SZABO Surname Meaning and Origin

SZABO Surname Meaning and Origin Szabà ³ is a common Hungarian occupational surname meaning tailor, or one who cuts or metes out. Surname Origin:  Hungarian Alternate Surname Spellings:  SABO, ZABO Fun Fact About the Szabo Surname Up until about the 17th century, Zabo was the most common spelling of the Szabo surname. Famous People With the Surname SZABO Laszlo Szabo - Hungarian chess grandmasterViolette Szabo (nee Bushnell) - decorated WWII female spyEcaterina Szabo - Romanian Olympic gymnastZachariah Szabo - American figure skaterDezsÅ‘ Szabà ³ - Hungarian writer Where Do People With the SZABO Surname Live? According to surname distribution data from Forebears, the  Szabo surname is by far the most prevalent in Hungary, where it ranks 3rd in the nation. It is also common in Slovakia, ranking 8th, followed by Romania (139th) and Austria (212th). Data from  WorldNames PublicProfiler  also identifies Szabà ³ as most prevalent in Hungary, by far, particularly in the Pest region. Genealogy Resources for the Surname SZABO Szabo Surname ProjectLearn about the Szabo DNA Surname Project at Family Tree DNA. Szabo Family Crest - Its Not What You ThinkContrary to what you may hear, there is no such thing as a Szabo family crest or coat of arms for the Szabo surname.  Coats of arms are granted to individuals, not families, and may rightfully be used only by the uninterrupted male line descendants of the person to whom the coat of arms was originally granted. SZABO Family Genealogy ForumThis free message board is focused on descendants of Szabo ancestors around the world. FamilySearch - SZABO GenealogyAccess over 1.9 million free historical records and lineage-linked family trees posted for the Szabo surname and its variations on this free genealogy website hosted by the Church of Jesus Christ of Latter-day Saints. SZABO Surname Mailing ListThis free RootsWeb mailing list for researchers of the Szabo surname and its variations includes subscription details and searchable archives of past messages. The Szabo Genealogy and Family Tree PageBrowse family trees and links to genealogical and historical records for individuals with the last name Szabo from the website of Genealogy Today. References Cottle, Basil.  Penguin Dictionary of Surnames. Baltimore, MD: Penguin Books, 1967.Dorward, David.  Scottish Surnames. Collins Celtic (Pocket edition), 1998.Fucilla, Joseph.  Our Italian Surnames. Genealogical Publishing Company, 2003.Hanks, Patrick and Flavia Hodges.  A Dictionary of Surnames. Oxford University Press, 1989.Hanks, Patrick.  Dictionary of American Family Names. Oxford University Press, 2003.Reaney, P.H.  A Dictionary of English Surnames. Oxford University Press, 1997.Smith, Elsdon C.  American Surnames. Genealogical Publishing Company, 1997.

