The Meaning of Method

Mackey, William F.

doi:10.1093/elt/v.1.3

Cited by 11 publications

(20 citation statements)

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“…Our results show good agreement with those obtained by Mackey et al (2016), and are in accordance with the general analysis of Henney & Arthur (2019b) for the case of a dust wave where the dust is decoupled from the gas. Indeed, the distribution of dust is mainly located in a region found immediately after the bow shock, as in the two works mentioned previously.…”

Section: Discussionsupporting

confidence: 91%

“…In both cases a partial shocked shell forms, upstream for the bow shock and in the lateral direction for the H II region, and can be unstable in certain circumstances. In the case of RCW 120, Mackey et al (2016) performed 2D radiation hydrodynamical numerical simulations of stellar wind bubbles and post-processing calculations to obtain synthetic intensity maps at infrared wavelengths. They found good agreement between their model and the RCW 120 observations.…”

Section: Introductionmentioning

confidence: 99%

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Numerical models for the dust in RCW 120

Rodríguez-González

Méliani

Sánchez-Cruces

et al. 2019

A&A

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Context. The interstellar bubble RCW 120 seen around a type O runaway star is driven by the stellar wind and the ionising radiation emitted by the star. The boundary between the stellar wind and interstellar medium (ISM) is associated with the arc-shaped midinfrared dust emission around the star within the HII region. Aims. We aim to investigate the arc-shaped bow shock in RCW 120 by means of numerical simulations, including the radiation, dust, HII region, and wind bubble. Methods. We performed 3D radiation-hydrodynamic simulations including dust using the guacho code. Our model includes a detailed treatment of dust grains in the ISM and takes into account the drag forces between dust and gas and the effect of radiation pressure on the gas and dust. The dust is treated as a pressureless gas component. The simulation uses typical properties of RCW 120. We analyse five simulations to deduce the effect of the ionising radiation and dust on both the emission intensity and the shape of the shock. Results. The interaction of the wind and the ionising radiation from a runaway star with the ISM forms an arc-shaped bow shock where the dust from the ISM accumulates in front of the moving star. Moreover, the dust forms a second small arc-shaped structure within the rarefied region at the back of the star inside the bubble. In order to obtain the decoupling between the gas and the dust, it is necessary to include the radiation-hydrodynamic equations together with the dust and the stellar motion. In this work all these elements are considered together, and we show that the decoupling between gas and dust obtained in the simulation is in agreement with the morphology of the infrared observations of RCW 120.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Numerical models for the dust in RCW 120

Rodríguez-González

Méliani

Sánchez-Cruces

et al. 2019

A&A

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“…While some scholars considered the method as the cause of failure and success in language teaching, for others little importance was assigned to methods and methods are considered merely as instruments in the hands of teachers (Simon, 1998) to provide opportunities for learners to acquire language (Salmani-Noudoushan, 2006). Mackey (1950) also asserts, after centuries of language teaching, there is no systematic reference to the meaning of method. Much of the field of language method has become a matter of opinion rather than of fact (Salmani-Nodouhsan, 2006).…”

Section: Methods Eramentioning

confidence: 99%

“…For example, in the decade of 20 and 30, there was a consensus among methodologists that teachers to move towards the control of vocabulary. Mackey (1950) believes that all teaching, whether good or bad, must include some sort of selection, some sort of gradation, some sort of presentation, and some sort of repetition. Selection, because it is impossible to teach the whole of a field of knowledge; we are forced to select the part of it we wish to teach.…”

Section: Methods Eramentioning

confidence: 99%

From Method to Post Method: A Panacea!

Masouleh¹

2012

ELT

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The foundation of language teaching has undergone many changes. The rise and fall of language teaching methods depends upon a variety of factors extrinsic to a method itself and often reflects the influence of profit-seekers and promoters, as well as the forces of the intellectual marketplace. There was always a source of contention among people that what the secret of a method life is. In this paper, the writer investigated why once have various teaching methods come into vogue and then disappeared? Some contradicted the method, while others came to provide a complementary view. The writer with a critical lens questioned the concept of post-method which qualitatively, as Akbari (2008) held, is not that much different from the term method. Furthermore, the author claimed the concept of post-method is not plausible by novice teachers. For the fulfillment of post-method perspectives, the whole system must be touched upon, not just a teacher as the key feature of post method. And if it is said there should be an attempt to find an alternative to method, is it really logical to imagine that even a novice teacher must seek for it?The one who first must be provided with some packages of principles in order to begin his teaching job? There is not a place to discuss whether a teacher should adopt a method or not, but what is plausible is that method is always present everywhere even in the body of the phrase like post-method. The writer, in the paper, attempted to shed lights into the concept of methods, beyond methods, post-method and, in a nutshell, what is going on in the history of language teaching.

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“…In these cases the arcs tend to be larger than average, with more extended 24 µm emission in the region between the convex side of the arc and the bright 8 µm bubble rim. Such objects are of particular interest as they appear to exemplify the transition between wind-blown bubble and bow shock morphologies (Mackey et al 2015(Mackey et al , 2016 and may provide laboratories for studying the physics of photoevaporative flows originating from the interface between hot ionised and cold molecular gas ('PEF' bow shocks; K16). We consider the prototypical bow shock candidate within a bubble to be RCW 120 ( Figure 27), a 'perfect' bubble due to its near-circular morphology (Deharveng et al 2009).…”

Section: Bubbles Versus Bow Shocks (And Bow Shocks Within Bubbles)mentioning

confidence: 99%

The Milky Way Project second data release: bubbles and bow shocks

Jayasinghe

Dixon

Povich

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Citizen science has helped astronomers comb through large data sets to identify patterns and objects that are not easily found through automated processes. The Milky Way Project (MWP), a citizen science initiative on the Zooniverse platform, presents internet users with infrared (IR) images from Spitzer Space Telescope Galactic plane surveys. MWP volunteers make classification drawings on the images to identify targeted classes of astronomical objects. We present the MWP second data release (DR2) and an updated data reduction pipeline written in Python. We aggregate ∼3 million classifications made by MWP volunteers during the years 2012-2017 to produce the DR2 catalogue, which contains 2600 IR bubbles and 599 candidate bow-shock driving stars. The reliability of bubble identifications, as assessed by comparison to visual identifications by trained experts and scoring by a machine-learning algorithm, is found to be a significant improvement over DR1. We assess the reliability of IR bow shocks via comparison to expert identifications and the colours of candidate bow-shock driving stars in the 2MASS point-source catalogue. We hence identify highly-reliable subsets of 1394 DR2 bubbles and 453 bow-shock driving stars. Uncertainties on object coordinates and bubble size/shape parameters are included in the DR2 catalog. Compared with DR1, the DR2 bubbles catalogue provides more accurate shapes and sizes. The DR2 catalogue identifies 311 new bow shock driving star candidates, including three associated with the giant H ii regions NGC 3603 and RCW 49.

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The Meaning of Method

Cited by 11 publications

References 0 publications

Numerical models for the dust in RCW 120

Numerical models for the dust in RCW 120

From Method to Post Method: A Panacea!

The Milky Way Project second data release: bubbles and bow shocks

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