过物体英语作文Title: The Phenomenon of Light Not Passing Through Objects。
Introduction:The phenomenon of light being unable to pass through certain objects is a fascinating aspect of physics that has intrigued scientists and thinkers for centuries. Whilelight is often considered as an omnipresent force capable of penetrating through various mediums, there exist materials that can block or obstruct its passage. In this essay, we will explore the science behind this phenomenon, its practical implications, and its significance in our understanding of the natural world.Understanding Light and Matter:Light, as we know it, travels in the form of electromagnetic waves. These waves propagate through spaceuntil they encounter an obstacle or a medium with different optical properties. When light interacts with matter, several processes can occur, including reflection, refraction, absorption, and transmission. The ability of a material to allow light to pass through it depends on its molecular structure and the energy levels of itsconstituent particles.Factors Affecting Light Transmission:The transmission of light through a material depends on various factors, including the wavelength of light, the density of the material, and its chemical composition. Materials such as glass, air, and water are transparent to visible light because their molecular structures allow photons to pass through relatively unhindered. On the other hand, opaque materials like metals and dense ceramicsabsorb or reflect light, preventing it from passing through. Mechanisms of Light Blocking:The inability of certain materials to transmit lightcan be attributed to different mechanisms. In some cases, the atoms or molecules in the material absorb the photons, converting their energy into internal vibrations or electronic transitions. This absorption process effectively prevents the light from propagating through the material. In other cases, the material may scatter or reflect light due to irregularities in its structure, further inhibiting its transmission.Applications and Implications:The phenomenon of light blocking has numerous practical applications across various fields. In architecture and design, opaque materials are used to create privacy and control the amount of light entering a space. In photography and imaging, the manipulation of light-blocking materials allows for the creation of shadows, contrasts, and artistic effects. Moreover, in industries such asoptics and telecommunications, the development of materials with specific light-blocking properties is crucial for the fabrication of lenses, filters, and optical fibers.Scientific Significance:The study of materials that block light not only has practical applications but also contributes to our understanding of fundamental physical principles. By investigating the interaction between light and matter at the atomic and molecular levels, scientists gain insights into the behavior of photons and the electronic structure of materials. This knowledge is essential for advancing fields such as quantum mechanics, photonics, and materials science.Conclusion:In conclusion, the phenomenon of light being unable to pass through certain objects is a complex yet intriguing aspect of physics. Through the study of light-blocking materials, scientists have gained valuable insights into the nature of electromagnetic waves and the behavior of matter at the atomic scale. Moreover, the practical applications of this phenomenon underscore its significance in everyday life, from architecture and design totelecommunications and scientific research. As our understanding of light and matter continues to deepen, so too will our ability to harness and manipulate these phenomena for the benefit of society.。
大学英语范文欣赏加强自然资源保护意识大学英语范文欣赏加强自然资源保护意识conquer v.征服,战胜,占领;克服,破除conquest n.征服conscience n.良心,良知conscientious a.认真的,conservation n.保存,保护,保守;守恒,不灭conservative a.保守的,守旧的n.保守主义者considerable a.相当大的`,可观的;值得考虑的considerate a.考虑周到的.体谅的consideration n.需要考虑的事,理由;考虑,思考;体谅,照顾consist v.在于,存在于;由组成,由构成consistent a.前后一致的,始终如一的consolidate v.稳固,加强conspicuous a.显眼的,明显的constant a.经常的,不断的;坚决的,永恒的,忠实的n.常数,恒量constituent a.形成的,组成的n.成分,要素constitute v.组成,构成constitution n.构成,构造,组成,成分;体格,体质;宪法A party consisted of ten conservatives. They were conscientious men. In consequence of their conscience, they worked constantly to raise peoples consciousness on the conservation of natural resources. They said that the humanbeing kept conquering nature and in consequence one day we would pay for the conquest at a considerable cost. Its conspicuous that forest was getting less and less. Consequently, every conscious person should give careful consideration to this problem. The ideas in their speeches were consistent. Analyzing their speech into its constituent parts, we knew that the strength of it consisted in the justice of it. Many people consented to support them. So their confidences were consolidated. The consensus of opinion at the latest meeting was that they would try to persuade the Congress to constitute some new constitutions. They were really considerate!。
Investigating the Properties ofMaterialsInvestigating the properties of materials is an essential aspect of scientific research and development. Understanding how different materials behave under various conditions can lead to the creation of new and improved products, as well as advancements in technology and engineering. This process involves testing and analyzing the physical, chemical, and mechanical properties of materials to determine their suitability for specific applications. One of the key properties of materials that scientists and researchers investigate is their strength and durability. This involves testing the material's ability to withstand external forces, such as tension, compression, or bending, without breaking or deforming.By understanding the strength and durability of materials, engineers can design structures and products that are safe and long-lasting. For example, in the construction industry, the strength of materials such as concrete, steel, and wood is crucial for ensuring the stability and integrity of buildings and infrastructure. Another important property of materials is their thermal conductivity, which refers to their ability to conduct heat. This property is particularly significant in industries such as electronics and manufacturing, where the efficient transfer of heat is essential for maintaining the performance and reliability of equipment and processes. By investigating the thermal conductivity of materials, scientists can develop new materials with improved heat transfer capabilities, leading to advancements in thermal management and energy efficiency. In addition to strength and thermal conductivity, the electrical conductivity of materials is also a critical property that researchers investigate. Electrical conductivity refers to the ability of a material to conduct an electric current, and it is a fundamental property in the design and manufacturing of electronic devices and components. By studying the electrical conductivity of materials, scientists can develop new conductive materials that are essential for the advancement of technologies such as semiconductors, batteries, and electrical wiring. Furthermore, the chemical properties of materials play a significant role in their suitability for specific applications. For example, in the pharmaceuticalindustry, researchers investigate the chemical stability and reactivity of materials to ensure the safety and efficacy of drugs and medical devices. Understanding the chemical properties of materials is also crucial in the development of new materials for environmental