Supersolar metal abundances and the Broad Line Region of Narrow-line Seyfert 1 galaxies
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solar energy阅读理解what is the ma阅读理解。
Solar energy (power from the sun) is of many uses. In many pa rts of the world, people are building solar houses with large numbe rs of windows to collect the heat of the sun. Solar collectors can m ake hot water from sunlight. The rays of the sun heat water in a so lar collector, and the hot water goes into a storage tank (蓄水箱). People can use the hot water for washing or for heating their houses. In the future, people may use the rays of the sun to make electricity for their homes. They will use photovoltaic cells to make electricity from sunlight.The sun is an important "new" source of energy. It is less expe nsive than oil or nuclear energy. Furthermore, it does not cause po llution, and it is not as dangerous as nuclear power. Many people t hink that solar energy will be the answer to our future energy probl ems.1. What is the ma source of solar energy?A. The earth.B. Oil.C. The sun.D. Nuclear energy.2. A solar collector can ______.A. answer our future energy problemsB. make electricity from sunlightC. use hot water for washingD. make hot water from sunlight3. Solar energy may solve ______.A. water shortagesB. storage problemsC. future energy problemsD. future water problems4. People may use the hot water from a solar collector ______.A. for nuclear powerB. for washing and heatingC. to cause pollutionD. to change sunlight into electricity。
The Potential of Solar Energy to ReplaceFossil FuelsIn the modern era, the quest for sustainable and renewable energy sources has become paramount. Fossil fuels, once considered the backbone of the global energy sector, are now being questioned due to their environmental implications and finite nature. Solar energy, on the other hand, has emerged as a promising alternative, offering a clean, renewable, and abundant source of power. This essay explores the potential of solar energy to replace fossil fuels and the associated benefits and challenges.Solar energy is derived from the sun's radiation and converted into usable electricity through photovoltaic cells. Its primary advantage lies in its limitless supply, as the sun is expected to shine for billions of years. In contrast, fossil fuels such as coal, oil, and gas are non-renewable resources and are rapidly depleting. According to the International Energy Agency, global energy demand is projected to increase by more than 30% by 2040, further stressing the need for alternative energy sources.Solar energy also boasts significant environmental benefits. The combustion of fossil fuels releases greenhouse gases such as carbon dioxide, contributing to global warming and climate change. Solar energy, on the other hand, produces no emissions, making it a clean and environmentally friendly option. Additionally, solar panels require minimal water use and land space compared to fossil fuel-based power plants.Economically, solar energy has become increasingly competitive with fossil fuels. The cost of photovoltaic technology has decreased significantly in recent years, making it more affordable for both residential and commercial use. Governments worldwide are also offering incentives such as tax credits and feed-in tariffs to encourage the adoption of solar energy.Despite these advantages, solar energy faces some challenges that need to be addressed. One of the main challenges is the intermittency of solar radiation, which can vary depending on weather conditions and地理位置. To overcome this, energy storage systems such as batteries orpumped-hydro storage can be employed to store excess energy during sunny days and release it when needed.Another challenge is the upfront cost of installing solar panels, which can be prohibitive for some. However, with the decreasing cost of photovoltaic technology and the increasing availability of financing options, solar energy is becoming more accessible to a wider range of users.In conclusion, solar energy has the potential to replace fossil fuels as the primary source of energy in the future. Its limitless supply, cleanliness, and cost-competitiveness make it an attractive alternative. However, to fully harness the potential of solar energy, it is crucial to address the associated challenges such as intermittency and upfront costs. With continued research and innovation, solar energy could play a pivotal role in ensuring a sustainable and environmentally friendly energy future.**太阳能潜力:替代化石燃料的可行选择**在现代社会中,对可持续和可再生能源的追求变得至关重要。
广州沪教牛津版(2024版新教材)七年级英语上册Unit 5 Off to space单元测试卷时间:90分钟满分:100分一、语音(共10小题;每小题1分,满分10分)A. 找出与前面音标发音相同的单词。
1./ ɜː / A. doct or B. act or C. f ir st D. b a nana2./ ə / A. b ir d B. h ur t C. n er vous D. pict ureB. 找出下列每组划线部分发音不同的选项。
3.A. c a mera B. rel a tive C. probl e m D. exc e llent4.A. w or k B. nev er C. G er man D. n er vous5.A. wh ole B. wh om C. wh at D. wh ose6.A. h er B. h onest C. h ear D. h orseC. 从下列各组选项中找出重读音节位置与其他不同的一项。