5 Free Assessment Apps for Teachers

5 Free Assessment Apps for Teachers Teachers are always looking for new ways to assess their students work. Regardless of what curriculum you teach, assessment is something that teachers must do every day, even informally. Thanks to the latest in mobile technology, assessing students work has never been easier! Top 5 Assessment Apps Here are the top 5 assessment apps that will assist you in observing and assessing your students. Nearpod The Nearpod app is a must-have application if your school has access to a set of iPads. This assessment app has been used by over 1,000,000 students was awarded the Edtech Digest Award in 2012. The best feature of Nearpod is that it allows teachers to manage content on their students devices. Heres how it works: First the teacher shares content with their students, through materials, lecture and/or presentation. This content is then received by the students on their devices, and they are able to participate in activities. Then teachers are able to access students n real time by seeing the students answers and having access to post-session activity reports. This is by far one of the best assessment apps out on the market today. A Spelling Tests The A Spelling Tests app is a must-have for all elementary classrooms. Students can practice their spelling words, while teachers can track how they are doing. By each spelling test, students and teachers can see their results. Other great features include the ability to instantly see if you are right or wrong, unscramble mode to help sharpen spelling skills, and the ability to submit tests through email. GoClass App The GoClass app is a free iPad application that allows users to create lessons and share them with their students. Documents can be broadcasted through student devices and/or by projector or TV. GoClass allows users to formulate questions, draw diagrams, and share materials with students in the class. Teachers can also keep track of what students are using which lessons, and when they are using them. To check for student understanding, the teacher can post a question or poll and get immediate feedback. This will help the instructor tailor his/her lessons to make sure all students are understanding the concept that is being taught. Teacher Clicker If youre looking for a way to engage students while getting results in real time, then Socrative made this mobile app for you. Not only does this app save you time, but it will grade your activities for you! Some features include the ability to: ask open-ended questions and get real-time answers, create a quick quiz and receive a report with the quiz graded for you, have students play a fast-paced space race game where they answer multiple choice questions and you receive a report of their graded answers. There is a separate app called Student Clicker that must be downloaded for students tablets. MyClassTalk MyClassTalk was designed to assess students participation in the classroom. With just a tap of your finger, you can easily award points and rank students class participation. Users can even upload students photographs for an even better visual. Forget about writing names on the board for not participating, this easy-to-use app is all you need. Additional Assessment Apps Worth Mentioning Here are a few more assessment apps that are worth checking out: Edmodo - This is a great app for assigning quizzes and collecting homework.ClassDojo - If youre looking to assess student behavior this is a great app.Easy Assessment - Rubric Creation - This costs $1.99 but you can easily create a rubric in two steps.

Choose a country, which underwent a recession, and where fiscal and Essay

Choose a country, which underwent a recession, and where fiscal and monetary policies were used to overcome the recession - Essay Example It is said to be integral in a free trade economy. The United Kingdom recession of 1981 was a result of the monetary strength which in turn affected manufacturing and by the government’s policy to reduce its past inflation of 27%; they enforced a stringent monetary policy by impeding their borrowing. Taxes were increased and the consumer’s purchasing power was diminished resulting to a downfall in spending. After a decade, in 1991 a ‘boom and bust’ of the UK economy ensued. Growth was seen at rapid growth that became unsustainable that inflation rose to 10%. Again, government set in and imposed interest rates to halt the people’s spending. These interests had a domino effect as it affected mortgage consequential to foreclosure of housing loans or sell thereof (EconomicsHelp, n.p.). Recession is a phase of the business cycle usually following a peak. It is a period characterized by a decline in the total output, income, employment and trade. This econ omic downturn is also marked by the widespread contraction of business activity in many sectors of the economy. But because many prices are downwardly inflexible, the general price level is more likely to fall only if the recession is severe and prolonged. If an economy fails to recover from a recession, then a depression occurs (McConnell and Brue, 134). The economy of the United Kingdom is no exception for these economic recessions as they already experienced and recovered from recessions several times. What is apparent in today’s economy is that it has a global characteristic which has a worldwide effect among interdependent countries. Many believe that a plummet in Real GDP will ultimately affect employment. In the Great Depression of the 1930s which included the UK, the famous economist Keynes debunked this concept and contended that negative output over a period will not necessarily clear out on its own as was regarded by the notion of the self-correcting aspect of a fr ee economy. He cited that there are four reasons for this; first, â€Å"Firms should cut wages to reflect lower prices but in reality workers are very resistant to cuts in nominal wages,† second, â€Å"2. If wages were cut in response to unemployment workers would have less spending power therefore AD would continue to fall,† and third, â€Å"In a recession people have low confidence and therefore spend less. Keynes said this was the â€Å"Paradox of Thrift† (EconomicsHelp, n.p.). In typical years, gross investment or all the country’s investment goods - both that replace machinery, equipment, and buildings that were used up or worn out or just made obsolete in producing the current year’s output and any net additions to the economy’s stock of capital exceeds depreciation or the amount used up over the course of a year (McConnell and Brue, 116). During these years, the net investment is positive and there will a recorded rise in nation†™s stock of capital. However, if gross investment is less than depreciation, net investment will be negative. This means that the economy is disinvesting because it is using up more capital than it is producing. When this happens, the nation’s stock of capital will shrink. When capital shrinks, the economic activities will also decline or slow down. This is what happened in the Great Depression of 1930s and its effects were felt by all countries across the world. Banks play important role in an economy. They act as intermediary between the producing and the consuming units. Banks take in leakages in