remediation, such as adsorbents and catalysts for pollution control and waste treatment. Moreover, the optical properties of materials, such as their ability to transmit, reflect, or absorb light, are essential for a wide range of applications, including optics, photonics, and display technologies. Investigating the optical properties of materials allows scientists to develop new materials with improved optical performance, leading to advancements in imaging, communication, and lighting systems. In conclusion, investigating the properties of materials is a multifaceted and essential aspectof scientific research and development. By understanding and manipulating the physical, chemical, and mechanical properties of materials, scientists and researchers can drive innovation and progress in various industries, leading tothe creation of new and improved products, as well as advancements in technology and engineering. This process involves testing and analyzing the strength, thermal and electrical conductivity, chemical stability, and optical performance of materials to determine their suitability for specific applications. Ultimately,the investigation of material properties is fundamental to the advancement of science and technology, and it continues to play a crucial role in shaping the world around us.。
“PEP”2024年小学三年级英语第三单元全练全测(含答案)考试时间:100分钟(总分:120)A卷考试人:_________题号一二三四五总分得分一、综合题(共计100题共100分)1. 填空题:My favorite toy is a ________ (弹珠). I love to collect and trade them with my ________ (朋友).2. 听力题:He is learning to ___. (write)3. 填空题:I have a pet ___ (小鸽子) that coos softly.4. 选择题:What is the capital city of China?A. ShanghaiB. BeijingC. Hong KongD. Xi'an答案:B5. 填空题:The pigeon coos softly in the _________. (城市)6. 选择题:What is the main function of a space telescope?A. To observe celestial objects without atmospheric interferenceB. To communicate with EarthC. To send astronauts into spaceD. To monitor weather patterns7. 填空题:The _____ (水果) of the berry plant is very nutritious.8. 填空题:The starfish has five ________________ (臂).9. 选择题:Which fruit is known for being tropical and having a spiky exterior?A. MangoB. PineappleC. BananaD. Coconut10. horizon) is where the sky meets the land or sea. 填空题:The ____11. 听力题:The chemical symbol for nitrogen is ______.12. 听力题:We will _______ (have) a barbecue this weekend.13. 选择题:Which of these is a popular fruit?A. LettuceB. SpinachC. MangoD. Broccoli答案:C14. 听力题:A polymer is a large molecule composed of many ______.15. 填空题:My sister is a _____ (作家) who explores diverse themes.16. 填空题:The __________ (历史的视野) invites exploration.17. 选择题:What do you call the process of producing energy from food?A. DigestionB. AbsorptionC. FermentationD. Respiration答案: A18. 选择题:Which animal is known for its ability to change colors?A. ChameleonB. FrogC. LizardD. Snake答案:A19. 听力题:A gas expands to fill the _______ of its container.20. 听力题:The __________ is a region known for its natural parks.21. 选择题:What do you call a young dolphin?A. CalfB. KitC. PupD. Cub22. 选择题:What do you call a story that is passed down through generations?A. FolktaleB. LegendC. MythD. Fable答案:A23. 听力题:Galileo was one of the first to use a ______.24. 选择题:Which holiday is celebrated on December 25th?A. ThanksgivingB. HalloweenC. ChristmasD. New Year答案:C25. 填空题:A parakeet's social behavior makes it a friendly ________________ (伴侣).26. 选择题:What do you call a person who writes poems?A. NovelistB. PoetC. AuthorD. Playwright答案:B27. 填空题:I got a new ________ (滑板) last week. I practice riding it in my ________ (车库).28. 听力题:The ________ (workshop) builds capacity.29. erranean Sea is located between ________ (地中海位于________之间). 填空题:The Medi30. 填空题:I enjoy riding my ______.31. 听力题:My brother is a ______. He likes to skateboard.32. 填空题:The ancient Romans were known for their military ________ (力量).33. 选择题:What is the capital city of Ghana?A. AccraB. KumasiC. TamaleD. Takoradi34. 填空题:My uncle is a __________ (商人).35. 选择题:What is the term for a journey made for pleasure?A. ExpeditionB. TripC. AdventureD. Quest答案:B36. 填空题:They are _______ (去) to the beach this weekend.37. 填空题:The __________ (历史的展现方式) affects audience engagement.She is a historian, ______ (她是一名历史学家), preserving important stories.39. 填空题:The kitten is chasing a ______ (小虫). It is very ______ (搞笑).40. 听力题:The __________ is a well-known landmark of freedom.41. 填空题:When we got home, I shared my day’s adventures with my friends online. They were excited to hear about the fun we had at the ______ (10).42. 填空题:The frog jumps from ______ to ______.43. 听力题:A ____ is often found swimming in ponds and has smooth skin.44. 选择题:What is the capital city of Egypt?A. CairoB. GizaC. AlexandriaD. Luxor45. 填空题:My __________ (玩具名) helps me to relax when I __________ (动词).46. 选择题:Which insect makes honey?A. AntB. FlyC. BeeD. Butterfly答案:C47. 选择题:What do you call a person who studies space?A. BiologistB. AstronomerC. GeologistD. Chemist48. 填空题:The _____ (sorrel) plant has a tangy flavor.The solid produced in a chemical reaction is called a __________.50. 听力题:A covalent bond is formed when atoms ______ electrons.51. 听力题:The chemical formula for potassium carbonate is _____.52. 填空题:The ________ (环境变化研究) informs practices.53. 填空题:The _______ (小肉桂) has a distinct smell and flavor.54. 填空题:The ancient Egyptians developed ________ for agricultural practices.55. 听力题:The process of making wine involves fermentation of _______.56. 填空题:The __________ (交通工具) varies in different regions.57. 听力题:A ______ is a geological feature that rises sharply.58. 填空题:We also share similar interests, like ______ and ______. Sometimes, we spend hours talking about our favorite books or movies. It’s amazing how we can understand each other so well.59. 填空题:The __________ is a famous site for ancient ruins in Greece. (雅典)60. 选择题:What is the main ingredient in ice cream?A. SugarB. MilkC. CreamD. Fruit答案:B61. 选择题:What do we call the act of gathering information?A. ResearchingB. CollectingC. StudyingD. Investigating62. 选择题:What do you call a story that explains how things came to be?A. LegendB. MythC. FableD. Tale答案:B63. 听力题:The dog is ______ (playing) with its owner.64. 选择题:Where does the President of the United States live?a. The White Houseb. The Capitolc. The Pentagond. The Courthouse答案:a65. 填空题:My sister is talented at ____.66. 填空题:The __________ (史前时期) gives insight into early human life.67. 选择题:What do we call the force that pulls objects toward the Earth?A. MagnetismB. GravityC. FrictionD. Inertia答案: B68. 选择题:Which month comes after January?A. FebruaryB. MarchC. AprilD. May69. 填空题:The skunk's spray is a powerful ________________ (防御).70. 填空题:My brother loves to play __________. (羽毛球)71. 填空题:The ________ (温暖气候) allows for diverse plants.72. 听力题:The process of chromatography separates mixtures based on _____.73. 填空题:I like to play ________ (拼图).74. 填空题:I enjoy playing ______ (棋类游戏) with my friends. It challenges our minds and is lots of fun.75. 听力题:The cat sleeps on a _____.76. 听力题:A strong base has a pH value that is ________ than .77. 选择题:What is the name of the famous American singer known for "Billie Jean"?A. Michael JacksonB. PrinceC. Elvis PresleyD. Justin Timberlake答案:A78. 填空题:I love to _____ (visit) botanical gardens.79. 填空题:The ancient Greeks believed in myths and _____.80. 听力题:I have a _____ (feather) from a bird.81. 听力题:A ____ is a playful creature that loves to chase butterflies.82. 选择题:What do we use to write on paper?A. BrushB. PencilC. SpoonD. Fork答案:B83. 填空题:The food smells _______ (很好吃).84. 填空题:The ant carries food back to its _______ (巢).85. 填空题:In ancient Rome, the Senate was a governing __________. (机构)86. 