7.A. excited B. able C. nervous D. camera8.A. ourselves B. pollute C. without D. picnic9.A. machine B. adult C. able D. magic10.A. return B. protect C. without D. garden二、语法选择。
(共15小题;每小题1分,满分15分)阅读下面两篇短文,按照句子结构的语法性和上下文连贯的要求,从11~25各题所给的A、B、C和D项中选出最佳选项,并在答题卡上将该项涂黑。
Sam lives in a big house in Tianhe District, Guangzhou. He works 11 at a university 12 weekdays. On Saturdays and Sundays he 13 go to work.At 14 weekend, Sam often does morning exercises at 7:30 a.m. and 15 tea in one of 16 restaurants near 17 home at 8:30 a.m. Then he usually spends two hours 18 in the library. In the afternoon, he 19 plays basketball or goes running in a park. He often has a big supper with three good friends at 6:30 p.m. When they are eating, he enjoys 20 with them 21 he wants to study 22 from others.After the meal, they often go along a river and look at the stars in the sky. And Sam is keenon 23 at night. He likes reading 24 . There 25 a book show two months later. He wants to buy some.11.A. hardly B. hard C. harder D. hardest12.A. in B. at C. on D. from13.A. does B. is C. isn’t D. doesn’t14.A. a B. an C. the D. /15.A. drink B. to drink C. drinks D. drank16.A. good B. better C. best D. the best17.A. he B. him C. his D. himself18.A. to read B. reads C. on reading D. reading19.A. some time B. some times C. sometimes D. sometime20.A. talk B. to talk C. talking D. talks21.A. or B. because C. if D. but22.A. a lot of B. a lots C. a lot D. lots of23.A. write B. writes C. to write D. writing24.A. something interesting B. interesting somethingC. anything interestingD. interesting anything25.A. is going to B. will be C. is going to have D. will have三、完形填空(共10小题;每小题1分,满分10分)阅读下面短文,掌握其大意,然后从26~35各题所给的A、B、C和D项中选出最佳选项,并在答题卡上将该项涂黑。
剑桥商务英语听说星系The Milky Way GalaxyThe Milky Way is the galaxy that contains our Solar System, with the Earth and Sun. This galaxy is a vast, spinning collection of stars, planets, dust and gas, held together by gravity. It is just one of hundreds of billions of galaxies in the observable universe.The Milky Way galaxy is estimated to contain 100-400 billion stars and have a diameter between 100,000 and 180,000 light-years. It is the second-largest galaxy in the Local Group, with the Andromeda Galaxy being larger. As with other spiral galaxies, the Milky Way has a central bulge surrounded by a rotating disk of gas, dust and stars. This disk is approximately 13 billion years old and contains population I and population II stars.The solar system is located about 25,000 to 28,000 light-years from the galactic center, on the inner edge of one of the spiral-shaped concentrations of gas and dust called the Orion Arm. The stars in the Milky Way appear to form several distinct components including the bulge, the disk, and the halo. These components are made of different types of stars, and differ in their ages and their chemicalabundances.The Milky Way galaxy is part of the Local Group, a group of more than 50 galaxies, including the Andromeda Galaxy and several dwarf galaxies. The Local Group in turn is part of the Virgo Supercluster, a giant structure of thousands of galaxies. The Milky Way and Andromeda Galaxy are moving towards each other and are expected to collide in about 4.5 billion years, although the likelihood of any actual collisions between the stars themselves is negligible.The Milky Way has several major arms that spiral from the galactic bulge, as well as minor spurs. The best known are the Perseus Arm and the Sagittarius Arm. The Sun and its solar system are located between two of these spiral arms, known as the Local Bubble. There are believed to be four major spiral arms, as well as several smaller segments of spiral arms.The nature of the Milky Way's bar and spiral structure is still a matter of active research, with the latest research contradicting the previous theories. The Milky Way may have a prominent central bar structure, and its shape may be best described as a barred spiral galaxy. The disk of the Milky Way has a diameter of about 100,000 light-years. The galactic halo is a spherical component of the galaxy that extends outward from the galactic disk, as far as 200,000 light-years from the galactic center.The disk of the Milky Way Galaxy is marked by the presence of a supermassive black hole known as Sagittarius A*, which is located at the very center of the Galaxy. This black hole has a mass four million times greater than the mass of the Sun. The Milky Way's bar is thought to be about 27,000 light-years long and may be made up of older red stars.The Milky Way is moving with respect to the cosmic microwave background radiation in the direction of the constellation Hydra with a speed of 552 ± 6 km/s. The Milky Way is a spiral galaxy that has undergone major mergers with several smaller galaxies in its distant past. This is evidenced by studies of the stellar halo, which contains globular clusters and streams of stars that were torn from those smaller galaxies.The Milky Way is estimated to contain 100–400 billion stars. Most stars are within the disk and bulge, while the galactic halo is sparsely populated with stars and globular clusters. A 2016 study by the Sloan Digital