This "book" accompanies the Harvard University graduate course Astronomy 201b, "The Interstellar Medium and Star Formation." The first incarnation was created in 2011 by Prof. Alyssa Goodman, Teaching Fellow Chris Beaumont, and the 21 Harvard graduate students who took the course at that time. The "book" will continue to evolve throughout Spring 2013 as student contributions…
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ISM and Star Formation | AY 201b Student Textbook | ay201b.wordpress.com Reviews
https://ay201b.wordpress.com
This "book" accompanies the Harvard University graduate course Astronomy 201b, "The Interstellar Medium and Star Formation." The first incarnation was created in 2011 by Prof. Alyssa Goodman, Teaching Fellow Chris Beaumont, and the 21 Harvard graduate students who took the course at that time. The "book" will continue to evolve throughout Spring 2013 as student contributions…
ay201b.wordpress.com
GMC Formation and Spiral Spurs | ISM and Star Formation
https://ay201b.wordpress.com/2011/04/07/gmc-formation-and-spiral-spurs
ISM and Star Formation. 8220;The Book”. GMC Formation and Spiral Spurs. On April 7, 2011. M51: Composite Hubble Image (Strong m=2 response and interarm spur features). There are several related questions that we want to address:. How does a Milky Way type galaxy evolve (in isolation)? What is it, how does it form, where does it occur, when, and why? We may have a good idea of what stars are, but: how do they form? The cloud formation rate sets the overall rate and nature of star formation. 8211; we must ...
The Hot ISM (Evidence and Observations) | ISM and Star Formation
https://ay201b.wordpress.com/2011/03/03/hot-ism
ISM and Star Formation. 8220;The Book”. The Hot ISM (Evidence and Observations). On March 3, 2011. The hot ISM, also called coronal gas, refers to very hot, low density gas which has been shock-heated by fast stellar winds and blast waves from novae and supernovae. Its temperature and density are. And it is believed to fill about half of the volume of the galactic disk, as well as much of the volume above and below the disk through chimney flows. Beyond the galaxy, much of the IGM is believed to be at.
X-ray Absorption by the ISM | ISM and Star Formation
https://ay201b.wordpress.com/2011/03/01/x-ray-absorption-by-the-ism
ISM and Star Formation. 8220;The Book”. X-ray Absorption by the ISM. On March 1, 2011. When interpreting data from X-ray satellites like Chandra and XMM-Newton, it is necessary to understand how the X-ray spectrum is modified as it passes through the interstellar medium, i.e. how high-energy photons (0.1-10 keV) interact with the ISM (and IGM). Essentially answering this boils down to calculating the (energy-dependent) photo-ionization cross-section of the ISM,. Of Wilms et al.). Is the atomic number, and.
Topical Modules | ISM and Star Formation
https://ay201b.wordpress.com/topical-modules
ISM and Star Formation. 8220;The Book”. Interactive Software Modules Created by Students. To see modules created by students in the Spring 2013 term. For a full description of the module creation process, motivations, and outcomes, see our article arXiv:1308.1908. Our list of ideas. For ISM-related web modules. Chris and Nathan’s notes. On individual projects and the module prospectus. W5 WWT “Director’s Cut” Prototype. By Alyssa Goodman, presented 4/2/13). 9654; 3 Responses. 8230;] This is the third in ...
Journal Club 2013 | ISM and Star Formation
https://ay201b.wordpress.com/journal-club-2013
ISM and Star Formation. 8220;The Book”. This page links to the journal articles discussed by the class in Spring 2013. Articles were selected from the AY201b Library at Mendeley. This page is a continual work in progress… the full journal club schedule can be viewed on the iSite. Some good examples from the 2011 course and Astrobites are below. Star Formation Via Momentum Input From Massive Stars. Dust Grain Size Distributions. The 3D structure of Cas A. Asteroid belt found in the Vega System. Concerned ...
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Meet the Eagle Nebula | The physics behind one of Hubble's most famous images
http://portillo.ca/nebula
Meet the Eagle Nebula. The physics behind one of Hubble's most famous images. Skip to primary content. Skip to secondary content. The Spectrum and Energy Levels. 8220;The Pillars of Creation” – a composite from images taken by the Hubble Space Telescope’s WFPC2. Hosted by Wikimedia Commons). 8220; The Pillars of Creation. 8221; is one of the most famous images taken by the Hubble Space Telescope. In conclusion, the WFPC2 images of M16 are visually striking, and noteworthy from that perspective alone.
