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Red Giants
Red Giants

... size of the star to expand. This is the fate of the Sun in about 5 billion years. You might want to mark your calendar!The long answer is that stars convert hydrogen to helium to produce light (and other radiation). As time progresses, the heavier helium sinks to the center of the star, with a shell ...
Lecture 7: The Sun - Department of Physics and Astronomy
Lecture 7: The Sun - Department of Physics and Astronomy

Size scales in the solar system - University of Iowa Astrophysics
Size scales in the solar system - University of Iowa Astrophysics

... Why talk about the solar system in “Stars, Galaxies, & Universe”? • It is a place to “start” the journey. • We get a close-up view of a star system and a star, the Sun • Planetary systems are part of stars, and form when the stars do. ...
Solar System Information
Solar System Information

... •Solar flares are explosions of gas that occur when loops in sunspot ...
Lecture 3 -- Astronomical Coordinate Systems
Lecture 3 -- Astronomical Coordinate Systems

... E le altre stelle”… Dante, end Of Paradiso ...
Scientific Method
Scientific Method

... • The principles & empirical processes of discovery & demonstration considered characteristic of or necessary for scientific investigation, generally involving a) The observation of phenomena b) The formation of a hypothesis concerning the phenomena c) Experimentation to demonstrate the truth or fal ...
Fun Facts: Sunshine
Fun Facts: Sunshine

Chapter 2 - The Solar System
Chapter 2 - The Solar System

... The Sun is a star. It is one of more than 100 billion stars in our galaxy. It contains more than 99.8% of the total mass of the Solar System. By mass, the Sun is, at present, about 70% hydrogen and 28% helium everything else ("metals") amounts to less than 2%. This changes slowly over time as the Su ...
The Sun - TeacherWeb
The Sun - TeacherWeb

... • The sun is so bright because it goes through thermonuclear fusion – when hydrogen atoms get turned into helium atoms due to high heat and pressure – Releases massive amounts of heat and light as a byproduct – This energy and light released from the sun takes 8 minutes to reach us ...
Review 1
Review 1

... ⇒ The flux from a black body is proportional to the the fourth power of the object’s temperature. 9. Particle nature: Each photon has an unique energy E. 10. Planck’s laws: E = h ν or E = h c/λ ....relate energy of a photon to its wavelength. 11. Each element, e.g. H, He, C,..., has its own unique s ...
Inquiring minds want to know
Inquiring minds want to know

... Neutrino of definite flavor is a superposition of several mass eigenstates whose different masses cause them to propagate differently changing the mixture of the mass eigenstates, i.e. neutrino oscillations in vacuum ...
AST101_lect_13
AST101_lect_13

... Tphotosphere is set by L~ R2Tph4 Core pressure balance: nkTc ~ GM/R2 Result of fusion: 4H He; n decreases T increases to compensate Nuclear reaction rate increases  L increases Tph increases Stars evolve up and to left in MS (but not much) Solar luminosity has increased by 30% in 4.6 Gyr ...
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22

AST101 Lecture 13 The Lives of the Stars
AST101 Lecture 13 The Lives of the Stars

... •  Stars generate luminosity through fusion of H into He •  The lifetime of a star is proportional to the amount of fuel it has (mass) divided by the rate at which it expends the fuel (luminosity) •  The lifetime τ ~ M/L ~ M-2 (because L ~ M3) •  τ ranges from 4x106 years for O stars to ~1012 years ...
Asteroseismology and the Solar
Asteroseismology and the Solar

... • Rise at low frequencies due to fixed Dc but largest shifts at higher frequency Metcalfe et al. (2007) ...
1. Describe (preferably with a sketch) what astronomer
1. Describe (preferably with a sketch) what astronomer

Spicy Solar System Goal Model the solar system with edible
Spicy Solar System Goal Model the solar system with edible

... objects) based on edible ingredients that can easily be found in most environments. If these ingredients are hard to find, they can of course be replaced by another of the same size. The Solar System Sun Mercury Venus Earth - Moon Mars Asteroid belt Jupiter Saturn Uranus Neptune (Pluto) ...
The structure and evolution of stars
The structure and evolution of stars

Our Solar system - World of Teaching
Our Solar system - World of Teaching

...  The outer layer is the chromosphere  The layer under the chromosphere is the photosphere, where light and other forms of energy are released  Under the photosphere is the convective zone where heat is released  The layer above the core is the radiative zone ...
Discussion Activity #9
Discussion Activity #9

Energy Production in Stars
Energy Production in Stars

...  Stars are at enormous distances, yet we can see thousands => extremely luminous  What is the source of their enormous energy? o Thermonuclear reactions (fusion) that convert mass to energy  In the special theory of relativity Einstein demonstrated that the total mass-energy was conserved => e = ...
ppt - Slides by Prof Christian
ppt - Slides by Prof Christian

... White Dwarfs < 1.4 Msun (Chandrasekar limit) Neutron Stars > 1.4 Msun < 3 Msun Black Holes > 3 Msun White Dwarfs - size of Earth (6000 km radius) Neutron Stars - size of small city (10 km radius) Black Holes - smaller* still than a city (< 10 km radius)! ...
Threat of Sunshine
Threat of Sunshine

... TIFF (LZW) decompressor are needed to see this picture. ...
Chapter 26
Chapter 26

23sun4s
23sun4s

... From radioisotope dating we know that the solar system is 4.5 billion years old ...
< 1 ... 210 211 212 213 214 215 216 217 218 ... 237 >

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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