Monday, September 9, 2019
Financial Statement Analysis Project Research Paper
Financial Statement Analysis Project - Research Paper Example In 2011 the cash and investment balances of the company rose to $125 million due to the initial public offering made in the year 1997. Financial Information of Company The company’s performance in case of the operating activities has been good enough but the same cannot be said as far as Amazon’s financial and investing activities are concerned because the company is showing a negative return of $482 million (financing activities) and $1930 million (investing activities) in 2011. This decrease was mainly the affect of the capital expenditures and the changes in the working capital over the year. Rising net sales of the company which by approximately 41% than the last year due to the effect of the exchange rates. But the effect of the rising sales were diluted due to the increase in the operating expenses of the company which resulted in the net income of Amazon to dip from $1152 million (2010) to $631 million (2011). Summary of the Firm Markets Market of operation for A mazon is mainly in North America, US and Canada. The common stock of Amazon.com, Inc. (AMZN) is dealt in Nasdaq Global Select Market. In 2010 amazon.com has witnessed a high of $185.65 in the fourth quarter and a low of $105.80 in the third quarter whereas in 2011 Amazon witnessed a high of $246.71 in the fourth quarter and a low of $160.59 in the first quarter. ... cation where the Amazon.com makes most of its business is North America, US, Canada, UK, France Germany, Italy, Spain, Japan, China and soon is going to launch websites in Poland, Sweden and Netherlands. Amazon.com has its services stations in prime areas of North America, Latin America, Europe and Asia. The global headquarters of Amason.com is situated in Seattle in Washington. Partners The main strategic partners of Amazon.com were America Online, Yahoo, Netscape, GeoCities, AltaVista, @Home and Prodigy maintaining a long-term relationship since the year 2007. Competitors The main competitors in the field of online trading in comparison to Amazon.com, Inc. are Apple Inc., Barnes & Noble, Inc. As the gross profit of Amazon is 22.76% whereas in case of Apple Inc. is 43.95% and Barnes & Noble’s, Inc. is 26.52%. Comparative Analysis The company chosen for the comparative analysis with the Amazon.com, Inc. are EBay, Inc. and Google, Inc. because both the companies of comparison b elong to the same industry (Catalogue and Mail Order Houses) dealing in the Nasdaq market. Net Income of Amazon.com, Inc. is $560 million whereas that of EBay, Inc. is $3.32 billion and Google, Inc. is $10.83 million. Thus being a giant in the field of online trading Amazon.com is a clear winner. The higher the price earnings ratio of the company higher is its growth rate. Price earnings ratio of Amazon.com, Inc. is 180.41, in comparison to EBay, Inc. which has a P/E ratio of 16.15 and Google, Inc. with a P/E ratio of 17.59. This proved that the stocks of Amazon.com, Inc. are much more preferable in comparison to EBay, Inc. and Google, Inc. The price to sales ratio of a company projects that lower the P/S ratio of the company the better it is as the investor has to pay less. Price to sales ratio
Sunday, September 8, 2019
People who are under 21 should not allowed to drive Research Paper
People who are under 21 should not allowed to drive - Research Paper Example These precautions can help saving 1,700 accidental injuries and 200 deaths from speed driving in a year. Rash driving needs to be controlled, as similar driving limits also apply in countries like New Zealand, Australia, and some regions in the US as well (Triggle par. 1-3). Although overall deaths from accidents have been on the decrease but the teenage habit of listening to music while driving is a big accidental risk. This bad habit of listening to music through MP3 players and iPods while driving has been acknowledged for awareness purpose by the Tune into Traffic campaign (Triggle par. 5). Teenagers go a step ahead by not just listening to music while driving, but also texting messages, which is a relatively bigger risk on the road for causing of road accidents. Incidentally, there has been a significant check on road accidents, reaching to an all-time low, but still 2,222 deaths were reported due to road accidents the previous year (Triggle par. 5). Teenage accidents cause loss of gasoline, life, and money, as they develop a habit of driving just for the fun of driving, which is a leading cause of wastage of gasoline. Gasoline being a limited natural resource, a check on its wastage by not allowing driving licenses till they reach the age of 21 can help in saving this resource. The practice of graduated driving licensing can save many accidents from occurring. Otherwise also, road accidents cause huge loss of money as well, as a reduction in accident rates in the UK can relieve the economy from the financial burden amounting to  £890m (Triggle par. 8-11). We should stop teenagers from driving for their own benefit and for the benefit of other society stakeholders. Actually, teenagers have other alternatives to reach their destinations. Teenagers should use the available public transportation system, such as buses to reach their destination. There is no logic in going privately when buses are