选择题:What is the name of the famous American holiday celebrated on the last Thursday in November?A. Independence DayB. ThanksgivingC. HalloweenD. Christmas答案: B. Thanksgiving87. 听力题:The process of changing a liquid to a gas is called __________.88. 填空题:The capital city of Iceland is _____.89. 选择题:What do you call a person who repairs watches?A. BakerB. JewelerC. MechanicD. Carpenter答案: B90. 选择题:What is the color of the sky on a clear day?A. GreenB. BlueC. YellowD. Black答案:B91. 填空题:My brother enjoys playing __________ (棋类游戏) with me.92. 听力题:A chemical reaction that occurs at room temperature is called a ______ reaction.93. 选择题:What do we call the process of removing the outer layer of a fruit?A. PeelingB. SlicingC. ChoppingD. Dicing答案:A94. 选择题:What do we call the study of the human body?A. AnatomyB. BiologyC. ChemistryD. Physiology答案:A95. 填空题:The _______ (猴子) eats bananas and berries.96. 选择题:How do you say "hello" in Spanish?A. BonjourB. HalloC. HolaD. Ciao答案:C97. 选择题:What do we call the act of telling someone what to do?A. AdvisingB. DirectingC. InstructingD. Commanding98. 选择题:What do you call the study of weather?A. GeographyB. MeteorologyC. ClimatologyD. Astronomy答案:B99. 选择题:Which of these is a season?A. JanuaryB. SummerC. TuesdayD. Breakfast答案: B100. 选择题:What is the name of the famous American singer known for her hit song "Respect"?A. Aretha FranklinB. Diana RossC. Tina TurnerD. Whitney Houston答案: A. Aretha Franklin。
2022年考研考博-考博英语-广东工业大学考试全真模拟易错、难点剖析B卷(带答案)一.综合题(共15题)1.单选题The Apple Project, code-named “Titan”, employed several hundred people working a few miles from Apple’s headquarters in Cupertino, and()auto industry experts.问题1选项A.allowedB.sponsoredC.gatheredD.recruited【答案】D【解析】考查动词词义辨析。
A选项allowed表示“允许,承认,接受”,B选项sponsored表示“赞助,发起,筹款”,C选项gathered表示“聚集,集中”,D选项recruited表示“招聘,雇佣,招募”。
分析句子结构可知,空缺处缺少部分为句子谓语动词。
由前文关键信息“employed several hundred people”可知,后文也应表示“招聘了一些自动化专家”,因此本题正确答案为D选项。
2.单选题Online services that provide()lovers saw a rise in popularity before the Valentine’s Day, which is celebrated every year on Feb 14.问题1选项A.humbleB.nobleC.radicalD.virtual【答案】D【解析】考查形容词词义辨析。
A选项humble表示“谦逊的,简陋的”,B选项noble表示“高贵的,宏伟的”,C选项radical表示“激进的,根本的,彻底的”,D选项virtual表示“事实上的,(计算机仿真)虚拟的”。
由句意可知,情人节前,网上提供()情侣的服务日渐增多。
由此可知,只有D选项最符合原文句意,virtual lover表示“虚拟情侣”。
核磁共振英语词汇英文回答:Nuclear magnetic resonance (NMR) is a powerfulanalytical tool that utilizes magnetic fields and radio waves to investigate the properties of atoms and molecules. It offers a non-destructive and versatile technique for characterizing materials at the atomic and molecular level. NMR has various applications across multiple scientific disciplines, including chemistry, physics, biology, and medicine.The basic principle of NMR involves the interaction between atomic nuclei with a magnetic field. Certain nuclei, such as 1H (proton), 13C, 15N, and 31P, possess anintrinsic magnetic moment due to their nuclear spin. When placed in a magnetic field, these nuclei align with or against the field, resulting in two distinct energy states. By applying radio waves to the sample at specific frequencies, it is possible to induce transitions betweenthese energy states.The absorption of radio waves by the nuclei leads to the resonance phenomenon, which forms the basis of NMR. The resonant frequency for a particular nucleus depends on its chemical environment, including the electron density and surrounding atoms. By analyzing the resonance frequencies and patterns, NMR provides detailed information about the structure, dynamics, and interactions of molecules.NMR spectroscopy is a widely used technique for identifying and quantifying different atoms and functional groups within molecules. It plays a crucial role in determining the molecular structure of organic and inorganic compounds, as well as studying chemical reactions and reaction mechanisms. NMR also finds applications in drug discovery and development, protein structure determination, and metabolomics.In medical imaging, NMR is employed as a non-invasive tool for obtaining detailed anatomical and functional information about the human body. Magnetic resonanceimaging (MRI) utilizes NMR techniques to create high-resolution images of organs, tissues, and blood vessels. MRI is particularly valuable for diagnosing and monitoring a wide range of medical conditions, including brain disorders, cardiovascular diseases, and musculoskeletal injuries.NMR also has applications in other fields, such as materials science, polymer characterization, and geological studies. It is a versatile technique that provides valuable insights into the structure, dynamics, and properties of various materials and systems.In summary, nuclear magnetic resonance (NMR) is a powerful analytical tool that offers a non-destructive and versatile approach for investigating the properties of atoms and molecules. Its applications span multiple scientific disciplines, including chemistry, physics, biology, and medicine, providing insights into molecular structure, dynamics, and interactions.中文回答:核磁共振(NMR)是一种强大的分析工具,利用磁场和射频波来研究原子和分子的性质。
Investigating the Effect of Aging onMaterialsIntroductionMaterials are essential for the development of modern society, they provide us with the necessary tools to build our buildings, create our vehicles and develop new technologies. But materials are not invincible, they can degrade over time due to several factors, including exposure to the environment, stress, and aging. Therefore, it is important to investigate the effect of aging on materials to better understand how they will perform over time and ensure their longevity.What is aging?Aging is a natural process that affects all materials, including metals, polymers, ceramics, and composites. It can be defined as the gradual deterioration of material properties due to various mechanisms such as chemical reactions, physical processes like diffusion, and structural changes on the atomic and molecular levels.The aging process is influenced by several factors, including temperature, humidity, exposure to UV radiation, and other environmental factors. Additionally, mechanical and physical stresses can also cause materials to age more quickly.The Effects of Aging on MaterialsAging can affect materials in several ways. One of the most significant effects is the degradation of mechanical properties, including strength, ductility, and toughness. Aging can cause microstructural changes that affect the material's ability to withstand stress and deformation.For example, metals can age due to corrosion, which can cause cracks and other defects that weaken the material's strength. Polymers can also undergo aging through oxidation, which can result in cracking, embrittlement, and loss of strength.Aging can also affect a material's thermal and electrical properties. For example, thermal conductivity may decrease due to the accumulation of impurities or changes in the microstructure. Additionally, aging can cause materials to become less electrically conductive.Methods of Investigating AgingThere are several methods for investigating the effect of aging on materials, including field experiments, laboratory testing, and simulation.Field experiments involve monitoring the performance of materials in real-world environments over a long period of time. This method is useful for investigating the effects of aging on materials in actual service conditions.Laboratory testing involves exposing materials to specific environmental conditions, such as temperature, humidity, and UV radiation, and monitoring their properties over time. This method is useful for simulating the effects of aging on materials in controlled conditions.Simulation involves predicting the aging behavior of materials using computer models. This method is useful for investigating the effect of aging on materials that are difficult or expensive to test in the laboratory or field.ConclusionThe effect of aging on materials is an important area of research that has implications for many industries. Understanding how materials age can help to develop more durable and reliable materials, which can enhance the safety and performance of critical infrastructure and other applications where materials are used. Methods of investigating the effect of aging on materials are diverse, and a combination of laboratory testing, field experiments, and simulation is often used to gain a comprehensive understanding of the aging process.。