Sky Survey suggested that the number is likely to be close to the lower end of that estimate, at 100–140 billion stars.The Milky Way has several components: a disk, in which the Sun and its planetary system are located; a central bulge; and a halo of stars, globular clusters, and diffuse gas. The disk is the brightest part of theMilky Way, as seen from Earth. It has a spiral structure with dusty arms. The disk is about 100,000 light-years in diameter and about 13 billion years old. It contains the young and relatively bright population I stars, as well as intermediate-age and old stars of population II.The galactic bulge is a tightly packed group of mostly old stars in the center of the Milky Way. It is estimated to contain tens of billions of stars and has a diameter of about 10,000 light-years. The Milky Way's central bulge is shaped like a box or peanut. The galactic center, which lies within this bulge, is an extremely active region, with intense radio source known as Sagittarius A*, which is likely to be a supermassive black hole.The Milky Way's halo is a spherical component of the galaxy that extends outward from the galactic disk, as far as 200,000 light-years from the galactic center. It is relatively sparse, with only about one star per cubic parsec on average. The halo contains old population II stars, as well as extremely old globular clusters.The Milky Way's spiral structure is uncertain, and there is currently no consensus on the nature of the Milky Way's spiral arms. Different studies have led to different results, and it is unclear whether the Milky Way has two, four, or more spiral arms. The Milky Way's spiral structure is thought to be a major feature of its disk, and it may berelated to the generation of interstellar matter and star formation.The Milky Way's spiral arms are regions of the disk in which the density of stars, interstellar gas, and dust is slightly higher than average. The arms are thought to be density waves that spiral around the galactic center. As material enters an arm, the increased density causes the material to accumulate, thus causing star formation. As the material leaves the arm, star formation decreases.The Milky Way's spiral arms were first identified in the 1950s, when radio astronomers mapped the distribution of gas in the Milky Way and found that it was concentrated in spiral patterns. Since then, astronomers have used a variety of techniques to study the Milky Way's spiral structure, including observations of the distribution of young stars, star-forming regions, and interstellar gas and dust.One of the key challenges in studying the Milky Way's spiral structure is that we are located within the disk of the galaxy, which makes it difficult to get a clear view of the overall structure. Astronomers have had to rely on indirect methods, such as measuring the distances and motions of stars and gas clouds, to infer the shape and structure of the galaxy.Despite these challenges, our understanding of the Milky Way's spiral structure has advanced significantly in recent years, thanks tonew observations and more sophisticated modeling techniques. Ongoing research is continuing to shed light on the nature and evolution of the Milky Way's spiral arms, and the role they play in the overall structure and dynamics of the galaxy.。
超导合金英文作文英文:Superconducting alloys are materials that exhibit zero electrical resistance and perfect diamagnetism at low temperatures. They have various applications in fields such as power transmission, magnetic levitation, and superconducting magnets. One example of a superconducting alloy is Nb3Sn, which is composed of niobium and tin. This alloy has a critical temperature of around 18 K, which means it can superconduct at temperatures below this value.Superconducting alloys have several advantages over conventional conductors. Firstly, they can carry much higher currents without any energy loss due to resistance. This means they are much more efficient and can save a lot of energy. Secondly, they can produce much stronger magnetic fields, which is useful in applications such as MRI machines and particle accelerators. Finally, they can be used to create levitation systems, which can be used totransport objects without any friction.However, superconducting alloys also have some disadvantages. Firstly, they are expensive to produce and require specialized equipment and techniques. Secondly,they are very brittle and can easily break under mechanical stress. Finally, they require very low temperatures to operate, which can be difficult to achieve and maintain.Despite these challenges, superconducting alloys have many potential applications and are an active area of research. For example, researchers are working ondeveloping superconducting wires that can be used in power transmission, which could greatly improve the efficiency of the electrical grid. They are also working on developing superconducting magnets that can be used in fusion reactors, which could provide a clean and sustainable source of energy.中文:超导合金是一种在低温下表现出零电阻和完美的抗磁性的材料。