MARKETING COMMUNICATIONS (Paragon Software Ltd) Assignment

MARKETING COMMUNICATIONS (Paragon Software Ltd) - Assignment Example The report will also explore the other marketing communication tools that can be used together with exhibition to promote the sales. Marketing communication can be described as the process which attempts to advance the interests of the company, product range or the brand. It comprises of the following elements; personal selling, sales promotion, advertising, public relations, and direct marketing. The main purpose of marketing communication is to persuade the customer (Kimmel 2005, p1). Exhibitions are very vital elements in the marketing communication strategies. These exhibitions have advantages and disadvantages. Exhibitions assist the organization to create relationships with the stakeholders on the basis of meeting face to face. There are varied reasons as to the use of exhibitions in an organization. Exhibitions come in three forms and each form aims at a certain group within the market; the consumer, the trade and both the trade and the consumer. The last category (exhibitions aimed at both the consumer and the trade) is the most common form of exhibition. Majority of the exhibitions begin as a trade exhibition and after a week or so, they become open to the public. A fee is paid by the public for entry into the exhibition. The fee is a source of revenue for the company. Most of the times, the products in the exhibition are of little or no interest to the public, thus, they may not purchase the products (Lancaster n.d., p1). Exhibitions can produce sales lead for the company. Immediate sales are achievable because the buyer comes to the trade fairs. New contacts of a business nature are made with the customers and even with the competitors. Positive media coverage is enjoyed by the organization through exhibition (Donaldson and Smit 2007, p86). Exhibitions at times are considered as a promotional activity. Exhibitions are encompassed within the trade shows and trade fairs. These trade shows perform two functions; non-selling and selling