关于公园的研究生英语作文Parks are an integral part of the urban landscape providing a much-needed respite from the hustle and bustle of city life. They offer a range of benefits to individuals and communities alike serving as hubs for recreation physical activity and social interaction. As a research topic parks present a rich area of exploration for graduate students interested in understanding the multifaceted role they play in shaping the built environment and enhancing quality of life.One key area of research in this domain is the environmental impact of parks. Parks serve as green oases in otherwise concrete jungles helping to mitigate the urban heat island effect and improve air quality through the absorption of carbon dioxide and release of oxygen by trees and other vegetation. Studies can examine the specific cooling effects of different park typologies and landscaping elements as well as quantify the air purification benefits afforded by urban greenspaces. This data can inform urban planning decisions to strategically locate and design parks to maximize their environmental services.Parks also play a crucial role in promoting physical activity and public health. Access to recreational facilities and green spaces has been linked to higher levels of physical activity among both children and adults. Research can investigate patterns of park usage analyzing who uses parks how often and for what purposes. This can shed light on barriers to park access and utilization particularly among underserved communities. Scholars can also explore the relationship between park proximity amenities programming and physical activity outcomes to identify best practices for park design and management that encourage active lifestyles.Beyond physical health parks also contribute to psychological wellbeing. Spending time in nature has been shown to reduce stress improve mood and enhance cognitive function. Parks provide opportunities for social interaction which is vital for combating loneliness and building a sense of community. Graduate students can conduct qualitative studies to understand the lived experiences of park users and the personal benefits they derive. They can also examine how factors like park size accessibility and programming influence perceptions of safety and comfort which are key determinants of park visitation.The economic value of parks is another important area of inquiry. Parks can increase nearby property values generate tourism revenue and produce cost savings for municipalities by reducing the need forexpensive stormwater management infrastructure. Researchers can assess the direct and indirect financial impacts of parks using techniques like hedonic pricing analysis and cost-benefit analysis. This information can strengthen the case for public investment in high-quality parks and greenspaces.Parks also have important social equity implications. Access to parks and green spaces is not equally distributed with underserved and marginalized communities often having less proximate and well-maintained parks. Research can investigate patterns of park provision across neighborhoods analyze barriers to access for diverse user groups and evaluate strategies for ensuring parks are equitably distributed and responsive to community needs. This work is crucial for promoting environmental justice and enhancing livability for all residents.Finally parks are dynamic spaces that evolve over time in response to shifting sociocultural and economic conditions. Graduate students can explore the historical development of parks studying how design priorities and usage patterns have changed. They can also examine contemporary trends and challenges facing park management such as the impacts of climate change, the role of public-private partnerships, and the incorporation of new recreational technologies. This historical and contemporary analysis can inform future planning to ensure parks continue meeting the needs of diverse communities.In conclusion the study of parks represents a rich and multifaceted area of research for graduate students. By investigating the environmental health social and economic impacts of parks scholars can generate valuable insights to guide more sustainable and equitable approaches to urban greenspace provision. Whether examining specific design features programming strategies or system-wide policies the research findings can ultimately improve quality of life for city residents of all backgrounds.。
a r X i v :a s t r o -p h /0703371v 2 9 J a n 2008D RAFT VERSION F EBRUARY 4,2008Preprint typeset using L A T E X style emulateapj v.10/09/06INVESTIGATING THE NATURE OF ABSORPTION LINES IN THE CHANDRA X-RAY SPECTRA OF THE NEUTRONSTAR BINARY 4U 1820−30E.M.C ACKETT 1,2,J.M.M ILLER 1,J.R AYMOND 3,J.H OMAN 4,M.VAN DER K LIS 5,M.M ÉNDEZ 5,6,7,D.S TEEGHS 3,R.W IJNANDS 5Draft version February 4,2008ABSTRACTWe use four Chandra gratings spectra of the neutron star low-mass X-ray binary 4U 1820−30to better understand the nature of certain X-ray absorption lines in X-ray binaries,including the Ne II ,Ne III ,Ne IX ,O VII ,and O VIII lines.The equivalent widths of the lines are generally consistent between the observations,as expected if these lines originate in the hot interstellar medium.No evidence was found that the lines were blueshifted,again supporting the interstellar medium origin,though this may be due to poor statistics.There is apparent variability in the O VIII Ly αline equivalent width providing some evidence that at least some of the O VIII absorption arises within the system.However,the significance is marginal (2.4-σ),and the lack of variation in the other lines casts some doubt on the reality of the variability.From calculating the equivalent hydrogen column densities for a range of Doppler parameters,we find they are consistent with the interstellar origin of the lines.Additionally we fit the spectra with photoionization models for locally absorbing material,and find that they can reproduce the spectrum well,but only when there is an extremely low filling factor.We conclude that both the ISM and local absorption remain possible for the origin of the lines,but that more sensitive observations are needed to search for low-level variability.Subject headings:accretion,accretion disks —stars:neutron —X-rays:individual (4U 1820−30)—X-rays:binaries —X-rays:ISM1.INTRODUCTIONHigh-resolution X-ray spectroscopy from Chandra and XMM-Newton allows for the study of absorption and emis-sion lines in Galactic X-ray binaries.While emission lines are clearly associated with the sources themselves (e.g.,Cottam et al.2001a,b;Schulz et al.2001),that is not always the case for absorption lines.In some systems,the absorp-tion lines are also clearly associated with the source,as they are observed to be variable and/or blueshifted (e.g.,Lee et al.2002;Parmar et al.2002;Ueda et al.2004;Boirin et al.2005;Díaz Trigo et al.2006;Miller et al.2006a,b).However,in other sources the lines are interpreted as being associated with absorption by the hot ionized interstellar