Saturday, September 7, 2019
The Depletion of Natural Resources Essay Example | Topics and Well Written Essays - 1000 words
The Depletion of Natural Resources - Essay Example The density of palms and lianas were also recorded as they were observed to have different behavior than that of the dicotyledonous trees. The study was conducted under the original site of 78/5 experiment that was conducted in 1978 at Tonka research site in Suriname that is located within the Kabo creek, comprising of rain forest area. The region had around 197 species with 37 of them having great commercial value. In 1978, three levels of exploitation and three levels of silviculture refinements were tested and replicated three times. Virgin forest plots or VFPs were also set up in three replications using different compartments. The replications were carried out in nine compartments comprising of 1 ha assessment plot which was further divided into ten subplots. The exploitation levels were coded as E14, E23, and E46 where logging took place. E46 saw excessive logging which was considered non-acceptable. Silviculture levels were coded as S0, S18, and S14 where unwanted trees. In the heavy refinement area, cutting off unwanted trees was accompanied by climber cutting and poison girdling of non-commercial trees. The current study took a small part of the original experimental area comprising of three compartments per replication along with 3 VFP compartments, totaling 60 subplots. The density of 8 selected tree species studied on the basis of 20% Random sampling of 100 plots. Species were selected for their adaptability to sunlight and shade. Vegetation layer of 3-10 m has opted because they were bested suited as test subjects. Using various statistical and non-statistical measurements like forest class, ANOVA, t, and chi-square test, Kruskal-Wallis and Wilcoxon signal tests were used to test the hypothesis. Mortality was higher in heavy exploitation and treatment region. Climax trees are not much-affected with treatments.
Success of Henry VII in strengthening the financial position of the Crown Essay Example for Free
Success of Henry VII in strengthening the financial position of the Crown Essay Crown lands were the kings estates. There were many ways in which Henry increased the yield of his crown lands. * Henry gained a lot of land from the Battle of Bosworth by naming himself king before the day of the battle therefore making all his opponents traitors and had the right to attain them all. * He gained a lot of land partly by good fortune from York and Lancaster. * Henry was not as generous as pass kings e.g. Edward IV, and kept most of his lands to himself but with the exception with some people like his mother, his uncle Jasper. * Used escheats, which were a right for the king to have lands passed to him when men died without heirs. * Skilful workers that helped Henry increase yield of lands e.g. Duchy of Lancaster and Sir Reginald Bray. Effectiveness of policy. Income from crown lands was increased by 30 % generally during his reign and with the help of Sir Reginald Bray the annual income of à ¯Ã‚ ¿Ã‚ ½650 increased 10 fold. Custom duties. Theses were levied on wool, leather, cloth and wine. It was a fee, which was needed to be paid for trading. Edward IV increased his income by increasing trade and cutting down on embezzlement at all levels. Henry did the same and followed what Edward IV did. Effectiveness of policy. The average annual receipts were à ¯Ã‚ ¿Ã‚ ½33,000 for the first 10 years of the reign and à ¯Ã‚ ¿Ã‚ ½40,000 thereafter, so there was not a great deal of raised income. Feudal dues. Feudal dues were paid be people who held land from the king in return for military service. Feudal dues included: * Wardship, in which the king took control in the estates of minors until they came an age. * Livery, the payment to recover lands out of wardship. * Marriage, right of crown to arrange marriages for unmarried heirs/heiresses. * Relief, payment made so that the crown recognised inheritance of land rather then reclaiming it to the throne. Effectiveness of policy. Initially the proceeds from wardship and marriage were small, amounting to only à ¯Ã‚ ¿Ã‚ ½350 in 1487, but after 1503 a special officer was appointed to supervise them and by 1507 the annual income was à ¯Ã‚ ¿Ã‚ ½6,000 a massive increase. Revenue through the operation of the judicial system. As monarch, Henry was head of the judicial system and was therefore entitled to its profits. Henry made the most of this by doing a number of things. * Fines: Henry was eager to exact fines rather then imprisonment or execution to increase his incomes. * Attainders: Method