New Potential Class of Long Gamma-Ray Bursts

New Potential Class of Long Gamma-Ray Bursts Intro Since their discovery, a debate has been sparked over the classification of a new potential class of long gamma-ray bursts (LGRB) that possess ultra-long durations lasting at least 1000s, along with distinctly different x-ray and optical light curves to regular gamma-ray bursts (GRB) (Levan 2014). The search for members of the ultra-long gamma-ray burst (ULGRB) population is currently gaining traction, with some suggesting they may be commonly occurring despite difficulties detecting them (levan 2014) and that their origins may be uniquely different from regular LGRBs (Boer 2015). It is thought that ULGRBs are produced by stars of very large radii evolving into an engine driven super-luminous supernova (SLSN), rather than an envelope stripped compact Wolf-Rayet star which is commonly accepted as a progenitor for LGRBs (levan 2014), however, the connection between SN signatures and ULGRBs is an ambiguous one. More recent work has been centred on exploring this partially vague connection, attempting to refine models explaining an engine driven SLSN, the nature of their progenitors and the host galaxy properties (bersten, kann, japlj, gao). The focus of this work is on two papers in this area of astrophysics: A very luminous magnetar-powered supernova associated with an ultra-long gamma-ray burst, (Greiner) and The Diversity of Transients from Magnetar Birth, (Metzger). The former details the discovery and observational analysis of SN2011k, preceded by GRB111209A, and postulates a magnetar origin, whereas the latter acknowledges the ULGB-SLSN connection and builds a thorough model of magnetar formation in order to explain it. A very luminous magnetar-powered supernova associated with an ultra-long gamma-ray burst Summary The work performed by (greiner) at first focuses on observational data of GRB111209A taken with GROND, a 7-channel imager specifically designed for rapid observations of GRB afterglows that performs simultaneous imaging in the Sloan grIz and near infra-red JHK bands. Use of the GROND imager gives the authors the ability to calculate multiple properties of the GRB, such as photometric redshift, the intrinsic power law slope of the continuum emission, and the galactic host emission, which can all be done in a short window and   monitored as the GRB afterglow evolves (greiner 2008). z΄ GROND was used on 16 epochs with logarithmic temporal spacing until 72 days after the GRB was detected by the Swift satellite on December 9 2011; however, readings were interrupted by the Sun until 280 days after detection when a final epoch for host photometry was obtained. There is also inclusion of supplementary observations of the GRB afterglow: u-band observations from Swift with applied UVOT photometry; HST F336W/F125W data from 11.1 and 35.1 days after the GRB, respectively; two epochs of VLT(X-shooter)/FORS2 g΄RCi΄z΄ data during the SN phase; a late-time Gemini-S u΄-band observation 198 days after the GRB. Data tables for all GROND and Swift data can be found in Appendix A. GRB111209A was measured to last ~10,000s at a redshift of z=0.677, and to have an equivalent isotropic energy output of Eiso = (5.7à ¯Ã¢â‚¬Å¡Ã‚ ±0.7)à ¯Ã¢â‚¬Å¡Ã‚ ´1053 erg which is among the brightest of LGRBs. After analysis of the VLT/X-shooter spectrum, obtained near the peak of excess emission and detailed below, (greiner) deduces this emission to be caused by a SN, dubbed SN2011k1, because of similarities in spectral shape to known GRB-SNe and development in time and colour. Decomposition of the GRB afterglow is shown in figure 1 which displays data from GROND and other instruments. Since the authors accurately determined the host galaxy emission, they were able to subtract it from the GRB afterglow. The optical light curve displays a deviation from its initial power law decay, remaining flat for around 15 days, before decaying again. They also plot the light curve in the u-band showing a steeper decay slope >10 days where the initial slope is a1.. and the second a2 Since there is no contribution from the associated SN in the u-band, they explain that they can build a template for the pure afterglow contribution from the SN. The authors construct a quasi-bolometric light curve for the SN from GROND and supplementary data by first extinction-correcting filter band with Avà ¢Ã¢â€š ¬Ã‚ ¦, galactic foreground, and Avhostà ¢Ã¢â€š ¬Ã‚ ¦ which was derived from the GRB afterglow spectral energy distribution, then secondly deriving quadratic polynomials for sets of 3 consecutive filters, which were combined to form the light curve.   