medium,which is thought to be present in the disk and halo of the galaxy,with temperatures around 106K (e.g.,Futamoto et al.2004;Yao &Wang 2005;Juett et al.2006,and references therein).From studies of the absorption lines in the black hole X-ray binary GRO J1655−40,the plethora of highly-ionized lines that are detected are all seen to be blueshifted –ev-idence for a mass outflow into our line of sight,presum-ably from the accretion disk.In fact,detailed modeling of the lines in this system suggest that magnetic fields may be the force driving the wind (Miller et al.2006a).OtherElectronic address:ecackett@1Department of Astronomy,University of Michigan,500Church St,Ann Arbor,MI 48109-1042,USA2Dean McLaughlin Postdoctoral Fellow3Harvard-Smithsonian Center for Astrophysics,60Garden Street,Cam-bridge,MA 02138,USA4MIT Kavli Institute for Astrophysics and Space Research,MIT,70Vas-sar Street,Cambridge,MA 02139-43075Astronomical Institute ‘Anton Pannekoek’,University of Amsterdam,Kruislaan 403,1098SJ,Amsterdam,the Netherlands6SRON -Netherlands Institute for Space Research,Sorbonnelaan 2,3584CA Utrecht,the Netherlands7Astronomical Institute,University of Utrecht,PO Box 80000,3508TA Utrecht,The Netherlandsblack hole systems also show evidence for highly-ionized out-flows such as H 1743−322,GX 339−4and GRS 1915+105(Miller et al.2006b,2004;Lee et al.2002).Disk winds are also observed from the accretion disks around supermassive black holes in Active Galactic Nuclei (e.g.Crenshaw et al.1999;Kaastra et al.2000;Kaspi et al.2000).Several neutron star low-mass X-ray binaries also display clear evidence for absorption local to the source.For ex-ample,GX 13+1shows blueshifted absorption lines indicat-ing an outflow with a velocity of ∼400km s −1(Ueda et al.2004).Moreover,in the X-ray dipping sources,strong absorp-tion lines are observed as these objects are inclined close to the orbital plane (e.g.,Sidoli et al.2001;Parmar et al.2002;Boirin et al.2005;Church et al.2005;Díaz Trigo et al.2006).On the other hand,the nature of the absorption lines ob-served in many other neutron star X-ray binaries is less clear -the lines are weaker and there is no evidence of signifi-cant blueshifts,supporting the interpretation that these lines are due to the interstellar medium (e.g.,Yao &Wang 2005;Juett et al.2006).As part of the Chandra HETGS Z/Atoll Spectroscopic Sur-vey (CHAZSS)we have obtained sensitive observations of 6neutron star low-mass X-ray binaries at 2separate epochs us-ing the Chandra high energy transmission grating spectrom-eter (HETGS).The multiple epochs allow for a search for variability in the absorption lines present in these systems;this is key for learning about the nature of the absorption lines.In this paper,we present the observations of the sys-tem 4U 1820−30from this survey.Tight limits can be set on the size of any absorbing region associated with a binary if the system is ultra-compact in nature.Therefore,the ultra-compact nature of 4U 1820−30(Stella,Priedhorsky,&White 1987)makes it a particularly interesting source to study ab-sorption lines.2Cackett et al.2.PREVIOUS CHANDRA OBSERV ATIONS OF4U1820−304U1820−30is an accreting neutron star low mass X-ray binary in the globular cluster NGC6624,which has a well determined distance(7.6±0.4kpc Kuulkers et al.2003) and reddening(E(B-V)=0.32±0.03Kuulkers et al.2003; Bohlin et al.1978).This reddening is consistent with the to-tal HI column density of our Galaxy in this direction deter-mined from21cm radio observations,N H=1.5×1021cm−2 (Dickey&Lockman1990).We adopt the above column den-sity throughout this paper.Absorption lines and edges in the X-ray spectrum of this source have been studied previously by Futamoto et al. (2004),Yao&Wang(2005)and Yao&Wang(2006)using an LETG/HRC Chandra observation(ObsId98),and by Juett et al.(2004),Yao&Wang(2005),Juett et al.(2006)and Yao&Wang(2006)using HETG/ACIS Chandra observa-tions(ObsIds1021and1022).A summary of the Chandra observations of this source is given in Table1.We briefly summarize the main results of these previous studies below. Futamoto et al.(2004)clearly detect the O VII Heα,O VIII Lyα,and Ne IX Heαabsorption lines in the LETG spectrum, and put upper limits on the O VII Heβline.From their curve of growth analysis and photoionization modeling,they deduce that all oxygen will be fully photoionized if the absorbing col-umn is located close to the binary system,and therefore at-tribute these lines to hot gas in the ISM.However,we note that they make two tacit assumptions-that thefilling factor of the gas is1,and that all the absorption arises from the same gas.The studies by Juett et al.(2004)and Juett et al.(2006)are concerned with the absorption edges from oxygen,neon and iron,comparing the spectra of a number of X-ray binaries.In Juett et al.(2004)the structure around the oxygen edge in7 X-ray binaries is studied,looking at the O I,O II,and O III absorption lines in that region.The edge and these low ion-ization lines are attributable to ISM absorption.In Juett et al. (2006)the neon and iron L edges are studied,and the nature of the neon absorption lines discussed.These authors come to the conclusion that the neon lines in the low-mass X-ray binaries studied are consistent with predictions for the ISM, except for the Ne IX line detected in the black hole X-ray bi-nary GX339−4Miller et al.(2004)which shows a column density significantly higher than predicted for the ISM,con-firming that the largest contribution to this line(in this source, at least)is from local absorption.From a study of10low-mass X-ray binaries,Yao&Wang (2005)find that the detected Ne IX,O VII and O VIII absorp-tion lines are consistent with the hot ISM origin.Yao&Wang (2006)focuses specifically on4U1820−30,discussing the implications of the Ne and O abundance in the ISM from the absorption lines/edges in the Chandra observations.3.OBSERV ATIONS AND DATA REDUCTIONAll the previous observations discussed above suffer from pileup,where a high count rate leads to more than one photon arriving at a pixel per read out.This affects the shape of the spectrum,typically making it harder as the sum of the ener-gies of the multiple photons that arrived between each read-out is detected as one count.It is unclear how pileup affects the measurement of absorption lines.It likely modifies the continuum level and shape,which would in turn change any measured equivalent widths(which depends on the continuum flux across the line).Currently,there is no unambiguous way to model pileup in Chandra gratings spectra.To minimize pileup we operated Chandra with the High Energy Trans-mission Grating Spectrometer in continuous clocking mode to significantly increase the temporal resolution.Continuous clocking mode allows milli-second timing at the expense of one dimension of spatial information.As part of CHAZSS,4U1820−30was observed twice with Chandra for approximately25ksec each time,first on2006 Aug12(ObsId6633),and later on2006Oct20(ObsId 6634).The HETGS-dispersed spectrum was read-out with the ACIS-S array operating in continuous-clocking mode.We reduced these data using CIAO version3.3.0.1and follow-ing the standard analysis ing the tgextract tool spectra the+1and-1order were extracted at the nominal in-strument resolution for both the high-energy grating(HEG) and the medium-energy grating(MEG).Using the standard redistribution matrixfiles(RMFs)from the CALDB,the an-cillary responsefiles(ARFs)were generated using the fullgarf script.We carefully inspected the MEG+1and-1orders to confirm there was no wavelength shift between the two or-ders.The spectra and ARFs were then added together us-ing the add_grating_spectra,giving afirst-order spectrum for the