Hydrodynamics | A visualization tool of 2D shocks simulations
https://2dshocks.wordpress.com/hydrodynamics
A visualization tool of 2D shocks simulations. An interactive module by Fernando Becerra. Euler equations describe a smooth flow. The equations represent conservation of mass (continuity equation), momentum and energy in the fluid. The set of equations are given by:. Is the total energy density. So far we have three equations and four variables, so we need a forth equation. In the case of a compressible fluid we add an equation of state (EOS) of the type. Which is equivalent to consider constant density).
Ultraviolet Radiation and Young Stars | Landmarks of the ISM
https://ismlandmarks.wordpress.com/ultraviolet-radiation
Landmarks of the ISM. A tour of some of the most beautiful objects in the interstellar medium and an introduction to what observations at different wavelengths can tell us about them. Skip to primary content. An Overview of the ISM. Ultraviolet Radiation and Young Stars. What is Ultraviolet Radiation? Ultraviolet radiation is electromagnetic radiation with a wavelength shorter than that of visible light (between 400 nm and 10 nm), but longer than X-rays. Ultraviolet Radiation and HII Regions. This websit...
Shocks | A visualization tool of 2D shocks simulations
https://2dshocks.wordpress.com/shocks
A visualization tool of 2D shocks simulations. An interactive module by Fernando Becerra. Shocks by definition are discontinuities in the fluid properties (e.g. density, velocity, pressure). A schematic image is shown in Fig.1, where we can clearly identify the discontinuity as a “shock jump”. The values of the fluid properties change abruptly at that interface. Pressure, energy and density have values. Respectively to the left of the shock, while to the right the values are. Which is basically jets eman...
Simulations | A visualization tool of 2D shocks simulations
https://2dshocks.wordpress.com/simulations
A visualization tool of 2D shocks simulations. An interactive module by Fernando Becerra. What is a numerical simulation? In astrophysics most processes can be described by a set of equations. A simple example are the equations of motion. Take a long time and we are not able to watch the whole process with telescopes. Another interesting example is the formation of the first structures in the Universe. A very famous simulation of large scale structure is the Millenium simulation. Based in an Lagrangian h...
Documentation | A visualization tool of 2D shocks simulations
https://2dshocks.wordpress.com/documentation
A visualization tool of 2D shocks simulations. An interactive module by Fernando Becerra. A zip version of the code is available here. Alternatively you can download pyro2 from its webpage. And add the file interface.py. To the pyro2/ directory. Here a list of programs you need to install before installing pyro2:. The only step needed to install pyro2 is building the fortran source. In order to do that just go to the pyro2/ folder and execute. Running a new simulation. Choose the initial conditions.
The Code | A visualization tool of 2D shocks simulations
https://2dshocks.wordpress.com/code
A visualization tool of 2D shocks simulations. An interactive module by Fernando Becerra. Pyro (from PYthon hydRO) was originally written in 2003-2004 by Michael Zingale. This version was resurrected beginning in 2012 and rewritten for numpy and brought up to date. pyro2. Is a 2D grid-based code mostly written in Python, with a few low-level routines written in Fortran. pyro2 employs a commonly used method to solve numerically the equations in grid-base codes, which is called the finite-volume method.
Supernovae and Shocks | Landmarks of the ISM
https://ismlandmarks.wordpress.com/supernovae-and-shocks
Landmarks of the ISM. A tour of some of the most beautiful objects in the interstellar medium and an introduction to what observations at different wavelengths can tell us about them. Skip to primary content. An Overview of the ISM. A supernova results from the explosion of a star. After the explosion, a remnant remains that consists of ejected material and the interstellar material swept up by an associated expanding shock. There are really two main routes to produce a supernova:. The shell begins to co...
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ISM and Star Formation | AY 201b Student Textbook
ISM and Star Formation. 8220;The Book”. Our Jointly-Edited Online “Book”. This “book” accompanies the Harvard University graduate course Astronomy 201b. Links at the top of each section (in orange. Are slides and notes from this year (2013), sorted by date. They will be posted within one day of the class date. Links in red. Are transcriptions of Alyssa Goodman’s notes, originally from 2011 and updated throughout the semester as we discuss each topic. Links in green. 1) Jan. 29:. 2) Jan. 31: Intro to ...
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Ay21arum's Blog | Just another WordPress.com site
Just another WordPress.com site. Stay updated via RSS. How to Develop Multiple Intelligences in the School? How to Develop Multiple Intelligences in the School? Posted: October 25, 2010 in Uncategorized. Extracurricular activities in the school can increase and develop multiple intelligences members. If the extracurricular is done effectively, school can accommodate all aspects of Multiple Intelligences. It can make the great changed in education world. Why can I say that? Ed) Australia : Thomson. 2010 f...
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