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

8 Common Types of Computer Viruses Essay

Dictionary.com defines a computer virus as â€Å"a segment of self-replicating code planted illegally in a computer program, often to damage or shut down a system or network (â€Å"Virus,† 2012).† The term virus has become more generic over the years and has come to represent any type of malware, or malicious software. There are many types of malware that can be classified as viruses but it is the intention of this paper to examine 8 of the most common types. These types are virus, worms, trojans, adware/pop-up ads, spyware, keyloggers, rootkits, and scareware. * Virus- as defined above, a virus is self-replicating code planted in a computer program. This malware’s sole purpose is to destroy or shut down systems and networks. (â€Å"Virus,† 2012). * Worms- These are standalone programs whose sole purpose is to replicate and spread themselves to other computers. Their main use is to search for and delete certain files from computers. * Trojans- This malware is designed to look like a useful program while giving control of the computer to another computer. It can be used for several malicious things: * As part of a botnet to use automated spamming or distribute denial-of-service attacks. * Electronic money theft * Data theft * Downloading or uploading of files to the computer * Deletion or modification of files * Crashing the computer * Watching the viewer’s screen * Anonymous internet viewing * Adware/pop-up ads- â€Å"The definition of adware is a software package which displays or downloads advertisements to a computer. These ads are usually in the form of pop-ups, and the goal of adware is to generate revenue for its author. In itself, adware is harmless, however, some of it may come integrated with spyware (What is the definition of adware? 2012).† * Spyware- Malware used to collect information about a user’s browsing habits  or to intercept personal data. (â€Å"Spyware†, 2012). * Keylogger- Using dedicated software or implanted hardware, this malware covertly monitors and records every keystroke made on a remote computer. (â€Å"Keylogger†, 2012). * Rootkits- â€Å"A rootkit is a collection of tools (programs) that enable administrator-level access to a computer or computer network.† â€Å"A rootkit may consist of spyware and other programs that: monitor traffic and keystrokes; create a â€Å"backdoor† into the system for the hacker’s use; alter log files; attack other machines on the network; and alter existing system tools to escape detection. (â€Å"Rootkit†, 2012) * Scareware- This is a class of malware that represents itself as antivirus software even though it is fake. It is used primarily to scam people into purchasing it but in most cases it does not actually do anything. Sometimes it will contain another piece of malware that it injects into the computer system. References Virus. (2012). Virus. Dictionary.com Retrieved from http://dictionary.reference.com /browse/virus. Spyware. (2012). Spyware. Dictionary.com Retrieved from http://dictionary.reference.com /browse/spyware. Keylogger. (2012). Keylogger. Dictionary.com Retrieved from http://dictionary.reference.com /browse/keylogger. Rubenking, Neil J. (2010) â€Å"Antivirus, and much more: when most people talk about antivirus software, they’re really talking about an app that blocks spyware, rootkits, keyloggers, scareware, Trojans, and more–not just viruses. We review 13 antivirus apps that do just that.† PC Magazine : 72+. Retrieved from http://go.galegroup.com.proxy.itt-tech.edu/ps /i.do?id=GALE%7CA226958047&v=2.1&u=itted&it=r&p=CDB&sw=w. What is. (2012). What is the definition of adware? DirectHit.com. Retrieved from http://www.directhit.com/shopping-answers/what_is_the_definition_of_adware?oo=0 Different Types. (2012). Different types of computer viruses. Buzzle.com. Retrieved from http://www.buzzle.com/articles/different-types-of-computer-viruses.html Rootkit. (2012). Rootkit. SearchMidmarketSecurity. Retrieved from http://searchmidmarketsecurity.techtarget.com/definition/rootkit Scareware. (2012). Scareware. Ask.com. Retrieved from http://www.ask.com/wiki/Scareware