MEG.Similarly,we created afirst-order spectrum for the HEG.In addition to analyzing these two new Chandra observa-tions,we also re-analyze the two previous Chandra HETGS observations of4U1820−30(ObsId1021&1022)to allow for a search for variability in the absorption lines.These two datasets were not operated in continuous-clocking mode,and suffer from pile-up.We reduce the data following the stan-dard analysis threads,extracting the spectra and ARFs using the same method described above.For consistency,we only analysis the HETGS observations here and not the LETGS observation which has a lower spectral resolution.4.ANALYSIS AND RESULTS4.1.Absorption linesWhen searching for absorption lines,we use only the MEG spectra,as the MEG has a higher effective area over the re-gion of interest compared to the HEG.We inspected the spec-tra over2Åsegments from2Åto24Åusing the ISIS spectral fitting package.In each segment,wefitted a simple power-law(modified,where appropriate,by an absorption edge due to neutral elements in the ISM).Within each segment,we searched for any significant absorption lines present.Wefit-ted a Gaussian to the detected absorption lines whose central wavelength,width,and normalization were all allowed to be free parameters.The equivalent width of the line was deter-mined from thefitted Gaussian.For line identifications we use Verner,Verner,&Ferland(1996)as a reference.How-ever,for Ne II and Ne III we use the wavelengths determined by Juett et al.(2006).Theyfind the weighted mean of the central wavelengths of these lines measured in multiple X-ray binaries.The wavelengths for these lines from different sources are seen to consistent with each other,and are all sys-tematically shifted by a small amount(∼20mÅ)from the the-oretical value determined by Behar&Netzer(2002),though within their stated errors.The Juett et al.(2006)values are known most accurately,thus we use them throughout the rest of the paper.8http:///ciao/threadsX-ray absorption lines in4U1820−303In the two new Chandra observations,we detect several X-ray absorption lines.We define a detected line as one for whichfits with a Gaussian give an equivalent width that excludes zero at more than the2σlevel of confidence(note that we are being conservative by using the significance with which we can measure the equivalent width as the significance of the detection).In increasing wavelength(theoretical/best observational wavelengths are given in brackets),the detected lines are:Ne IX(13.447Å),Ne III(14.508Å),Ne II(14.608Å),O VII(18.629Å),O VIII(18.967Å).All these absorption lines are detected in both observations,however,some were not detected in the previous Chandra observations,likely due to the lower sensitivity of those shorter observations.Whilst the O I absorption line at∼23.5Åwas detected in all obser-vations,we have not attempted tofit this line due to the com-plicated structure around this region due to multiple oxygen lines.The structure in this region has been studied in detail previously by Juett et al.(2004).The interstellar absorption at this wavelength also significantly increases the noise in the data,therefore the LETG observation of4U1820−30previ-ously studied present the best available dataset for analysis of this region.We also note that the O VII line at∼21.6Åwas not detected in any of these observations,due to the low signal-to-noise in that region.Again,the previous LETG observation of4U1820−30gives the best detection of this line.In cases where an absorption line had been detected in one of the other observations,but not in the observation we were studying,a95%confidence level upper limit for the lineflux and equivalent width was determined.This was achieved by fixing the line wavelength at the theoretical value,fixing the width at a value smaller than the instrument resolution(as would be the case if the line was unresolved),and then in-creasing the lineflux until theχ2value for thefit increased by2.7.We justifyfixing the width smaller than the instru-ment resolution as for the MEG,the resolution corresponds to a FWHM of∼350km s−1at18.967Å,and higher at shorter wavelengths.This is significantly higher than the expected thermal broadening in the ISM.Table2gives the line proper-ties determined from the spectralfitting.In Fig.1we show the absorption lines detected in the two new Chandra obser-vations.As Ne IX is detected at13.447Åone should also expect to find additional Ne IX lines at11.547Åand11.000Å.How-ever,we do not clearly detect these lines in any of the obser-vations.If the line is not saturated,the ratio of the equiva-lent widths should follow the ratio of the oscillator strengths times the ratio of the wavelengths squared.The mean value of the equivalent width of the Ne IX(13.447Å)line is approxi-mately5mÅ.From the oscillator strengths,this would put the expected equivalent widths for the Ne IX lines at11.547Åand 11.000Åto be0.8mÅand0.3mÅ,respectively.In Ob-sId6633,we note that there may be a weak absorption line present atλ=11.550±0.007Å,with an equivalent width of EW=1.8±0.9mÅ,though this is only a2σdetection. This measured equivalent width is consistent with what is pre-dicted from the oscillator strengths.The line at11.000Åis not detected,and we determine the95%confidence level up-per limit to be1.7mÅ-the line would be too weak to de-tect given the noise in the data.In ObsId6634these Ne IX lines are not detected,and wefind the upper limits on the equivalent width for the lines at11.547Åand11.000Åto be1.6mÅand1.3mÅrespectively,consistent with what would be expected from the oscillator strengths.We do not determine upper limits for these lines from the ObsId1021 and1022datasets,as they are substantially less sensitive, and therefore the lines could not be detected at the predicted equivalent widths.While the upper limits do not rule out that the line is saturated,we cannot be conclusive.Similarly,we try to determine whether the O VIII lines are saturated by determining limits on the O VIII Lyβline at 16.006Å.Fitting a Gaussian,with central wavelengthfixed at16.006Åto ObsId6633and6634we measure equivalent widths of3.0±1.5mÅ,and3.4±2.8mÅrespectively.This gives the ratio of the equivalent widths of the O VIII Lyβto Lyαas0.47±0.32and0.18±0.16for ObsId6633and6634 respectively.For comparison,if the lines are not saturated we would expect this ratio to be0.14given the oscillator strengths and wavelengths.The measured value from ObsId6634is clearly consistent with this ratio,and in ObsId6633the ratio is not significantly different.Therefore the O VIII lines are not highly saturated.Another check on saturation can be performed using the measured equivalent width of the O VII Lyαline(measured in previous Chandra LETG observations by Futamoto et al. 2004)and comparing it with the weighted average of the O VII Lyβequivalent widths measured here.Wefind that the ratio of O VII Lyαequivalent width to Lyβequivalent width is5.5±2.2.From the line wavelengths and oscillator strengths(taken from Verner et al.1996),the expected ratio in the non-saturated regime is6.4,consistent the ratio from the observed equivalent widths,suggesting that the O VII lines are not highly saturated.4.2.Column DensitiesFrom the measured equivalent widths of the lines,we de-termine the column densities.Firstly we assume that the lines are not saturated and on the linear part of the curve of growth.Under this assumption,the column density and equivalent width are associated via Wλ=(πe2/M e c2)N jλ2f i j= 8.85×10−13N jλ2f i j,where Wλis the equivalent width(in cm),N j is the column density of a given species,λis the line wavelength(in cm)and f i j is the oscillator strength(Spitzer 1978).However,as we cannot conclusively