“PEP”2024年小学3年级上册英语第5单元寒假试卷[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:They are ___ their bikes. (riding)2、What shape has three sides?A. SquareB. TriangleC. CircleD. Rectangle答案: B3、填空题:My favorite character is __________ (超级英雄) because he is very brave.4、听力题:A physical change does not produce a new ______.5、听力题:The ______ is known for her motivational speeches.6、听力题:A saturated solution contains the maximum amount of ______.7、选择题:What is the largest planet in our solar system?A. EarthB. MarsC. JupiterD. Venus8、听力题:The ______ is the force that holds atoms together in a molecule.9、What is the name of the area around a star where conditions might be right for life?A. Goldilocks ZoneB. Habitable ZoneC. Life ZoneD. Safe Zone10、What is the main ingredient in sushi?A. NoodlesB. RiceC. BreadD. Potatoes答案:B11、听力题:The process of extracting metals from ores is called _______.12、What is the largest planet in our solar system?A. EarthB. JupiterC. SaturnD. Mars13、What is the main purpose of a compass?A. To measure distanceB. To find directionC. To show timeD. To calculate speed14、填空题:In ancient Rome, people used to watch _____ (gladiator) fights in the arena.15、填空题:I enjoy learning about different ______ (历史人物) and their contributions to society. It inspires me.16、选择题:What do we call a large body of water surrounded by land?A. LakeB. OceanC. SeaD. River17、填空题:A _____ (自然观察) can reveal many secrets of plant life.18、听力题:The __________ is a critical area for studying the impacts of climate change.19、听力题:The ______ grows in forests.20、听力题:The first space shuttle launch was in _______.21、听力题:A solar eclipse happens when the ______ passes between the Earth and the sun.22、填空题:I like to drink ______ (果汁) in the morning with my breakfast.23、Which of these is not a vegetable?A. CarrotB. TomatoC. BananaD. Spinach答案:C24、听力题:Salt is an example of a ______ formed from an acid and a base.25、填空题:I have a _____ (拼图) of a beautiful landscape that I enjoy completing.我有一个美丽风景的拼图,喜欢完成它。
地球化学资料1地球化学资料(1120101)第⼀章地球化学定义DefinitionB.И.韦尔纳茨基(1922):地球化学科学地研究地壳中的化学元素(chemical elements),即地壳的原⼦,在可能的范围内也研究整个地球的原⼦。
地球化学研究原⼦的历史、它们在时间和空间上的运动(movement)和分配(partitioning),以及它们在整个地球上的成因(origin)关系。
V.M.费尔斯曼(1922):地球化学研究地壳中化学元素---原⼦的历史及其在⾃然界各种不同的热⼒学(thermodynamical)与物理化学条件(physical-chemical conditions)下的⾏为。
V.M.哥尔德施密特(1933):地球化学是根据原⼦和离⼦的性质,研究化学元素在矿物、矿⽯、岩⽯、⼟壤、⽔及⼤⽓圈中的分布和含量以及这些元素在⾃然界中的迁移。
地球化学的主要⽬的,⼀⽅⾯是要定量地确定地球及其各部分的成分,另⼀⽅⾯是要发现控制各种元素分配的规律(laws governing element distribution and partitioning)。
V.V.谢尔宾娜(1972):研究地球的化学作⽤的科学---化学元素的迁移、它们的集中和分散,地球及其层圈的化学成分、分布、分配和化学元素在地壳中的结合。
(地球化学基础)涂光炽(1985):地球化学是研究地球(包括部分天体celestial bodies)的化学组成(chemical composition)、化学作⽤(chemical process)和化学演化(chemical evolution)的科学。
刘英俊等(1987):地球化学研究地壳(尽可能整个地球)中的化学成分和化学元素及其同位素在地壳中的分布、分配、共⽣组合associations、集中分散enrichment-dispersion及迁移循徊migration cycles规律、运动形式forms of movement和全部运动历史的科学。
The Mystery and Applications of Light on MetalsLight, a fundamental aspect of our universe, interacts with matter in a multitude of fascinating ways. When light interacts with metals, the results are particularly intriguing, giving rise to a range of applications that span from everyday life to cutting-edge technologies.Metals, being made up of a dense array of atoms, exhibit a unique optical behavior known as metallic reflection. This is the reason why metals appear shiny and reflective. When light strikes a metal surface, the electrons within the metal are excited, causing them to oscillate in unison. This collective oscillation of electrons, known as a plasmon, results in the reflection of light, giving metals their characteristic光泽.Apart from their reflective properties, metals also exhibit another remarkable optical phenomenon known as absorption. Depending on the wavelength of light, certain metals can absorb specific colors, giving them a characteristic hue. For instance, gold absorbs blue light and reflects yellow-orange light, thus explaining its rich golden hue.The interaction of light with metals finds applications in various fields. One such application is in the field of optics, where metals are used to create high-quality mirrors and lenses. Metals' ability to reflect light makes them ideal for such applications, as they can produce clear and distortion-free images.Another application of light-metal interaction is in the realm of photonics, which deals with the generation, control, and detection of light. Metals are used in photonic devices such as lasers and photodiodes, where they play a crucial role in amplifying or detecting light signals.Additionally, the unique optical properties of metals are exploited in the field of plasmonics, which aims to control and manipulate light at the nanoscale. Plasmonic devices, such as plasmonic antennas and sensors, utilize the collective oscillation of electrons in metals to enhance or manipulate light-matter interactions, leading to a range of applications in areas like biosensing, imaging, and photovoltaics.In conclusion, the interaction of light with metals gives rise to a fascinating array of optical phenomena that have found applications in various fields. From creating high-quality optical devices to manipulating light at the nanoscale, the study of light-metal interaction continues to reveal new insights and potential applications that hold promise for future technological advancements.。