They then integrate the polynomials over rest-frame wavelength from 3860/(1+z) Ã… to 13560/(1+z) Ã…, corresponding to the blue limit of the g-band filter to the red limit of the J filter, and used k-correction computed from the spectral energy distribution. Finally, they transformed the integrated flux into luminosity (figure 2), employing a luminosity distance of d=4080 Mpc, using concordance cosmology (à ¯Ã‚ -à ¯Ã‚ Ã…’=0.73, à ¯Ã‚ -m=0.27, and H0=71 km sà ¯Ã¢â€š ¬Ã‚ ­1 Mpcà ¯Ã¢â€š ¬Ã‚ ­1) Using data from the VLT/X-shooter spectrum, which is the sum of light from the GRB afterglow, the GRB host galaxy, and the supernova SN 2011kl and taken near the SN peak, (greiner) again subtracts the GRB and host contributions followed by rest-frame conversion and correction for intrinsic reddening of E(Bà ¯Ã¢â€š ¬Ã‚ ­V)=0.04à ¯Ã¢â‚¬Å¡Ã‚ ±0.01 mag. They use this data, shown in figure 3, to draw similarities between SN2011k1 and SLSN, noting that its flat shape and high UV flux is clearly different from the brightest known GRB-SNe. When comparing this spectrum (figure 3) to the GRB afterglow, they find that there is no change in absorption lines or redshift and that they are similar to those found in hosts of LGRBs, thus relating SN2011k1 to the same galaxy as GRB111209A. Also mentioned in this comparison is that there is no offset between the GRB afterglow and SN images, which the authors say implies the events are co-spatial to within Spectral analysis of SN2011k1 reveals very low metal content and lack of H or He, unlike typical SNe Ic associated with LGRBs, therefore, (greiner) apply parameterized SN light curve fits to derive an ejecta mass Mej = 3à ¯Ã¢â‚¬Å¡Ã‚ ±1 Mà ¢Ã…  Ã¢â€ž ¢ and a 56Ni mass of 1.0à ¯Ã¢â‚¬Å¡Ã‚ ±0.1 Mà ¢Ã…  Ã¢â€ž ¢ for photospheric velocity vph = 20,000 km/s, and a grey opacity of 0.07à ¯Ã¢â‚¬Å¡Ã‚ ±0.01 cm2 gà ¯Ã¢â€š ¬Ã‚ ­1. The high Ni/Mej ratio is reported to be incompatible with the spectrum (figure 3) and thus the authors seek an alternative explanation for the luminosity source. The likeness of SN2011k1 to SLSNe, its host galaxy properties, low metal abundance, improbable Ni powered luminosity and association with GRB111209A lead to the authors to suggest a magnetar origin for this event, stating that post-birth from the collapse of a massive star it powers the surrounding ejecta for a super-luminous effect. This hypothesis is evidenced by reproducing the SN spectrum via sampling of   magnetar initial spin period Pi, magnetic dipole field strength B, Mej and rotational energy Ek. Best fits to the data found P=12.2à ¯Ã¢â‚¬Å¡Ã‚ ±0.3 ms and B=7.5à ¯Ã¢â‚¬Å¡Ã‚ ±1.5à ¯Ã¢â‚¬Å¡Ã‚ ´1014 G for observed short tpeak (à ¯Ã‚ Ã‚ ¾14 rest-frame days) and moderate peak luminosity, as well as Mej=2.4 ±0.7 Mà ¢Ã…  Ã¢â€ž ¢ and energy EK=(5.5à ¯Ã¢â‚¬Å¡Ã‚ ±3.3)à ¯Ã¢â‚¬Å¡Ã‚ ´1051 erg. Importance and Implications The significance of this paper arises from its robust analysis of the GRB111209A afterglow and SN2011k1 using multiple datasets on top of their own data, collected with GROND. It is clear that the development (g2008) and implementation of this instrument is extraordinarily useful in this area of observational astrophysics due to its multiple measurement taking capabilities. Without this device, it is unlikely the authors could have developed their results as well as they have done, despite much of their comparison data coming from other sources, such as the ESO VLT/X-shooter. On the note of observational data analysis, there are a few important points to consider underneath the various statistical methods and rebinning mentioned in this paper. It is explained that the SN light curve error depends on the decay slope a2 remaining constant after the last afterglow measurement before onset of the SN, and since the GRB light curve is observed to steepen, the authors claim their SN luminosity measurement of 2.8+1.2-1.0 x 1043 erg/s is in fact a lower limit. They also explain that they lack any near-infrared measurements for SN2011k1, acknowledging that the bolometric peak luminosity could be underestimated by 5%-30%. A crucial achievement from this paper is that a SN with such high bolometric peak luminosity was detected, not only within the same host galaxy, but to within Evidently the authors are confident that neither the GRB is caused by a tidal disruption event, or that the unusual SN spectrum and luminosity is caused by 56Ni brightening and hence distancing it from SNIc. The former is explained by the lack of ejecta and fall back accretion time being too short to produce an ULGRB, and the latter simply by the overly large amount of 56Ni needed to reproduce the spectrum of SN2011k1. Formation and subsequent accretion of matter on a black hole is also rejected, leaving the authors to suggest the birth of a magnetar as the cause, and as seen in fig 2 their model reproduces the quasi-bolometric spectrum of SN2011k1 rather well without invoking any 56Ni interaction. Critical Assessment This paper is difficult to follow for a number of reasons. The layout is most unusual for a scientific report; it presents the abstract, which is well written and informative, then without a section heading proceeds to give a few paragraphs summarising their observational findings, with some values then absent in crucial places throughout the remainder of the work. These paragraphs are followed by a qualitative description of their interpretations for an origin of GRB111209A and SN2011k1 and their modelling of magnetar SN enhancement, in attempt to draw connections. At the end of this section, they suggest that the events could have been caused by formation of a magnetar which then lives on to power SN2011k1, and up to this point they make a good argument. The problem with this argument is that it is devoid of any mathematical content, and all the data provided is in the three graphs included in this work or essentially contained in references to other papers, making it difficult to decipher which parts (greiner) did themselves, or how they did it. The captions for each figure are also all on separate pages to the