of punishment whereby the profits from the attained persons lands go to the crown. Effectiveness of policy. There were a lot of attainders e.g. Sir William Stanley had to payà ¯Ã‚ ¿Ã‚ ½9,000 and thenà ¯Ã‚ ¿Ã‚ ½1,000 p.a. for his treason in 1495. The highest passed was 51, total of 140, a third reversed. Parliamentary grants. Extraordinary revenue was money which came to the crow on particular occasions and therefore with no regularity. It arose from the obligation of the kings subjects to help him when the national interest was threatened. It was received, by the king requesting for the parliamentary consent. The usual type of tax levied was a national assessment. Effectiveness of policy. Parliamentary grants were less successful as they restricted Henrys freedom of action in return for money. By 1485 the taxes raised had ossified into a fixed sum of about à ¯Ã‚ ¿Ã‚ ½29,000. Loans and benevolences. The king could rely on loans from his richer subjects in times of emergency by request, and was almost virtually impossible to decline. Effectiveness of policy. It was effective in the way it was quite successful as Henry had only asked modest amounts of money from his subjects and had always repaid back, probably to lessen the risk of rebellion of some sort. Feudal obligations. As feudal overlord Henry could demand money from his subjects for special occasions e.g. the knighting of his eldest son, marriage of his eldest daughter. Effectiveness of policy. Anyone who earned more then à ¯Ã‚ ¿Ã‚ ½40 p.a. had to become a knight, along with the financial burdens that it entailed in military service. So this would have made a lot of money to add to the kings income from the financial burdens. Clerical dues and other income from the church. Convocation usually offered money when the king was requesting it from the parliament grant e.g. in 1489 when à ¯Ã‚ ¿Ã‚ ½25,000 was raised for the French war. Effectiveness of policy. Due to a rash of deaths amongst the bishops in the last years of the reign, Henry received over à ¯Ã‚ ¿Ã‚ ½6,000 per annum in this way.
Friday, September 6, 2019
The Human Population Essay Example for Free
The Human Population Essay Abstract Why is it that there are countries today experiencing economic stability and unrelenting progress while, in contrast, there countries still experiencing poverty? These are questions that can be answered when look through and compare populations of different countries. There are stages that a population goes through over time and those have major effects on what a country experiences in general. The Human Population            It’s splendid how colorful and beautiful a Monarch butterfly (Danaus Plexippus) is that no one would think that it started as a poor and humble larva called the caterpillar. Similarly, human population doesn’t just pop – out of the smoke and there is it – in its most thriving state. Just like a butterfly, human population undergoes several transformations and transitions towards its prosperity as time winds off. Even first world countries today experienced misery before. It’s just that they have already much further gone through what we call the demographic transition.            Having a sort of similarity to butterflies’ metamorphic process, demographic transition is one dramatic process of transformation that a certain human population experiences at different periods of time. What we don’t know is that population changes its â€Å"state†at different points of history. Say for example, a certain country now experiences an explosion in terms of child population. This is true for the third world countries such as Africa’s sub – Saharan countries such as Ghana and some South – East Asian countries like Laos. But that doesn’t mean that such countries would experience it forever. There would be some point in time that they would undergo transformation and leave the current state of their population. Even well developed countries experienced undergoing high population rates due to extensive CBR (Crude Birth Rate). The only thing is that history has provided them to surpass the stage earlier than other countries. Take England as an instance. England had experienced undergoing this stage as early as the 1800’s.            Just what was said earlier, a certain human population doesn’t just emerge immediately already as a thriving population. It undergoes several stages in the demographic transition.            Stage 1 of the demographic transition is generally the â€Å"struggle†. At this stage, people’s way of thinking is that they must bear many children to ensure a stronger working force in the future, that contributes to a high CBR. Also, another reason that contributes to a high CBR at this stage is the lack of birth control programs that is being implemented. This is true for the western countries during the industrial revolution although there are still some countries under this stage up to this day. Along with the high CBR is also a high CDR (Crude Death Rate) in the population. Failure to prevent epidemics and diseases due to lack of sanitation and medicine is one factor that contributes to a high CDR.            