太阳能英语作文六级作文Title: Embracing Solar Energy for a Sustainable Future。
In recent years, the global community has increasingly recognized the importance of renewable energy sources in mitigating climate change and achieving sustainable development. Among these sources, solar energy stands outas a promising solution due to its abundance, accessibility, and environmental friendliness. In this essay, we will explore the significance of solar energy and its potentialto shape a more sustainable future.First and foremost, solar energy offers a renewable and inexhaustible source of power. Unlike fossil fuels, which are finite and contribute to greenhouse gas emissions,solar energy relies on the continuous and abundantradiation from the sun. This means that harnessing solar power does not deplete natural resources or exacerbate environmental degradation. As concerns about climate change intensify, transitioning to renewable energy sources likesolar power becomes imperative for reducing carbon emissions and curbing global warming.Furthermore, solar energy technology has experienced significant advancements in recent years, making it more efficient and affordable than ever before. Innovations in photovoltaic (PV) cells and solar panel design have dramatically increased the efficiency of convertingsunlight into electricity, while economies of scale have lowered the cost of solar installations. As a result, solar energy has become increasingly competitive with conventional energy sources, particularly in regions with ample sunlight. This trend is further reinforced by government incentives, such as subsidies and tax credits, which incentivize investment in solar infrastructure.Moreover, the decentralized nature of solar energy makes it a highly resilient and versatile solution for meeting diverse energy needs. Unlike centralized power plants that rely on extensive transmission networks, solar installations can be deployed at various scales, from individual households to large-scale solar farms. Thisdistributed generation model enhances energy security by reducing reliance on centralized infrastructure and minimizing the risk of widespread power outages. Additionally, off-grid solar systems provide a lifeline for remote communities and developing regions without access to reliable electricity, empowering them to improve their living standards and economic opportunities.In addition to its environmental and economic benefits, solar energy also offers social advantages by promoting energy equity and inclusivity. By democratizing energy production and consumption, solar power empowersindividuals and communities to take control of their energy future. Through initiatives such as community solarprojects and rooftop solar programs, households and businesses can participate in the transition to clean energy while reaping the financial rewards of reducedutility bills and energy independence. Furthermore, investing in solar infrastructure creates job opportunities across the entire value chain, from manufacturing and installation to maintenance and research, thereby stimulating economic growth and fostering a skilledworkforce.Nevertheless, realizing the full potential of solar energy requires concerted efforts from policymakers, businesses, and society as a whole. Governments play a crucial role in setting ambitious renewable energy targets, implementing supportive policies, and facilitating research and development initiatives. Similarly, businesses have a responsibility to invest in sustainable practices and technologies, including the adoption of solar energy solutions in their operations. At the same time,individuals can contribute to the transition to solar energy by making informed choices about energy consumption, advocating for renewable energy policies, and embracing energy-efficient lifestyles.In conclusion, solar energy holds immense promise as a sustainable and environmentally friendly alternative to fossil fuels. By harnessing the power of the sun, we can reduce our dependence on finite resources, mitigate climate change, and create a more equitable and resilient energy system. However, realizing this vision requires collectiveaction and commitment to accelerating the adoption of solar energy technologies. Through collaboration and innovation, we can pave the way towards a brighter and more sustainable future for generations to come.。
五年级天文知识英语阅读理解25题1<背景文章>The Sun is a very important star in our solar system. It is a huge ball of hot gas. The Sun is extremely bright and gives off a lot of heat and light. Without the Sun, life on Earth would not be possible.The Sun is made up of mostly hydrogen and helium. It is constantly undergoing nuclear reactions that release a tremendous amount of energy. This energy travels through space and reaches Earth, providing warmth and light for all living things.The Sun also has sunspots, which are areas that appear darker on the surface. Sunspots are caused by intense magnetic activity. Sometimes there are solar flares and prominences, which are powerful eruptions on the Sun.1. The Sun is mainly made up of ___.A. oxygen and nitrogenB. hydrogen and heliumC. carbon and oxygenD. nitrogen and carbon答案:B。
