HS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us
What students must show for performance expectation HS-ESS1-1, with a lesson sequence built on live data, the misconceptions to expect, and assessment questions with answers.
Last updated . Curriculum links last reviewed November 2026.
What students must show
Our summary- Students develop a model, based on evidence, of the Sun's life span and of how nuclear fusion in its core releases energy that eventually reaches Earth as radiation.
How energy travels from the core to Earth. Evidence includes other stars' masses and lifetimes, solar flares and the 11-year sunspot cycle.
The atomic and subatomic details of solar fusion.
Our summary, in our own words. Read the official wording.
The three dimensions
High schoolDeveloping and using models
Develop a model based on evidence to show relationships between parts of a system.
ESS1.A and PS3.D
The Sun is changing and will run out of fuel over a life of about 10 billion years; fusion in its core releases the energy that reaches us.
Scale, proportion and quantity
A phenomenon depends on the scale at which it occurs.
Live tools for this standard
3 toolsLesson sequence
Engage to evaluate- Engage10 min
Spin the live Sun and count the sunspots today. Ask: where does all this energy come from, and why has the Sun not run out?
- Explore25 min
Energy budget: the Sun gives off about 3.8 x 10^26 watts. Using E = mc^2, students find the mass turned into energy every second (about 4 million tonnes).
- Explain20 min
Model the journey: fusion in the core; energy carried outward by radiation, then by convection; light leaving the surface and reaching Earth about 8 minutes later. Evidence for change: the 11-year sunspot cycle and flares. The aurora forecast shows space weather arriving.
- Elaborate15 min
Life span: the Sun is about 4.6 billion years old, roughly halfway through its life. A star ten times more massive lasts only a few tens of millions of years. Why would bigger stars live shorter lives?
- Evaluate15 min
Students draw a labeled model from the core to Earth and add one piece of evidence for the Sun's life span.
Common misconceptions
3 to watch forThe Sun is burning like a fire.
Nothing is burning: there is no oxygen fire. Hydrogen nuclei fuse into helium, a nuclear process.
A Sun made of burning coal would have gone out within a few thousand years.
Light made in the core reaches us 8 minutes later.
The 8 minutes is the trip from the surface. Energy made in the core takes many thousands of years to work its way out.
Ask why the light we see today began its journey long before people existed.
The Sun will explode as a supernova.
The Sun is not massive enough. In about 5 billion years it will swell into a red giant, then shrink to a white dwarf.
Compare its future with a massive star on the telescope page.
Assessment questions
Answers folded awayHS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us · orbitalradar.com/schools/us/standards/hs-ess1-1
- What powers the Sun?
- Burning gas
- Nuclear fusion of hydrogen into helium
- Radioactive decay
- About how long will the Sun shine in total?
- 10 million years
- 10 billion years
- Forever
- Each second the Sun turns about 4 million tonnes of matter into energy. Why will it not run out soon?
- How do sunspots and flares show that the Sun changes?
- Check the aurora forecast. Is space weather active today? What on the Sun would raise it?
Answer key
- Nuclear fusion of hydrogen into helium.
- About 10 billion years.
- Its mass is about 2 x 10^27 tonnes, so even at that rate it lasts billions of years.
- Their numbers rise and fall over about 11 years, and flares release bursts of energy we detect on Earth.
- It depends on the day; a flare or coronal mass ejection aimed at Earth.
Worksheet
US LetterNo live-data worksheet for this standard yet: print the assessment questions above. All sheets: the worksheet library.
The same idea in state standards
Texas, Florida, Georgia- Texas: Astronomy 12D
- Florida: SC.912.E.5.4, SC.912.E.5.3
- Georgia: SAST3.b, SAST5.a
Related, not equivalent: each state words and groups its standards differently.
More standards pages
High schoolAbout these codes
These are our suggestions for where each tool fits. Always preview a page before using it with a class: some tools show ads, these school pages do not.
Codes are performance expectations of the Next Generation Science Standards*, for example 5-ESS1-2. Each summary is our own wording; follow the link on a standard page for the official text.
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Cite this page
Pick a style, then copy it or download it for your reference manager.Orbital Radar. (2026, November 6). HS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us. Retrieved November 6, 2026, from https://orbitalradar.com/schools/us/standards/hs-ess1-1
“HS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us.” Orbital Radar, 6 Nov. 2026, orbitalradar.com/schools/us/standards/hs-ess1-1. Accessed 6 Nov. 2026.
Orbital Radar (2026) HS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us. Available at: https://orbitalradar.com/schools/us/standards/hs-ess1-1 (Accessed: 6 November 2026).
Orbital Radar. “HS-ESS1-1: The Sun's fusion, its life span and the energy that reaches us.” Last modified November 6, 2026. https://orbitalradar.com/schools/us/standards/hs-ess1-1.
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* Next Generation Science Standards is a registered trademark of WestEd. Neither WestEd nor the lead states and partners that developed the Next Generation Science Standards were involved in the production of this product, and do not endorse it.