The structure of a star will also be affected by how easily photons can pass through the material in any given layer. If a layer absorbs photons, then it will be heated with an increase in pressure that will expand the layer. Alternatively, if a layer is transparent and allows photons to readily escape, then that layer will be cooler with a lower gas pressure that will allow gravity to compress its material. Astronomers actually use the reciprocal of transparency, or opacity, to measure the ability of photons to pass through material. A low opacity means high transparency; a high opacity means a low transparency. The opacity of the material in a given layer depends on the chemical composition (some elements absorb light more easily than other elements), the temperature, and the density.
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- Introduction to the Solar System
- Origin and Evolution of the Solar System
- Terrestrial Planets, Gas‐Giant Planets
- Comparative Planetology: Terrestrials
- Comparative Planetology: Gas Giants
- Minor Objects: Asteroids, Comets, and More
- Other Planetary Systems
- Properties of Earth and the Moon
- Earth's Atmosphere
- Earth's Chemical Composition
- Interior Structure: Core, Mantle, Crust
- The Age of Earth
- Origin of the Earth‐Moon System
- Tidal Forces
- Evolution of the Earth‐Moon System
- Properties of the Sun
- The Photosphere
- The Chromosphere
- The Corona
- The Sunspot Cycle
- Internal Structure; Standard Solar Model
- Energy Generation: Proton‐Proton Cycle
- Solar Neutrino Problem
- Helioseismology
- Three Types of Astronomical Study
- Stellar Parallax and Distances
- Apparent Magnitudes
- Absolute Magnitudes
- Luminosities
- Masses
- Radii
- Colors
- Spectral Types
- Surface Temperature
- Chemical Composition
- Luminosity Classes
- Proper Motions and Radial Velocities
- Properties of Secondary Importance
- Hertzsprung‐Russell Diagram: The Basics
- Main Sequence Stars
- Mass‐Luminosity Relationship
- Red Giants and Supergiants
- White Dwarf Stars
- Spectroscopic Parallax
- Equation of State
- Hydrostatic Equilibrium
- Thermal Equilibrium
- Energy Generation: The CNO Cycle
- Opacity
- Energy Transport
- High‐Mass Stars versus Low‐Mass Stars
- Other Types of Stars
- White Dwarf Stars
- Novae
- Type I Supernovae
- Type II Supernovae
- Neutron Stars (Pulsars)
- Black Holes and Binary X Ray Sources
- Interstellar Matter
- Interstellar Nebulae
- Star Clusters
- Structure of the Galaxy
- Origin and Evolution of the Galaxy
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A Brief History of Astronomy
The Structure of Stars