a r X i v :a s t r o -p h /0106242v 1 13 J u n 2001Astronomy &Astrophysics manuscript no.(will be inserted by hand later)Supersolar metal abundances and the Broad Line Region ofNarrow-line Seyfert 1galaxiesStefanie Komossa 1,Smita Mathur 21Max-Planck-Institut f¨u r extraterrestrische Physik,Giessenbachstr.,D-85748Garching,Germany 2The Ohio State University,140West 18th Avenue,Columbus,OH 43210,USAReceived:February 2001;accepted:June 2001Abstract.Narrow-line Seyfert 1galaxies (NLSy1)are intriguing due to their extreme continuum and emission line properties which are not yet well understood.This paper is motivated by the recent suggestion that NLSy1galaxies might be young active galactic nuclei (AGNs)and that they may have supersolar metal abundances.We have examined the stability of broad emission line region (BLR)clouds under isobaric perturbation and its dependence on gas metal abundances.We show that supersolar metallicity increases the range where multiple phases in pressure balance may exist.This is particularly important for NLSy1s with steep X-ray spectra where it delays the trend of hindrance of a multi-phase equilibrium.Finally,the role of warm absorbers in the context of this scenario is assessed.Key words.Galaxies:active –Galaxies:nuclei –Galaxies:abundances –Galaxies:SeyfertRESEARCH NOTE1.Introduction1.1.Narrow-line Seyfert 1galaxiesX-ray and optical observations of the last decade revealed a new sub-class of active galaxies,termed Narrow-line Seyfert 1galaxies (NLSy1s hereafter).NLSy1galaxies are intriguing due to their extreme continuum and emission line properties.Their optical broad lines are narrower than in ‘normal’Seyferts and they show strong FeII emission.Their X-ray spectra are often unusually soft.Many prop-erties of AGN were shown to correlate strongly with each other.The strongest variance,often referred to as ‘eigen-vector 1’is defined by the correlation between the width of the H βemission line and the strength of the [OIII]emis-sion line,and the anticorrelation with the ratio FeII/H β(Boroson &Green 1992).NLSy1galaxies are placed at one extreme end of eigenvector 1and,in general,their X-ray softness correlates with their optical properties.There is evidence that the X-ray properties of NLSy1galaxies are best explained by a high accretion rate close to the Eddington rate (Pounds et al.1995).Recently,it has been proposed that the reason for the high accretion rate is the age (Mathur 2000a).In this scenario NLSy1galaxies with high accretion rate are AGNs in an early evolutionary phase.There are several lines of evidence which indicate that NLSy1galaxies may have super-solar gas phase metal abundances (Mathur 2000a,b;see our Sect.3for details)2St.Komossa,S.Mathur:The BLR of NLSy1galaxiescated in that intermediate region have revived the in-terest in multi-phase cloud models.It is also interest-ing to note that recent Chandra HETG observations of NGC4151confirmed the existence(Elvis et al.1990)of a high-temperature X-ray emitting plasma,interpreted in terms of a hot intercloud medium(Ogle et al.2000).This observation can be well explained by the classical KMT modeld,due to the veryflat X-ray spectrum of NGC4151 (Komossa2001b).With respect to Narrow-line Seyfert1galaxies,Brandt et al.(1994)suggested that the relatively narrow optical BLR lines of these galaxies might be traced back to the hindrance of BLR multi-phase equilibrium in the presence of steep X-ray spectra.Model calculations of Komossa &Meerschweinchen(2000,KM2000hereafter;see also Komossa&Fink1997a)confirmed the idea.However,re-cent observations suggest that other mechanisms might be at work(e.g.,a small black hole mass would lead to narrow lines in NLSy1galaxies).Motivated by the recent evidence for supersolar metal abundances in NLSy1galaxies we ex-tend here the earlier calculations to explore in more detail the influence of gas abundances.We show that supersolar metallicity increases the range where multiple phases in pressure balance may exist,and that it delays the trend of hindrance of a multi-phase equilibrium due to steep X-ray spectra.2.Model calculations and results2.1.The modelWe used the photoionization code Cloudy(Ferland1993) to carry out the calculations.In order to obtain the cloud temperature as a function of pressure the following as-sumptions about the cloud properties were made: Constant gas density(log n H=9.5)and solar element abundances according to Grevesse&Anders(1989)were adopted,and then varied relative to the solar value.It was assumed that there is no strong temperature gradi-ent across the clouds.The clouds were illuminated by the continuum of a central point-like energy source with a spectral energy distribution(SED)from the radio to the gamma-ray region as in Komossa&Schulz(1997).This mean Seyfert SED1consists of piecewise powerlaws with, in particular,an energy indexαuv−x=−1.4in the EUV. The X-ray photon indexΓx was varied to cover the range typically observed in NLSy1galaxies.The cloud temperature after each model run was ex-tracted,as a function of the ionization parameter.The ionization parameter is defined asU=Q1Rodriguez-Pascual et al.