Star Life Cycles 5E

Does the exoplanet have a star like our Sun?

Driving question: Which kinds of stars are most likely to support Earth‑like planets?

Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Engage

What happens to stars over time? What will happen to our Sun?

  • Observe a data visualization of Supernova 1054 (Crab Nebula remnant).
  • Individually answer Q1–Q4 on “What Was Supernova 1054?”
  • Share in Domino Discover routine.

Consider:

  • What might cause a star to change and explode?
  • What other phenomena are similar to a supernova?
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Engage: Access & Setup

  • Materials: “What Was Supernova 1054?” handout; video link; images
  • Pair-share: Generate questions about star stability relevant to Earth-like planets
  • Post class questions under “What do we need to know about other stars?”

Implementation tip:

  • Patterns & Stability: Ask “Are changes in stars fast or slow? Do patterns differ across stars?”
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explore 1

Observing patterns of star stability and change

Goal:

  • Use a computational model (Star in a Box) to collect data on star mass, lifespan, and stability.

Focus data:

  • Time (lifespan), size (radius), temperature, luminosity

Task:

  • Complete “What Kinds of Stars Have Long and Stable Life Spans?” in pairs.
  • Group stars by life-cycle category; fill Group 1 as example.
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Have you ever seen stars in the night sky? If you live in the city, you may see fewer stars than in the image below. From a dark place on Earth, many stars are visible.

center

What do you think we would see if we looked at that same portion of the sky with an even more powerful telescope?

Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Hubble Telescope












Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Spectra Data from Omega Centauri Star Cluster

center

Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Composition of 1 Solar Mass Star

center

Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explore 1: See–Think–Wonder

Synthesize:

  • See: Patterns observed in mass vs. lifespan/stability
  • Think: Implications for supporting Earth-like planets
  • Wonder: New questions about star change

If counterintuitive:

  • Discuss why higher‑mass stars die faster.
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explore 2

Making connections between observable star properties and lifespan

Goal:

  • Develop a mathematical model (HR Diagram) with provided star circles.
  • Identify patterns relating temperature, luminosity, color, mass, and expected lifespan.

Task:

  • Plot the 60-star set on poster-size HR template.
  • Complete See–Think–Wonder; share via Domino Discover.

Look for:

  • Hotter → brighter; main sequence clustering
  • Red stars = longest expected lifespan
  • ~1 solar mass stars stable >10 billion years
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explore 2: Class List

Build a consensus list:

  • Properties that allow predictions of lifespan & stability
  • Kinds of stars that live long, stable lives

Important:

  • Mass predicts life cycle & stability
  • Color/temperature/luminosity indicate mass → stability
  • Post‑main‑sequence changes are large and disruptive
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explain

Developing an explanatory model for stability and change

Core ideas:

  • Gravity pulls matter inward; fusion releases energy outward.
  • Stability occurs when inward gravity and outward fusion pressures are balanced.
  • More massive stars fuse faster → higher luminosity → shorter lifespans.

Task:

  • Read “How and Why do Stars Change” with text annotation:
    • Circle: info for size increases
    • Underline: info for size decreases
    • Box: uncertainties; annotate questions
  • Label force diagrams for key stages.
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Explain: Evidence & Reasoning

From model/data:

  • Main sequence = most stable; ~90% of life
  • Lifespans (example): 1 M☉ ~8993 Myr; 4 M☉ ~179 Myr; 40 M☉ ~4.9 Myr
  • Hydrogen→helium conversion time: faster for higher mass (e.g., 10 M☉ ~19.5 Myr vs 1 M☉ ~10 Gyr)
  • Higher mass → higher luminosity (energy per second)

Summary task prompts:

  1. How did you use models & evidence to explain star life cycles?
  2. Why does stability matter for habitability?
  3. What new questions remain?
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Class Consensus Discussion

Steps:

  1. Selected groups present claims & models
  2. Peers paraphrase & ask clarifying questions
  3. Whole-class discussion; agree on shared representation

Prompts:

  • Why do higher mass stars die faster?
  • How does luminosity relate to fusion rate?
  • How long must a star be stable to support life?
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Elaborate

Explaining differences in stability via nucleosynthesis

Model:

  • Iron [26] game to simulate gravity-driven fusion rates
  • Represent gravity:
    • High-mass star → faster random key taps
    • Low-mass star → slower random key taps

Tasks:

  • “Why do more massive stars change and die faster?”
  • “How are elements heavier than iron produced?”

Look for:

  • Stronger gravity → more frequent, energetic collisions → faster fusion → higher luminosity
  • High-mass stars produce heavier elements; supernova required for >Fe
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Elaborate: Reflection

Prompt:

  • Why was it necessary to study stars at multiple scales (supercluster, one star, atomic) to explain stability and change?