The next stage of the demographic transition is when the population is rapidly growing at an alarming rate. There is a high rate of children getting born over time but the death rate doesn’t grow. In some countries which are at this stage provides insufficient birth control programs but is providing adequate health care programs. Creating an unequal trend between the CBR and the CDR. More children in the population means that there is a large number in the population that must be provided with needs that accounts to more expenses that must be satisfied by the population. This results to an extensive use of resources that leads to environmental destruction like far-reaching logging and illegal quarrying. This in turn leads to poverty which is true in certain developing countries such as the third world countries. In order to get through, just like what the stable countries have done, the government must find ways to solve such problems. Providing jobs, better health care and sanitation programs and education can help on alleviating the crisis.            During the third stage of the transition, there is already an apparent stability of the CBR and CDR. The countries at this stage can already provide for much better birth control programs although there is still a slight increase of birth rate. China, South Korea and Cuba are examples of countries undergoing this stage.            The last stage is during the time a certain country has already attained economic stability. Some Europeans are had already reached this stage of Demographic transition. The labor force in these countries is massive that creates a large income flow, that’s why the country is undoubtedly able provide effective health programs, birth control programs and other courses that would take care of its population and maintain it.            One distinguishing characteristic of countries at this stage is that it has a mature population. Meaning to say that a large percentage making up the population is people aging from 60 years old and above or what we call the senior citizens. Gradually, aging countries, that’s how we should call them, experiences economic turn down. The reason for this is that the aging population grows that result to the dropping of the working population. And also, contributing to the population’s economic crisis is that the government tends to allocate a large part of the country’s budget for old age people’s care and services.            And also, a large part of countries in the fourth stage of demographic transition are immigrants.            So when we see a population in such a state, it doesn’t mean forever. Before being a butterfly, it must be a caterpillar at first. References About.com (2007). Demographic Transition. Retrieved October 22, 2007, from http://geography.about.com/od/culturalgeography/a/demotransition.htm Institute For Futures Studies (October 2000). Four Phases in the Demographic Transition. Retrieved October 22, 2007, from http://www.framtidsstudier.se/filebank/files/ 20051201$132852$fil$u0byJpuS9KO6S443Tj6g.pdf
Thursday, September 5, 2019
Solar Radio Emissions: Investigating Reactivated Prominences
Solar Radio Emissions: Investigating Reactivated Prominences Madeleine Eve Andrew Johnston Solar Radio Emissions in Investigating Reactivated Prominences Literature Review Abstract Astronomical objects that have a changing magnetic field can produce radio waves, which are the longest waves in the electromagnetic spectrum. By studying the radio waves emitted by the Sun, astronomers can acquire information about its composition, structure and motion. This aim of the present project is to use solar radio emissions produced during the re-activation of prominences in order to investigate possible energy sources for the activation. The purpose of this literature review is to analyse relevant papers on the subject matter that will be covered in this project, and give a summary of the literature in the field, whilst covering the history and importance of the topic, along with what types of instruments can be used to measure radio waves, and how radio waves are useful in studying prominences and their reactivation. 