(1997)collected IR−X-rayfluxes of Seyfert and NLSy1galaxies and concluded that both are generally very similar concerning luminosities in different en-ergy bands except that NLSy1s tend to be underluminous in the UV.where n is the gas density,r the distance of the gas cloud from the continuum source,c the speed of light,and Q the number rate of photons above the Lyman limit(ν0=1015.512Hz).The stability of broad line clouds to isobaric perturba-tions can be examined by studying the behavior of tem-perature T as a function of pressure.If the temperature is multi-valued for constant pressure,and the gradient ofthe equilibrium curve is positive,several phases may exist in pressure balance.Results are shown in Figure1where variations in U/T correspond to variations in1/pressure.In the upper part of Fig.1,we have plotted a sequence of curves which were derived by using different X-ray slopesin the SEDs which illuminate the clouds.The powerlaw index changes fromΓx=–1.5to–4from left to right,and the multi-valued nature of the curves disappears for steepX-ray spectra.Due to the relatively weaker X-rayflux and the fact,that the value of U is dominated by the EUV flux near the Lyman limit,the gas remains longer in thephase which is characterized by photoionization-heating and collisional-excitation-cooling.The same holds for acontinuum with a hot soft X-ray excess(KM2000).For comparison with results obtained using the mean Seyfert SED,we have collected multi-wavelength continuum ob-servations of the NLSy1galaxy NGC4051(Komossa& Fink1997a and references therein),and plotted the corre-sponding equilibrium curve in Fig.1(see next Section fordetails).Metal abundances,which affect the cooling of the gas,were then varied.Wefind that supersolar metal abun-dances increase the range where a multi-phase equilib-rium is possible,whereas subsolar abundances have theopposite effect(cf.the curve of Fig.1which refers toΓx =–1.9).Whereas SEDs with an X-ray spectrum steeper thanΓx≈−2.5do no longer allow for multiple phases in pressure equilibrium if solar gas phase abundances are adopted,such equilibria are still possible in case of super-solar abundances.In a next step,we selectively increased the neon and nitrogen abundances(Z N,Ne=3×Z⊙),motivated by(a1) the observations of X-ray spectral features around∼1.1-1.4keV which could partly be due to increased Ne absorp-tion,(a2)optical evidence for overabundant N,and(b)the report of Fabian et al.(1986)that Ne has a particularly strong influence on the equilibrium curve(but see com-ment(ii)of our Sect.3.3).We do notfind any exceptional effects(Fig.1),but note that modifications of the shape of the curve are dominated by Ne,not N.2.2.The BLR in NGC4051We have constructed the equilibrium curves with the SED of the NLSy1NGC4051as an input.The results for solar and super-solar abundances are shown in Figure1c.Below, we give some order-of-magnitude estimates of the parame-ters of the BLR of NGC4051in the context of our general modeling approach.It is clear from thefigure that a two-St.Komossa,S.Mathur:The BLR of NLSy1galaxies3Fig.1.Equilibrium gas temperature T against U/T for various SEDs incident on the gas and metal abundances of the gas.Upper panel:Solid black lines:mean Seyfert input continuum withΓx=–1.5,–1.9,–3.0and–4.0as labeled in the graph;dot-dashed line:observed multi-wavelength continuum of the NLSy1galaxy NGC4051withΓx=–2.3.Solar gas phase abundances were adopted.Middle panel:sector of upper panel,showing the dependence on abundances. Solid lines:mean Seyfert input continuum withΓx=–1.9and–3.0replotted for comparison;thick dashed lines: overabundant metals(Z=3×Z⊙),thin dashed line:selectively enhanced nitrogen and neon abundances of3×solar, dotted lines=underabundant metals(Z=0.3×Z⊙).Lower panel:results specific to NGC4051.The dot-dashed line corresponds,again,to the observed multi-wavelength continuum of NGC4051using solar abundances.The open circles mark the location of NGC4051’s warm absorber,observed at two different epochs(Nov.1993,Komossa&Fink 1997a;and Nov.1991,KM2000).The values were derived from one-component warm absorberfits to the ROSAT X-ray spectrum of this galaxy,assuming solar metallicity.Dashed and dotted line have the same meaning as above.4St.Komossa,S.Mathur:The BLR of NLSy1galaxiesphase equilibrium with common pressure does not existfor solar abundances.On the other hand,such an equi-librium is possible if abundances are super-solar.In thecontext of the BLR cloud model,the lower temperatureregion corresponds to the BLR clouds while the the con-fining medium is in the hot region.From Figure1c,wefindthat the ionization parameter of the BLR spans a rangebetween log U=0.12and log U=0.30.Reverberationmapping observations can determine the distance of theBLR from the nucleus accurately.In NGC4051it wasfound to be1.6×1016cm(Peterson et al.2000).Usingequation1,the density in the BLR can be constrainedto be8.7<log n<9.1.2If such a model for a BLR isvalid for all NLSy1s,then it implies that BLR densities inNLSy1s are low and ionization parameters are higher thanthe“standard”value(log U≈−2).Higher densities andlower U may be obtained for even higher metallicities.These results are consistent with the conclusions ofRodriguez-Pascual et al.