Write:

  • Short paragraph referencing modeled patterns at each scale.
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Evaluate

Constructing arguments: Which star best supports an Earth-like planet?

Tasks:

  • Revise group models (Idea Carousel routine)
  • Annotate peer models: ✔ resonates; ➕ add; ? question; Δ clarify
  • Use Star Life Cycles Model & Argument rubrics
  • Return to Performance Task Organizer; self-assess & revise

Consider:

  • Main sequence stars ≤ 1 M☉ with stable properties ≥ 9–10 Gyr
  • Exclude: blue giants (Eta Carinae), red giants (Kepler-432), faint white dwarfs (Gliese 440)
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Evaluate: Driving Question Board

Revisit:

  • What did we figure out?
  • What do we still need to investigate?
  • Generate one new question on planet characteristics (distance, temperature, liquid water, atmosphere, terrestrial vs jovian)

Next 5E:

  • Focus on planets’ habitable zones and liquid water evidence.
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Materials & Grouping (Quick Reference)

  • Handouts: Supernova 1054, Star properties & lifespans, HR star circles + template, How & Why Stars Change, Fe‑26 tasks, Performance Task Organizer
  • Routines: Domino Discover; Think–Talk–Open Exchange; Class Consensus; Idea Carousel
  • Grouping: Pairs; small groups; class discussion
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Standards Alignment

Science & Engineering Practices:

  • SEP2 Models (computational & mathematical)
  • SEP6 Explanations from evidence

DCIs:

  • ESS1.A Universe & Stars
  • PS3.D Energy in nuclear processes

Crosscutting Concepts:

  • Patterns across scales
  • Energy & Matter
  • Stability & Change

Common Core:

  • ELA: RST.9‑10.1, RST.9‑10.7, WHST.9‑10.1
  • Math: MP2, MP4
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

Exit Ticket (End of Unit)

  • Identify one star from the dataset and argue for/against habitability using:
    • Lifespan/stability evidence
    • HR diagram position
    • Fusion/nucleosynthesis reasoning
  • 3–5 sentences; cite at least two pieces of evidence from your investigations
Star Life Cycles 5E • Maple Hill Jr/Sr High • Room 116

TEACHER NOTE: - Purpose: Full 5E sequence slides for "Star Life Cycles." - Student-facing content only on slides; teacher prompts and flow in comments. - Accessibility: read aloud key prompts; describe images verbally; coordinate with TVI (Ms. Loyche) for tactile/alt text as needed for Keira.

TEACHER NOTE: - Set context: connects to prior 5E "How the Sun Works." - Mention stability of energy over ~4–5 billion years.

TEACHER NOTE: - Project the visualization/video; narrate. - If students don’t mention gravity, nuclear fusion, or nebula formation, seed those ideas. - For Keira: provide verbal description of the visualization and printed Braille/tactile summaries.

TEACHER NOTE: - Facilitate Domino Discover. Capture top 3 class-relevant questions to carry forward.

TEACHER NOTE: - Model link: https://starinabox.lco.global/ - Clarify computational models are evidence-based. - Conferring questions: Which stages change least/most? Relation of mass to lifespan and stability?

TEACHER NOTE: - If key observations didn’t surface, run a demo and prompt with questions. - Differentiate: sentence starters in “See” column; sample responses for tables.

TEACHER NOTE: - Emphasize Patterns CCC; color–temp–luminosity relationships. - Address outliers (not on main trend line) later during Explain/Extension.

TEACHER NOTE: - Capture the list on chart paper for reference in Explain and Evaluate.

TEACHER NOTE: - Facilitate causal reasoning: how/why stars change. - Use Natural Reader for ELL/below-level readers. - Video: Star Formation by Collapse of Molecular Clouds—students note gravity-driven collapse.

TEACHER NOTE: - Elevate key points on a shared HR diagram. - If needed, assign “Why do some stars not fall on the main trend line?” as extension.

TEACHER NOTE: - Choose claims that advance understanding. - Link back to Patterns across scales (solar system, cluster, atomic).

TEACHER NOTE: - Use Think–Talk–Open Exchange to articulate ideas. - Video: Stephen Hawking – Supernovas to close phenomenon loop. - Assess CCC Patterns across scales (supercluster, Sun, atomic).

TEACHER NOTE: - Collect for formative assessment; highlight the multi-scale reasoning.

TEACHER NOTE: - Provide rubric, sample composite work, peer review flow. - Emphasize evidence-based claims using patterns, stability, and nucleosynthesis reasoning.

TEACHER NOTE: - Transition to next investigation; capture questions for planning.

TEACHER NOTE: - Prepare printed/large-font versions; alt text packets for TVI coordination. - Verify Star in a Box access; poster supplies for HR graphing.

TEACHER NOTE: - Use this slide for admin/observer context or students’ reflection.

TEACHER NOTE: - Collect as summative checkpoint; align to argument rubric.