figures, located after the end of the untitled section and a collection of references. Beyond this point is a Methods section with seven 7 subsections, each with their own title and even some supplementary data to explain the origin of their work. Unfortunately, this part of the paper feels cyclical and can often feel at odds with methods they had already discussed. For example, they talk about subtracting the host galaxy emission from most of the light curves, but at multiple points in between mention they firstly have to build a template for the emission, which is detailed in a later section to be constructed from GROND data and using LePHARE . Again, there is a complete lack of mathematical clarity on their methods, however, it appears that the majority is all computational statistics performed on their copious data sources or modelling techniques. Even when discussing the origin for their magnetar properties, they give a simple qualitative explanation which should probably have been accompanied by some mathematics. When all of this is put together, it makes for an excruciatingly difficult read. There are inconsistencies everywhere in its presentation and in some comments of the work, making one wonder why they would read it again. Despite (greiner) providing some outstanding results and performing brilliant analysis on the afterglow of GRB2011k1 and spectrum of SN2011k1, the details of their work is lost to disorganisation. The Diversity of Transients from Magnetar Birth Summary This paper takes an approach to modelling physical properties of highly magnetized, millisecond rotational neutron stars, known as magnetars, in order to unify ULGRBs and SLSNe in a common framework. The authors intend to show that under their model, both of these events can be explained individually with a magnetar central engine and simultaneously via magnetar formation, as well as stating that the transition from ULGRBs to SLSNe is a natural consequence of the model. They focus on the observations of GRB111209A and SN2011k1 as a benchmark since the pair were found to be closely associated events, whilst also including various observational signatures of magnetar formation. Also discussed is the SLSN, ASASSN-15lh, which has the highest recorded peak luminosity of à ¢Ã¢â€š ¬Ã‚ ¦ (very recently it has been suggested to be a tidal disruption event (leloudas)). This event challenges the magnetar central engine model because of its extreme energy peaks, however, the authors go on to sh ow that the maximum energy output from magnetars was previously underestimated and hence fit ASASSN-15lh within their model. The proto-magnetar spin-down energetics used in the model were given as follows: firstly, the rotational energy of a magnetar with mass is where is the NS moment of inertia and is the rotational period. The rate which the NS loses rotational energy for an aligned force-free wind is given by is the spin-down luminosity, the NS magnetic dipole moment and is the surface equatorial dipole field, with a radius 12 km and is the initial spin-down time. The authors note that, although the correction is minor for ULGRBs, the spin-down luminosity given in equation eqref{2} is exceeded for a few seconds after core bounce due to neutrino-heated wind. (Metzger) secondly consider the constraints on the GRB jet collimation and how the NS properties described by the above equations can be translated to derive opening angle conditions for observed peak luminosity. Though a stable jet may be formed, it may not cleanly escape the star over time, tsd, of peak spin-down power. This is because there is uncertainty over whether the strong toroidal magnetic field in the nebula, separating the magnetar wind from the surrounding star, remains stable in the case of non-asymmetric instabilities. It is required, for a jet of luminosity Lj and half opening angle à ¢Ã¢â€š ¬Ã‚ ¦, that tesc Where (Metzger) assume Erot=à ¢Ã¢â€š ¬Ã‚ ¦ since the kinetic energy of the explosion is dominated by the magnetar rotational energy. A cleanly escaping jet will then have a peak spin-down luminosity of Lj=.., implying that the observed isotropic gamma-ray luminosity is Liso=.., where e= is the radiative efficiency and fb=.. the beaming fraction. The authors state that, assuming the propagation time through the star is negligible, we can expect the GRB duration, Ty, to be such that Ty=.. Lastly, the authors describe how SN mass ejecta, Mej, thermalizes over time through adiabatic expansion and 56Ni decay (the standard process for type Ic SNe), which is enhanced by input from the NS to super-luminous levels. The thermal energy E evolution over time t as the ejecta expands is given by For an initial kinetic energy of Eokà ¢Ã¢â€š ¬Ã‚ ¦ , where the LHS accounts for PdV losses, vej=.. is the ejecta velocity and rej the mean radius. Conservation of energy requires that the kinetic energy Ek=à ¢Ã¢â€š ¬Ã‚ ¦ increases due to the work done from PdV, thus dEk=à ¢Ã¢â€š ¬Ã‚ ¦ Lsn=à ¢Ã¢â€š ¬Ã‚ ¦ is the radiated luminosity, where td=.. is the photon diffusion timescale, with k=à ¢Ã¢â€š ¬Ã‚ ¦ the optical opacity which is set by electron scattering and Doppler broadening lines. Lni=à ¢Ã¢â€š ¬Ã‚ ¦ is the rate of heating due to 56Ni decay where Mni is the 56Ni mass. The final term is the energy input from the magnetar which is assumed to thermalize the ejecta with unity efficiency.