(1997)who argue in favour ofsmaller density and higher ionization parameter in NLSy1galaxies.Note,however,that they did not consider super-solar metallicities in their model.The next question is whether the parameters of thewarm absorber in NGC4051are consistent with beingin pressure equilibrium with the BLR clouds.This is anon-trivial question in the case of NGC4051with highlyvariable ionizing continuum.Presenting non-equilibriumphotoionization calculations,Nicastro et al.(1999)esti-mated that the warm absorber in NGC4051is at a dis-tance of∼1.3±0.3×1016cm from the nucleus,which issimilar to that of the BLR.Therefore,pressure equilib-rium with the BLR clouds is possible.A more detailedcomparison will be possible,once X-ray observations ofhigher spectral resolution of NGC4051become available,in combination with photoionization calculations that in-clude time-dependent effects.3.Discussion3.1.Evidence for supersolar metallicity in NLSy1galaxiesMathur(2000a;see also Kawaguchi&Aoki2000)sug-gested NLSy1s to be young/rejuvenated active galaxies.In analogy to high-z quasars they may have super-solarmetal abundances,as indicated by a number of observa-tions:An overabundance of iron was suggested to explainthe strong optical FeII emission in NLSy1s(Collin&Joly2000).Supersolar Fe or Ne provide a possible explanationfor the peculiar absorption features around∼1keV seen insome NLSy1galaxies(e.g.,Ulrich et al.1999,Turner et al.1999).Overabundant Fe was also discussed to explain the3 e.g.,Murray&Chiang1995(disk-driven winds;see alsoDietrich et al.1999),Edwards1980,Alexander&Netzer1994(bloated stars),Perry&Dyson1985(cloudlet creation by ra-diative shocks)St.Komossa,S.Mathur:The BLR of NLSy1galaxies5an AGN(Ogle et al.2000),interpreted as hot intercloud medium.The study of Rodriguez-Pascual et al.(1997)showed that NLSy1galaxies possess broad emission lines in the UV.They explained the different line-widths measured in the optical and UV by a matter-bounded BLR,as discussed by Shields et al.(1995),in NLSy1galaxies.Thisfits to the KMT model approach,which predicts a thin shell-like BLR.3.4.Warm absorbers in NLSy1galaxiesThe region in which the temperature is multi-valued for constant pressure is preserved by supersolar metallicity in NLSy1s.If the X-ray spectra are not too steep,a pressure balance between a cold phase(the BLR in NLSy1s)and a hotter intermediate phase is possible(even if the very hot phase is absent).This intermediate region has previously been asso-ciated with ionized absorbers(e.g.,Reynolds&Fabian 1995,Komossa&Fink1997a,b,Elvis2000a,b;see Fig.1 of Komossa2001for a summary).The suggestion that NLSy1s are young objects with a high accretion rate makes the presence of a large amount of(ionized)gas in the nucleus likely(Mathur 2000b).Indeed warm absorbers have been detected in quite a number of NLSy1galaxies(e.g.,Brandt et al. 1997,Komossa&Fink1997a,Hayashida1997,Komossa &Bade1998,Iwasawa et al.1998,Ulrich et al.1999, Vaughan et al.1999),or have been suggested to explain some unusual spectral/variability properties of NLSy1s (e.g.,Komossa&Meerschweinchen2000).Some studies indicate that ionized absorbers are somewhat less abun-dant in NLSy1s than in Seyferts(Leighly1999).The rea-son could be a higher degree of ionization of the absorbers which makes them less easily detectable in NLSy1s.The OVII absorbers,seen in some NLSy1galaxies(e.g.,IRAS 17020+4544),which might atfirst glance suggest a low de-gree of ionization,can easily be explained by the presence of a second warm absorber component which is located at larger distances from the nucleus,and which is mixed with dust(Komossa&Bade1998).4.Summary and conclusionsWe have presented a study of the influence of metallicity on the multi-phase equilibrium in photoionized gas.We find that supersolar metallicity increases the range over which a multi-phase medium in pressure balance may ex-ist.In objects with steep X-ray spectra,like NLSy1s,such an equilibrium is not possible if gas metallicity is less than or equal to solar.As a result a pressure confined BLR cannot exist.This problem is alleviated if metallicity is supersolar.This offers further credence to the suggestion that NLSy1s may have supersolar metallicity.High reso-lution X-ray spectroscopy,together with optical/UV spec-troscopy,is required to derive elemental abundances and to address these issues in more detail.The results of this Note are also of relevance to high-redshift quasars,since their BLR clouds show supersolar metal abundances. 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