How has life changed since 1800? Essay

Life as we know it today in the modern world, is significantly different to the lives that our predecessors lived during the period 1500-1800. The changes across the centuries are the result of a process of advancements over time. This essay will examine life in the period 1500-1800 as highlighted in the work of George Blainey (2000) and will compare key differences of life in this early period, against life in the modern world today. Throughout this essay, the main focus will be based on three areas which have seen significant change over this period of time: the production of food, work practices and the standard of living. The advancements in these three areas, has led to societies living very different lifestyles in the current modern times. Day to day life in the period 1500-1800 revolved around hunting, collecting and cultivating food in order to survive. Grain made up 80% of most people’s diet and was used to make bread, beer, damper or gruel and in particularly lean ti mes, was mixed with water to relieve hunger (Blainey 2000, p. 410). Bread and beer were the basis of most people’s diet. Bread was so important to everyday survival that a baker could be hanged for selling an underweight loaf of bread. Blainey (2000) describes a life where most families owned no land, or if they did, it tended to be too small to sustain their food needs. The main priority was to provide enough food to feed their small communities and everyone, including women and children had to assist in this. As highlighted by Blainey (2000), most people worked on the land and the majority of work revolved around the production of food. Successful grain harvests were imperative to survival and everybody had to work together to reap, bind, carry and store the harvest. Woman and children did much of the rural work, such as weeding, carting water, spinning fibres, brewing beer, gathering firewood and making clothes. Many men as well as unmarried woman, left their own small farms or communities to go and work on larger farms or at different trades, which often incorporated meals as part of their payment (Blainey 2000, p. 409). While these workers could be sure of not going hungry, this meant the take home wages were low. Living standards as described by Blainey (2000) were bleak. Most people lived in one roomed,  small stone houses, often with four or more sharing one bed. Homes often remained unheated due to scarcity of wood (Blainey 2000, p. 423). People were largely uneducated and knew little about healthcare. Sewerage was disposed of in the same rivers that were used to drink and wash from. These contaminated rivers were used to supply water to the growing crops. This had a huge impact on health, causing infection in around two out of every three people in rural areas (Blainey 2000, p. 415). Lack of hygiene and knowledge of healthcare led to shorter lifespans. Life today in 2014 is vastly different to the period 1500-1800 as described by Blainey (2000). Survival no longer hinges on hunting and gathering food. In fact many people today give little or no thought to food production. Instead, we drive to a supermarket and buy whatever we want to eat. We have access to many restaurants and fast food outlets, so we not only have ample food at our fingertips, we don’t even have to prepare it if we choose not to. Advancements in production and using machines in place of humans (Henslin, Possamai and Possamai-Inesedy 2011, p. 139) mean food is now farmed and produced on a much larger scale (Macionis and Plummer 2012, p. 113), this has freed people up to work in other areas. Now that people are not tied to working to produce food to survive, they have more time to get educated and learn new skills. Work in modern times has moved away from farming. Today’s society is an industrial and information based one that revolves more around accumulating wealth and material possessions (Henslin, Possamai and Possamai-Inesedy 2011, p. 140). Woman as well as men, work outside the home in many different varied jobs, and children attend school. This is immensely different to life as discussed by Blainey (2000) whereby woman and children were home working on the land while men worked tending the harvest and work all revolved around food production. Living standards in today’s world are likewise very different than the period Blainey (2000) describes. In modern societies, many people live in homes that are large, with many rooms, furnished and full of material possessions. These homes often have heating and cooling at the push of a button, along with toilets, showers, clean running water and pantries stocked with food. They have warm beds to sleep in at night and clothing to wear that they don’t have to make themselves. Amongst their many possessions, people have cars to get where there want to go and televisions to watch. There are computers and mobile  phones to keep in touch with family and friends. There are health systems and education available to many societies. It is much more common for people to own their homes in these more modern times, (Henslin, Possamai and Possamai-Inesedy p. 140) along with other possessions such as cars. In conclusion, life in modern times is very different than life was in the period 1500-1800. People from the period 1500-1800 worked to produce food to survive. People lived in poverty, ill heath was common, as was hunger. Advancements in technology have made this a thing of the past in many areas, although there are still societies where poverty does still exist. Although the world in the period 1500-1800 as described by Blainey (2000), was a great deal tougher than modern society, it was much less complicated than the world of today with all its technology. Many people live a privileged life these days, however today’s societies have lost a lot of the family closeness of working together that those in the period 1500-1800 had to have to survive. Progress will continue as the years go on, bringing with it both good and bad consequences. References Blainey, G 2000, A Short History of the World, Viking, Ringwood. Henslin, J, Possamai, A & Possamai-Inesedy, A 2011, Sociology: A down-to-earth approach, Pearson, Frenchs Forest NSW. Macionis J & Plummer, K 2012, Sociology: a global introduction, 5th edn, Pearson Prentice Hall, Harlow. Povos Indigenas no Brasil n.d., Yanomami family, digital image, viewed 22 November 2014, .

Fire And Water Facing Your Fears And Crossing Your...

Alexander Lattin Mrs. Lee English 10 3 March 2014 Fire and water: Facing your Fears and Crossing your Boundaries â€Å"You gain strength confidence and courage by every experience in which you stop and really take the time to stop and look fear in the face† (Eleanor Roosevelt) Fahrenheit 451, by Ray Bradbury, and The Truman Show both present the trials but the overall triumphs of Truman and Montag and their journeys to victory. While exploring and pondering upon the text, Fahrenheit 451, by Ray Bradbury, certain themes appear that connect to The Truman Show which together suggest that knowing your fears and boundaries is certainly normal, yet it’s essential to not allow those fears and boundaries prevent you from knowing, discovering or†¦show more content†¦Montag is on a fire call, drowning books in kerosene, this routine is familiar, then Montag does something he knows he shouldn’t have, in fact, Beatty was just around the corner. â€Å"Montag’s hand closed like a mouth, crushed the book with wild devotion, with an insanity of mindlessness to his chest† (Bradbury 34). Montag Fears fire because it burns books, it burns fantasy, he also knows that fire is an obvious boundary. He knows that taking a book is frowned upon by most of society. Regardless, he took the book because he was curious and hungry for knowledge. Having knowledge would allow him to realize how important, and wonderful things really are supposed to be, he could experience happiness. He overlapped his fears and went past his boundaries and that’s what made him take the book in the first place. He becomes so intrigued in solving the concealed reality he feels that he should reveal his position to others. Upon entering his living room Montag is disgusted by the stupidity of the opinions and the viewpoints of Millie and her friends. â€Å"Montag said nothing but stood looking at the women s faces as he had once looked at the faces of saints in a strange church he had entered when he was a child. The faces of those enameled creatures meant nothing to him, So it was now, in his own parlor, with these women twisting in their chairs under his gaze, lighting cigarettes, blowing smoke, touching