determine whether the lines are saturated,we also calculate the column density for a range of Doppler parameters,b.For a lower limit for the line broadening,we estimate the FWHM of the Galactic rotation in the direction of the source from a Besancon model of the Galaxy to be50km s−1.We also evaluate the column densities assuming b=100km s−1and b=200km s−1.The latter being an upper limit on the width of O VI emission lines from UV observations with FUSE(Otte&Dixon2006).Given the os-cillator strength,line wavelength,observed equivalent width and assumed Doppler parameter,we determine the required column density for each line in ObsIds6633and6634,us-ing the curve of growth equations in Spitzer(1978).For the blended O VIIIfine structure components we compute the col-umn densities numerically.Table3gives the calculated col-umn densities.In order to test whether these column densities are consis-tent with the interstellar medium,we converted the column density for each species into an equivalent hydrogen column density.To do this we require the ionic fraction for each ion, which for collisional ionization(the mechanism present in the ISM)depends on the temperature.The low ionization lines4Cackett et al.(Ne II and Ne III)will be in a lower temperature gas than the higher ionization lines(Ne IX,O VII,O VIII),thus we esti-mated the temperatures paring the observed ratio of Ne II/Ne III with the ratio of the ionic fractions for those ions at a range of temperatures(as calculated for colli-sional ionization by Mazzotta et al.1998),we determined the best-fitting temperature of the gas.Given that temperature, the ionic fractions at that temperature and the ISM abundances from Wilms et al.(2000)we converted the ionic column den-sities into equivalent hydrogen column densities(see Table3). We found the temperatures for the Ne II and Ne III gas to be in the range(4.8−5.2)×104K.Similarly for Ne IX,O VII,O VIII we determined a tem-perature from the ratios of O VII/O VIII and O VII/Ne IX(as-suming Ne/O from Wilms et al.2000)compared to the ionic fractions from Mazzotta et al.(1998),and then used the esti-mated ionic fractions and abundances to convert to equivalent hydrogen column densities(see Table3).The temperatures we determine for this gas is in the range(1.3−2.0)×106K, consistent with the hot phase of the ISM.The equivalent hydrogen column densities that we estimate are all consistent with having a lower column density than the column to the source as seen in H I(1.5×1021cm−1, Dickey&Lockman1990).4.3.Photoionization modelingIn order to assess the possibility of the observed absorp-tion lines originating from local absorption in the X-ray bi-nary system(rather than the ISM)we used the photoioniza-tion code XSTAR v2.1(Kallman&Bautista2001)to model the observed spectrum in ObsID6633and6634.For the in-put ionizing spectrum we use the unabsorbed source spectra for each observation,scaled to the observed luminosities(see section4.4for details on determining the sourceflux,we as-sume d=7.6kpc giving0.5-10keV luminosities of5.7×1037 and8.1×1037erg s−1for ObsID6633and6634,respectively). For each observation we then created a grid of absorption line models allowing the column density and ionization parame-ter,ξ=L/nR2,to vary.In our models we assume solar abun-dances,a covering fraction of0.5,and turbulent velocities of 200km s−1.From these grids of models we thenfit the ob-served spectra(again using ISIS)from13Åto20Åwith a power-law(with Galactic absorptionfixed at1.5×1021cm−1) convolved with the absorption line models calculated from XSTAR.This allows us to determine under what conditions the observed spectrum can be reproduced by photoionization of local absorbing gas.In Fig.2we show the best-fitting models from the pho-toionization modeling.Wefind that for both observations,the observed Ne IX,O VII,O VIII lines can be reproduced well withχ2ν=1.13for ObsID6633,andχ2ν=1.15for ObsID 6634.Note that the Ne II and Ne III lines are not included in the code,and thus are not reproduced.For ObsID6633wefind the bestfit with N H=(6.1±1.5)×1019cm−2and logξ=1.36±0.05(whereξ=L/nR2).For ObsID6634wefind the bestfit with N H=(7.6±1.3)×1019 cm−2and logξ=1.34±0.03.Given that the binary separation for4U1820−30is∼1010cm(Stella et al.1987),with the ionization parameters wefind the gas density would have to be n=2.5×1016cm−3for ObsID6633and n=4×1016cm−3 for ObsID6634for the largest plausible radius for absorbing gas within the system.The implies that thefilling factor,f, is extremely low with f=N H/nR=2.4×10−7for6633and f=1.9×10−7for6634.Since f scales with R,smaller radii within the system make the problem worse.It seems unlikely that the gas would be in a shell,as the filling factor would mean that the thickness of the shell would be very small(on the order of only tens of metres for gas within the system).Additionally it is also unlikely to be a shell covering the entire4πor else one would also observe emission lines.One possibility is that thermal instabilities produce small,dense structures,or alternatively there could be partial covering by larger blobs,which could be driven by a wind.Therefore,while it seems possible that locally pho-toionized material could account for the absorption,it does re-quire fairly extreme parameters.We note that Futamoto et al. (2004)use CLOUDY to run a numerical simulation for pre-vious observations of4U1820−30.These authors concluded that photoionized gas within the binary system could not re-produce the observed line column densities.In summary,the ISM may be the more likely source of the absorption lines,but our models demonstrate that photoionization cannot be ruled out,especially given the presence of variability.4.4.SourcefluxIn order to compare absorption line properties with the source properties,we determine the sourceflux from the best fitting continuum model to the HEG spectrum.For this broad-band spectralfitting we use XSPEC(Arnaud1996).We do notfit the MEG and HEG simultaneously due to the signifi-cant pileup in thefirst two observations,where the observa-tions were not operated in continuous clocking mode.As the MEG has a larger effective area than the HEG at low ener-gies(by about a factor of2)it is more substantially affected by pileup.This is clearly apparent when trying tofit a con-tinuum model to just the MEG spectra in these observations. There is an excess of counts at high energies and deficit at low energies,as expected by pileup.The HEG is much less affected,and thus we choose tofit to just the HEG1st order spectra.For consistency,we use this method forfitting to the new Chandra observations also,even though they do not suf-fer from pileup.We choose tofit an absorbed blackbody plus power-law model to the HEG spectra over the energy range1.2−8keV with the column density isfixed at the galactic value towards this globular cluster for all observations.Models to neu-tron star X-ray binary spectra can be degenerate(Lin et al. 2007),especially over a short energy range,such as covered by the HEG.The model we adopt isfiducial and reflects a physically-motivated scenario consisting of thermal and non-thermal emission.It allows us to characterize the sourceflux well because it provides a goodfit to the spectrum.Impor-tantly,it is a simple continuum model and so is easily repro-ducible,but,due to modeling degeneracies the specific pa-rameter values derived should be regarded with caution.The fitted spectral parameters are given in Table4.We determine the0.5-10keV sourceflux,by extending a dummy response to lower and higher energies.We deter-mine the uncertainty in theflux by propagating the errors on the individual parameters.The calculatedfluxes are given in Table4.We note