1 Introduction Radio waves are a type of electromagnetic radiation, which is a form of energy produced whenever charged particles are accelerated. They have frequencies from 3kHz to 300GHz, with corresponding wavelengths ranging from just 1mm to 100km. The understanding of solar radio emissions began in 1942, when an English physicist and radio astronomer, James Hey, was tasked to work on radar anti-jamming methods for the military. He had several reports of severe noise jamming of radars signals in the 4-8 meter wavelength range, and after examination, he realised that the direction of maximum interference was coming from the Sun, and concluded that the Sun radiates radio waves (M. Pick, 2008). The observation of solar radio emissions has proved to be a useful tool in our efforts to understand solar physics., In particular solar radio emissions can be used to study local plasma density and magnetic reconnection, which relates to the release, over periods of a few minutes, of magnetic energy stored in the corona and which accompany solar eruption events like prominences which this project will be focusing on. In addition, radio wave emissions from solar flares offer several unique diagnostic tools which can be used to investigate energy release (A. O. Benz; 2005), plasma heating, particle acceleration, and particle transport in magnetized plasmas. A Solar flare is an observed sudden flash of brightness over the Sun’s surface or the solar limb, powered by magnetic reconnection. Scientists study the Sun through radio emissions and other electromagnetic emissions and this has an additional advantage in that it provides a better understanding other stars, and the important processes they have to offer, such as nuclear fusion, which is a potential alternative energy source scientists have been trying to recreate on Earth for decades. The study of prominences and other eruptive events is important for providing an insight into the mechanics of the interior of the Sun, and also to assist us in the prediction of ‘space weather,’ which can effect satellites, and the Earth’s atmosphere and magnetic field. A solar prominence is a large, bright, gaseous feature that is anchored to the surface of the Sun in the photosphere, and extends outwards into the Sun’s corona in a loop shape. Solar prominences are made from plasma that is roughly 100 times cooler and denser than the plasma in the corona and so, when viewed with the sun as a backdrop, they appear dark, and are referred to as ‘filaments.’ They can last for several months, and are held in place above the Suns surface by strong magnetic fields. The exact composition of prominences is currently unknown, but it has been proposed that they are made up of roughly 10% helium and 90% hydrogen. Solar prominences, like other erupting projectiles, are useful to observe as they are good indicators of the magnetic field pattern of the sun, since they lie above the magnetic neutral lines. There are two basic types of prominences: quiescent and active-region prominences. Quiescent prominences are typically larger than active-region prominences, and also extend further into the corona, often reaching up to and over 30 000 kilometres above the Sun’s corona (T. E. Berger, 2012). In addition, quiescent prominences have a magnetic field of roughly 0.5-1mT, allowing them to extend further from the surface of the Sun than active-region prominences, which are much smaller, have much larger magnetic fields of around 2 – 20mT, and mostly do not travel over 30 000km. This project will largely be focusing on Quiescent prominences, as, extending further away from the Sun, they are easier to study using radio waves. Prominences are always projected from filament channels, which are along polarity inversion lines; where the magnetic field is highly non-potential (J. Chaf, 2005). These channels are the source of all major solar eruptions, such as coronal mass ejections and flares. The temperature of a prominence that hasn’t erupted, is typically , and these often appear as a long horizontal sheet of plasma. Several different models have been proposed in order to explain how cool, dense objects like prominences can be supported and thermally isolated from the surrounding hot coronal plasma. It is generally accepted that these models can generally be placed into one of two main categories: dip models, and flux rope models (for example: D. H. Mackay, 2010, D. J. Schmit, 2013, P. F. Chen; 2008). The main similarity between dip models and flux rope models is the suggested existence of concave-upward directed magnetic fields to support the prominence plasma against the downward gravitational force. Following this mechanism, it can be assumed that the plasma in a prominence is frozen to the magnetic field lines. Prominence plasma, however, is actually only partially ionised, and so it is not entirely clear how the non-ionized portion of plasma is supported, and how rapidly the neutral material might drain across the magnetic field lines. Scientists are still researching how and why prominences are formed, and the cause for their reactivation. The models proposing how prominences are supported are vital in understanding their formation and reactivation. 2 Radio Emissions with Prominences Measurable coherent radio emissions occur during flares, and are intermittent and in bursts, driven by the magnetic reconnection process, giving them the term ‘radio burst.’ Previous experiments (J. P. Raulin; 2005, J. P. wild; 1956, R. F. Wilson; 1989, G. Swarup; 1959) in measuring radio emissions produced from prominences have found that Type I bursts are predominantly emitted, Type I being characterised by their long lifespan lasting from hours to days, having a frequency of 80-200mHz with corresponding wavelengths of roughly 2m, and being produced by electrons with a charge of several keV within coronal loops. Moving Type IV radio bursts are also associated with prominence eruptions, these last from half an hour to 2 hours, with a frequency of 20-400MHz, and a corresponding wavelength range of 1 to several meters. As mentioned in the introduction, scientists can use radio waves to gain an insight into how plasmas behave during the prominence eruption process. This can be done through magnetohydrodynamics (MHD), which is the study of the dynamics of electrically conducting fluids. Scientists have previously used MHD equations in investigations to understand the formation and reactivation of prominences (J. A. Linker; 2001, D.J. Schmit;2013, G. P. Zhou;2006, A. K. Srivastava; 2013). An investigation using SDO/AIA (T. E. Berger; 2012) on the formation of prominences produced a series of images that showed the reactivation of a prominence. The sequence showed that after a prominence has completed its eruptive cycle, it slowly disappears due to drainage and the lateral transport of plasma, and a bright emission cloud forms in the upper regions of the coronal cavity. The cloud descends towards the lower region of the cavity while successively becoming brighter, and a new prominence then forms, rapidly growing in both the vertical and horizontal dimensions. The new prominence is the reactivated old prominence. The coronal cavity core in the image then grows darker as the reactivated prominence continues to grow. The reactivated prominence reaches its maximum size after a number of hours, and the emission cloud in the cavity reduces correspondingly. Using the time sequence of images from this T. E. Bergers paper, an idea of what to search for in data to find reactivat ed prominences can be formed. Work has been performed (by C. Chifor; 2006; D. H. Mackay; 2010, D. J. Schmit, 2013) which also investigates how prominences are formed, concluding that reconnection events trigger different phases in prominence eruption. The flux rope model discussed earlier has been found to be a good model in several investigations (S. E. Gibson; 2006, P. F. Chen; 2008, G. P. Zhou, 2006). Helical field lines provide a support for the mass of the prominence, and are capable of storing the magnetic energy needed to propel the prominence. A coronal flux rope can be interpreted as a magnetic structure which consists of field lines that intricately twist around each other a number of times between the two ends that are anchored to the photosphere. Studies mentioned earlier involving MHD have been found to support the flux rope model, making the model a good investigation point for the project. Further research has been carried out into the cause of reactivated prominences (R. F. Wilson; 1989), producing evidence that suggests that as the initial prominence dissipates, a ‘feed-back’ mechanism occurs, during which interactions of the large scale loops trigger burst activity in lower lying loops. 3 Instruments There are two main types of instruments that can be used to observe objects in the radio wave portion of the electromagnetic spectrum, the type selected for use depending on the strength of the signal and the amount of detail needed. The first type of instrument comprises radio telescopes, which are a form of directional radio antenna. As the range of frequencies in the radio wave portion of the electromagnetic spectrum is very large, there are a variety of different antennae that are used in radio telescopes, differing in their size, design and configuration. When measuring wavelengths of 30-3 meters, the radio telescopes use either directional antenna arrays, or large stationary reflectors with moveable focal points. At shorter wavelengths dish style radio telescopes are more largely used. The second type of instrument comprises radio interferometers, which are made up of arrays of telescopes or mirror segments. The main benefit of using a radio interferometer is that the angular resolution is similar to that of a radio telescope with a large aperture, however, radio interferometers do not collect as many photons as radio telescopes, and they cannot detect objects that are too weak. However, an array of telescopes will provide very good resolution as a result of aperture synthesis. Aperture synthesis is an imaging process that mixes signals from the array of telescopes to produce images with an angular resolution equivalent to that of a single instrument with a diameter equal to the overall size of the array of telescopes. This makes it easy to obtain high resolution images of the Sun. SDO/AIA EUV Several different types of data that can be used to review the radio emissions of the Sun in order to extract information on prominences have been researched. The first is SDO/AIA EUV data; SDO being the Solar Dynamics Observatory, which is a NASA mission that has been observing the Sun since 2010. The goal of the SDO is to understand