In this Grade 6 Earth Science lesson from Chapter 22, students learn how stars are classified by size, brightness, and temperature, and how they form and change over their life cycles. Key vocabulary includes light-years, nebula, main sequence, neutron stars, and black holes. Students also explore parallax through hands-on experiments to understand how astronomers measure the distance of stars from Earth.
Section 1
Stars Transform Energy Through Their Life Cycles
Stars begin as gas clouds called nebulae, enter the main sequence where they fuse hydrogen, then expand into giants or supergiants, and eventually end as white dwarfs, neutron stars, or black holes.
Section 2
Astronomers Use Parallax to Measure Stellar Distances
Scientists observe a star's apparent shift in position from different locations in Earth's orbit. The greater the shift, the closer the star. This helps determine a star's true brightness.
Section 3
Temperature Determines a Star's Color and Classification
Stars are classified by their surface temperature and color, from hot blue-white stars (over 25,000°C) to cool red stars (below 3,500°C). The Sun, a yellow G-class star, has a temperature of 6,000°C.
Section 4
Mass Controls How Stars Live and Die
Lower-mass stars like our Sun remain in the main sequence for billions of years, eventually becoming giant stars then white dwarfs. Higher-mass stars burn faster, becoming supergiants that explode as supernovae.
Section 5
Scientists Plot Stars' Brightness and Temperature on Diagrams
Using the Hertzsprung-Russell diagram, astronomers map stars by their surface temperature and luminosity. This scatter plot helps identify relationships between star properties and their life cycle stages.
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Section 1
Stars Transform Energy Through Their Life Cycles
Stars begin as gas clouds called nebulae, enter the main sequence where they fuse hydrogen, then expand into giants or supergiants, and eventually end as white dwarfs, neutron stars, or black holes.
Section 2
Astronomers Use Parallax to Measure Stellar Distances
Scientists observe a star's apparent shift in position from different locations in Earth's orbit. The greater the shift, the closer the star. This helps determine a star's true brightness.
Section 3
Temperature Determines a Star's Color and Classification
Stars are classified by their surface temperature and color, from hot blue-white stars (over 25,000°C) to cool red stars (below 3,500°C). The Sun, a yellow G-class star, has a temperature of 6,000°C.
Section 4
Mass Controls How Stars Live and Die
Lower-mass stars like our Sun remain in the main sequence for billions of years, eventually becoming giant stars then white dwarfs. Higher-mass stars burn faster, becoming supergiants that explode as supernovae.
Section 5
Scientists Plot Stars' Brightness and Temperature on Diagrams
Using the Hertzsprung-Russell diagram, astronomers map stars by their surface temperature and luminosity. This scatter plot helps identify relationships between star properties and their life cycle stages.
Book overview
Jump across lessons in the current chapter without opening the full course modal.
Continue this chapter