that the uncertainties in thefluxes may be dominated by calibration uncertainties,and could be closer to around6%(the difference influx wefind betweenfitting to the MEG and HEG)than those we determine from spectral fitting.We check whether pileup alters the determinedfluxes sub-stantially by comparing the calculated sourcefluxes with theX-ray absorption lines in4U1820−3051-day average RXTE All-Sky Monitor(ASM)count rate for the day of each Chandra observation(see Tab.4).Compar-ing the sourceflux against the ASM count rate,they are seen to be correlated,with no large offsets(see Fig.3).To look for variability of the absorption lines between each epoch,in Fig.4we plot the measured equivalent width(or upper limit,if the line is not detected)for each observation vs the0.5-10keV unabsorbed sourceflux(see Table4).The er-rorbars indicate1σuncertainties in the equivalent width.The dashed lines indicates the weighted mean(weighted by the uncertainties)of the equivalent widths of the detected lines. Generally,the equivalent widths of the lines are consistent between the observations.However,we note that the O VIII line does seem to display variability,although the variability is not highly significant and does not appear to be correlated with the sourceflux(see Fig.4).The observed wavelength of the O VIII line is also found to be consistent with the theoret-ical wavelength and not blueshifted.We calculate theχ2value for afit of the equivalent widths for the O VIII line to their weighted mean to assess the sig-nificance of this variability.For the non-detection in ObsId 1021,we use the equivalent width determined fromfitting a Gaussianfixed at the wavelength of the line in the calcula-tion.This equivalent width is found to2.9±2.9mÅ.We get χ2=14.1(3degrees of freedom)whenfitting the equivalent widths to their weighted mean.For the hypothesis that the equivalent widths are constant,this corresponds to a proba-bility for achieving a higherχ2value of0.003.However,we note that we have searched5lines tofind variability of this level,and thus this increases the probability to0.015.This is equivalent to the line being variable at the2.4σlevel of confidence.Thus,while it is not a highly significant result, low-level variability cannot be ruled out for this line.In comparing equivalent width measurements from multi-ple epochs,it is important to consider whether any systematic effects can cause variability in the lines.Importantly,neither thefirst two observations(ObsId1021and1022)were oper-ated in continuous-clocking mode,and thus both are affected by pileup.It is not clear how pileup alters equivalent width measurements,though we note that as the O VII and O VIII lines are close together in wavelength they should be affected similarly.Any effect must be fairly small,as the O VIII line is seen to vary whereas the O VII is not.5.DISCUSSIONWe have analyzed four Chandra HETGS observations of the neutron star low-mass X-ray binary4U1820−30and de-tect a variety of absorption lines in the spectra.Thefirst two archival observations suffer from pile-up,and thus measure-ments of lines from these observations may not be robust. However,the two new observations presented here do not suf-fer from this problem and have an increased sensitivity com-pared to the previous observations,allowing for a significantly improved study of the absorption lines in this system.To investigate the nature of these lines,we compare the line equivalent widths between the observations.If the line is un-saturated and on the linear part of the curve of growth,then the equivalent width is a direct measure of the absorbing col-umn.If the equivalent width does not vary between observa-tions,this would therefore indicate that the absorbing column has remained unchanged between the observations,as would be expected for absorption lines associated with the ISM.The majority of the absorption lines present in4U1820−30are consistent with remaining constant between the observations,suggesting they are interstellar in origin.However,if the lines are saturated,then even if the column density changes signif-icantly(for instance in response to changes in the source)the equivalent width would remain more or less constant.Simi-larly,in the saturation regime even if the ionizingflux changes by a factor of2(as observed between ObsId6633or6634)the equivalent width and ion relative abundance fractions may not change by a similar amount.However,even though we do not observe theα−β−γsequence for each line,upper limits on β/αindicate that the lines are not highly saturated.Wefind that there may be a low level of variability(2.4-σsignificance)in the O VIII Lyαline,which may indicate it is associated with the source.If the absorption is local to the source,this variability could be,for example,due to changes in mass accretion rate leading to changes in mass outflow.If one naively assumes that the continuumflux traces the mass accretion rate one would therefore see correlated variability between the sourceflux and the line equivalent width.Alter-natively,if the properties of the absorbing column are approx-imately constant and the ionizingflux changes,the fraction of oxygen in O VIII should change,which could lead to corre-lated variability.However,there appears to be no such cor-relation observed(see Fig.4)though more observations are required to be conclusive.Additionally,if the gas in the system responds to changes in the ionizingflux more slowly than the inherent changes in the ionizingflux(i.e.if the recombination time is long),this would have the effect of greatly dampening the amplitude of variations seen in the absorption relative to the incidentflux. For O VIII originating within the system,the size of the ab-sorbing region is<1011cm.The column density we observe to be about1020cm−2,thus the density is n e∼109cm−3.The recombination rate coefficient for O VIII isα=1.5×10−12 cm3s−1at106K,so the recombination timescale=1/(n eα)∼700s.This is significantly shorter than the timescale be-tween the observations and thus should not be a factor.If the absorption lines were associated with a disk wind, then blueshifts would be expected.Wefind that the wave-length of the absorption lines are consistent with their rest wavelengths(after accounting for the absolute instrumental calibration uncertainty of0.05%),as expected for interstellar lines.However,we note that in the dipping X-ray binaries, absorption lines that are local to the source are not seen to be blueshifted and are thought to be associated with the accre-tion disk corona rather than an accretion disk wind.Similarly, here the lack of blueshifts could just be explained by absorp-tion from an accretion disk corona(Díaz Trigo et al.2006). To test both possible origins for the lines,wefirst calculated the equivalent hydrogen column densities(implied by the ob-served equivalent widths)for a variety of Doppler parameters, andfind that they are consistent with the interstellar origin for the lines.Additionally we perform photoionization model-ing of absorption by material local to the system.Wefind that photoionization can reproduce the observed spectra well. However,to do this requires a very lowfilling factor,but this could possibly be explained by absorption from dense blobs. We conclude that while the Ne II and Ne III lines are produced in the ISM,the origin of the Ne IX,O VII and O VIII lines re-mains unclear,with both the interstellar and local absorption remaining possible.The key to determining the origin of these lines may lie in variability,thus additional sensitive observa-tions of4U1820−30are needed to confirm variability in the O VIII line,and search for low-level variability in other lines.。