the influence of the sun on the Earth and close space by studying the solar atmosphere over time and space in many wavelengths at the same time. Currently, investigations are focused on how the Suns magnetic field is generated and structured, and how the stored magnetic energy is converted and released into the heliosphere and geospace in the form of solar wind, energetic particles, and variations in solar radiance, which is the measure of the power per unit area on the Earth’s surface. The SDO uses the Atmosphere Imaging Assembley (AIA), an instrument which provides continuous full-observations of the solar chromosphere and corona in seven extreme ultraviolet channels. The AIA is comprised of four telescopes providing individual light feeds to the instrument. The Extreme Ultraviolet Experiment (EUV) is the instrument that measures the Sun’s extreme ultraviolet irradiance, and incorporates physics based models in order to further understand the relationship between EUV variations and magnetic variation changes in the Sun (N. Labrosse, 2011). Fig 1. This image is an example of SDO/AIA data, taken from (T. E. Berger; 2012) from a time sequence which investigates the radio emissions from the Sun leading up to the reactivation of a prominence event. Using the data produced by the two, an image can be created of the Sun that combines physical processes such as prominences, with information on the magnetic field at the time. An example is shown in ‘Fig 1’ above, which shows a reactivated prominence eruption and its corresponding radio emission in the form of a cross-sectional image of the surface of the Sun. Data collected from the AIA has been made public through online databases, providing a ready set of images and films that can be analysed in order to observe prominences and their reactivation for this project. NoRH The second type of data that will be focused on in order to infer radio emissions from the Sun is Nobeyama Radioheliograph data. The Nobeyama Radioheliograph is an array of 84 antennas dedicated for solar observation at the Nobeyama Radio Observatory, located in the Japanese Alps, and was constructed with the purpose of observing the Sun, using non-thermal emissions in particular. The Nobeyama Radioheliograph is a radio interferometer, and the original data comprises sets of correlation values of all the combination of antennas. The antennas correspond to the spatial Fourier components of the brightness distribution of the solar disk. The Nobeyama Radioheliograph is particularly useful in studying prominences (M. Shimojo, 2005), as due to its large daily observation window, combined with the low time resolution of 1 second, and a spatial resolution of roughly 13†, it can produce highly dynamic images. Even though the NoRH is ground based, the consequences of the surrounding weather conditions are minimal compared to that of other ground based observations, and observations can take place even in turbulent unclear weather. NoRH has also developed an automatic detection method, the most important factor in using the instrument to detect prominences, as data will be recorded automatically when there is an eruptive projectile. However, due to the limited time resolution and the field of view, NoRH cannot detect vary fast or very slow eruptive events, simultaneous events, and events where the structure has a weak brightness. Fig 2 This is an image taken by the NoRH (M. Shimojo) which is an example of a prominence eruption, recorded by the automatic limb detection method. The panels are negative images, so the dark region indicates the high temperature. NoRH uses the radio interferometer to create images of the Sun such as in ‘Fig 2,’ which is an example of use of the automatic limb detection method to record images of prominence eruption. Data recorded from the NoRH automatic limb detector has also been made public through online databases, giving a further set of images that can be analysed in order to extract information on prominences and their reactivation. 4 Conclusion The topics covered in the papers that were researched lead to an adequate proposal of how to investigate the reactivation of prominences. Using NoRH and AIA data from SDO, the radio bursts emitted during the collapse and reformation of a prominence, an idea of what causes the reformation can be found. The investigation will centre on the different models, primarily the magnetic flux rope model, and the magnetohydrodynamics behind them that have been proposed for the formation of prominences, and how these models could support the ‘feed-back’ theory. 