The Presentation of Self in Everyday

In his book, The Presentation of Self in Everyday Life, Erving Goffman compares life to acting. He argues that â€Å"when the individual is in the immediate presence of others, his activity will have a promissory character† (Goffman 2). I think it is ironic because I always thought that movies or theaters have always tried to imitate reality and not the other way around. In order to clearly show his analogy, Goffman presents elements of acting such as the front. We are all familiar with the term front act.† In Goffman’s opinion, people are all playing an act. This is such a bold claim to make because he is saying that we are all just performing and not being our real selves, though there are some truths to his claim. What is confusing is when do we really act, or when do we be ourselves? Most of us would not acknowledge his belief that we are playing a character, but then again, the person that denies this may also just be playing a role, and so the question remai ns unanswered.One idea of Goffman that caught my attention is his theory that people cooperate in an act to cover, say, something embarrassing. I have experienced it myself—I would pretend that I have not witnessed someone undergo an embarrassing moment, although unconsciously, I was not trying to make that person feel the embarrassment more, but rather, I was just trying not to be mean.It did not occur to me that by pretending (and therefore joining in the scene, or rather excluding myself from the scene) not to see the embarrassing act, I have helped in saving that person’s face. What follows is an array of lectures, as it were, like that of a professor teaching a theater or film student, only that his lectures are philosophical and are related to our everyday lives. After reading Goffman’s work, I found myself smiling because of the truths in his analogies that never crossed my mind before.

Example Of The Medicaid Benefits - 1046 Words

They are expected to pay a portion of their health care costs. Keep in mind though that these are elderly and disabled citizens, usually on fixed and very limited incomes. These Medicare members will always more than qualify for Medicaid benefits. The Medicaid program differs by state. There are dozens of ways to qualify for this state and federally funded health insurance program. There are Medicaid programs for the low-income, disabled, elderly, children, and long-term care. â€Å"Since its inception in 1965, the Medicaid program has evolved to become the largest single source of health coverage in the United States† (Crowley Golden, 2014). From its beginnings the goal of single payer health care is on a slow roll for all citizens. Some†¦show more content†¦Private Insurance Private insurance is a way to help mitigate the rising cost of health care in the US. Health care and health insurance get used interchangeably in the US but they are vastly different. Pri vate insurance is generally paid by a combination of employer and employee contributions. This helps reduce the impact of the cost of health care for those who have it. The analogy that researchers use is that the stereotype is that a privately held hospital will assist you much better because they have the money to do so. A nonprofit hospital will be less beneficial in treating patients because they lack the equipment and staff to do so. This article argues that nonprofit organizations can be inferior to for profit, even if markets are incomplete. This is beneficial to the paper because it will show the structure financially what privately and non- profit hospitals must offer (Kessler, McClellan, 2002). The profit that private insurance creates supports the economy and continues to help invocation in treatments. However private insurance does not cover all of the cost of health care. Research shows that â€Å"US adults’ exposure to costs results from insurance benefit gaps as well as a high percentage of adults without insurance. Adults who had been insured the entire previous year were about as likely to spend US$1,000 or more as were those who had been uninsured. Among US adults under age sixty-five, 38 percent ofShow MoreRelatedThe Oregon Health Services Commission1647 Words   |  7 PagesThe Oregon Health Services Commission addressed budget cuts in 1990 by proposing a list of Medicaid services. The list was ranked by priority, based on a cost-effectiveness analysis. Access to particular services became limited, but coverage was increased from 67% to 100% of the poverty line1. Much protest broke out in regards to how the treatments were prioritized on the list. 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