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Is the Sun a Star? - Classroom Websites
Is the Sun a Star? - Classroom Websites

Lecture 13 Presupernova Models, Core Collapse and Bounce
Lecture 13 Presupernova Models, Core Collapse and Bounce

... Ye could raise YL. ...
Slide 1
Slide 1

... 2. A Protostar forms in the centre, when the core becomes dense enough; later will become the Sun. 3. Dust grains stick to each other and sweep their paths, forming larger particles (Planetesimals). 4. Orbital paths are cleared. 5. The Sun and its planets all spin in the same direction. ...
Stellar Evolution and our Sun (Song “The Sun” from “Severe Tire
Stellar Evolution and our Sun (Song “The Sun” from “Severe Tire

... thermonuclear energy core the only part of the sun that actually makes energy about 1/4 of Sun’s radius T = 18 million degrees F (10 millions K) Radiative Zone where most of the harmful gamma rays bounce around dissipating energy until they become less harmful forms of energy out to about 0.71 Sun r ...
Stellar Evolution
Stellar Evolution

... With a thin crust of Iron. It begins to spin super-fast with a period is as little as a second! This generates a strong magnetic field and a beacon of radio energy that acts like a spinning search-light. That appear to us as a Pulsar, a source of a rhythmic radio signal first thought to be intellige ...
What is a Star - Optics Institute of Southern California
What is a Star - Optics Institute of Southern California

PowerPoint Presentation - Copernicus
PowerPoint Presentation - Copernicus

... Place: Center for Creative Photography (UA Main Campus). Gregory Benford, Author and Astrophysicist at UC Irvine "Seeking Ozymandias: Building and Searching for Beacons” What would transmitters be like if built by civilizations with a variety of motivations, but who cared about cost? We have conside ...
The Earth and Beyond
The Earth and Beyond

...  Life cycle of stars – differs for massive & small stars  Red-shift – evidence for fast expansion of galaxies  History of the Universe – Big Bang or Steady State  Future of the Universe – Big Crunch or Eternal Expansion ...
Slide 1
Slide 1

... know everything about everything, and that is where the challenge comes in. You really need to be at the top of your game when you teach this unit. There are some fantastic web sites out there with some incredible information, the information is written at all levels of understanding. I recommend to ...
1.4 Our Solar Neighbourhood
1.4 Our Solar Neighbourhood

... are objects made up of dust and ice that travel through space. Their long tails and bright glow only Comets spend most of their time slowly orbiting in the outer reaches of the solar system. Halley’s comet, which is visible from Earth every 76 years. The last time it was seen was in 1986. ...
Sublimation • In a vapour in thermal equilibrium, the molecules of
Sublimation • In a vapour in thermal equilibrium, the molecules of

mechanical
mechanical

... • Photo-electric emission – Photons hit surface, release electrons ...
Mercury, the closest planet to the Sun, is a small
Mercury, the closest planet to the Sun, is a small

A glimpse at the formation of our Solar System
A glimpse at the formation of our Solar System

... Our protoplanetary disk probably lasted “only” a few million years before being absorbed or blown away by the Sun, but most of the planet formation could be completed during that time. Our parent cloud was mostly made of gaseous hydrogen and helium, which are the main constituents of the Universe, b ...
Facts and figures on the sun and planets
Facts and figures on the sun and planets

... Under such conditions, the methane found in Neptune's atmosphere also decomposes, as the bonds holding methane's four hydrogen atoms dissolve and the carbon atoms may bind to one another in the extreme pressure to form diamonds (according to a new hypothesis by a team at the University of California ...
Phys133 Sample MidTerm #2 Covers Chs.10
Phys133 Sample MidTerm #2 Covers Chs.10

Answers
Answers

Numerical simulations of convection in A
Numerical simulations of convection in A

The Physics of the Sun
The Physics of the Sun

... The equatorial coordinate system is used to illustrate the motion of heavenly stars on the celestial sphere—an imaginary sphere of radius equal to the distance of stars so that they appear to be lying on its surface. The projection of the earth’s equator onto the celestial sphere is called the celes ...
life cycles of stars
life cycles of stars

... Helium fusion does not begin right away because it requires higher temperatures than hydrogen fusion—larger ...
Secrets of the Sun
Secrets of the Sun

Earth Movement in Space
Earth Movement in Space

... In this alignment winter will occur in the northern hemisphere when we are at aphelion so winters will be very cold and summer will occur when we are at perihelion so summers will be very hot.  precession animation ...
MS-ESS1 Earth`s Place in the Universe
MS-ESS1 Earth`s Place in the Universe

... ESS1.A: The Universe and Its Stars  Patterns of the apparent motion of the sun, the moon, and stars in the sky can be observed, described, predicted, and explained with models. (MS-ESS1-1)  Earth and its solar system are part of the Milky Way galaxy, which is one of many galaxies in the universe. ...
Gravitational Waves from Neutron Stars
Gravitational Waves from Neutron Stars

... - Kaon and/or Pion condensations, - Transitions from ordinary nuclear matter to quark matter ...
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Standard solar model

The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma). This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined. The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System. The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium. All heavier elements, called metals in astronomy, account for less than 2 percent of the mass. The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to ""fit"" the observed Sun.
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