5 References J. P. Wild, H. Zirin. On the Association of Solar Radio Emission and Solar Prominences (1956) 320, 322, 323 G. Swarup, P. H. Stone, A. Maxwell. The Association of Solar Radio Bursts With Flares and Prominences. Radio Astronomy Station of Harvard College Observatory (1959) 725,726 R. F. Wilson, K. R. Lang. Impulsive Microwave Burst amd Solar Noise Storm Emission Resolved with the VLA. Department of Physics and Astronomy (1989) 856, 864, 866 J. A. Linker, R. Lionello, Z. Mikic. Magnetohydrodynamic Modeling of Prominence Formation with a Helmet Streamer. Science Applications International, California (2001) A. O. Benz, H. Perret, P. Saint-Hilaire, P. Zlobec. Extended Decimeter Radio Emission After Large Solar Flares. Institute of Astronomy, Switzerland (2005) 954, 955 J. Chaf, Y. Moon, Y. Park. The Magnetic Structure of Filament Barbs. (2005) 574-578 J. P. Raulin, A. A. Pacini. Solar Radio Emissions. Universidade Presbiteria Mackenzie (2005) 741-745 M. Shimoji, T. Yokoyama, A.Asai, H. Nakajima, K. Shibasaki. One Solar-Cycle Observations of Prominence Activities Using the Nobeyama Radioheliograph 1992-2004. University of Tokyo, School of Science (2005) 85, 86 S. E. Gibson, Y. Fan. Coronal Prominence Structure and Dynamics: A Magnetic Flux Rope Interpretation (2006) 1-5 G. P. Zhou, J. X. Wang, J. Zhang. Two Successive Coronal Mass Ejections Drivin by the Kink and Drainage Instabilities of an Eruptive Prominence (2006) 1244 C. Chifor, H. E. Mason, D. Tripathi, H. Isobe, A. Asai. The Early Phases of a Solar Prominence Eruption and Associated Flare: a Multi-Wavelength Analysis. Department of Applied Mathematics and Theoretical Physics, Centre for Mathematical Sciences (2006) 966-968 P. F. Chen, D. E. Innes, S. K. Solanki, SOHO/SUMER Observations of Prominence Oscillations Before Eruption. Department of Astronomy, Nanjing University (2008) 4,5 M. Pick, N. Vilmer. Sixty-five years of Solar Radioastronomy: Flares, Coronal Mass Ejections and Sun-Earth Connection. Astron Astrophys Rev (2008) 6,7 D.H. Mackay, J.T. Karpen, J.L. Ballester, B. Schmieder, G. Aulanier. Physics of Solar Prominences: II – Magnetic Structure and Dynamics. Springer Science and Business Media (2010) 335-338 N. Labrosse, K. McGlinchey. Plasma Diagnostics in Eruptive Prominences from SDO/AIA Observations at 304 A. University of Glasgow (2011) 2-4 T. E. Berger, W. Liu, B. C. Low, SDO/AIA Detection of Solar Prominence Formation Within a Coronal Cavity. National Solar Observatory (2012) 1-4 D. J. Schmit, S. Gibson, M. Luna, J. Karpen, D. Innes. Prominence Mass Supply and the Cavity. Max Planck Institute for Solar System Research (2013) 1-5 A. K. Srivastava, B. N. Dwivedi, M. Kumar. Observations of Intensity Oscillaations in a Prominence-Like Cool Loop System as Observed by SDO/AIA: Evidence of Multiple Harmonics of Fast Magnetoacousic Waves (2013) 31
Wednesday, September 4, 2019
THE SELLING OF ORGANS: RIGHT OR WRONG :: Ethical Issues, Human Organs
I Introduction All humans have organs. The organ is very important to the humans because without organ humans will not be able to live well. At present, there are many actions that are done by irresponsible people to sell organs. Organ sales cases occur when a person sells or transfers an organ from one body to another body for the purpose of replacing the recipient’s damaged organ. There are thousands of people dying to buy a kidney, and thousands of people dying to sell a kidney because of the lack of organs availability. Lives should not be wasted, they should be saved. Indirectly, there are many reasons why they sell the organs, where the organs mostly sold to and consequences of selling human organs. II Body A Most of the countries have organ selling issues from poor people to rich people and from less powerful people to the most powerful people. 1 The country that sell the most number of organs is India and has become one of the largest country for human organs selling and transplants in the world. a Poor people in India usually sell their organs while they are still alive (Scheper-Hughes, 1998, para. 7). b India hospitals are under investigation by the government because of the illegal organ sales (Carney, 2007, para. 4). 2 People use the body for their own benefit but they cannot change the other bodies for its own interests. a People agree to sell their organs because of their benefit. i Poor families are desperate to send their son to University (Maconachy, 2007, para. 4). ii Most parents want their daughters to marry will be collecting money for a dowry to the groom and they had to sell their organs to make the exchange. B People usually sell their organs in an underground market for human organ around the world that is called blackmarket (Maconachy, 2007, para.1). 1 Most the donors came from middle class family who’s searching clients via the internet. (Maconachy, 2007, para.3). a They find the client from specific sites where most of people posted organ selling on that websites. b The meeting can arranged if the client agree to go through the procedure. c According to Kenichiro Hokamura, he was faced two choice whether to wait for the transplant or buy organ on the internet. i He buys the organ from Japanese broker in China and get the new kidney two months later(Coonan & McNell, 2006, para. 2). 2 In China, the government is trying to strike down the black market (Coonan & McNell, 2006, para.
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