Learn

Learning preferences

Make learning more comfortable. Changes apply immediately.

Enlarges page content, including diagrams and their labels. You can also use your browser’s zoom.

Choose the colours that are easiest for you to distinguish. Applies to lesson diagrams and lab plots. Labels, shapes, hatching and line patterns also distinguish meanings. Source photographs and raw image brightness stay unchanged; mask-only views are available for image overlays.

ExampleComparisonSample link

Saved in this browser on this device. Preferences are separate from progress backups.

SCIENCE · INVESTIGATE AND EXPLAIN

Track hydrogen through the pp-I chain

Cancel intermediates and returned protons while keeping nuclear and atomic bookkeeping separate.

Learning outcome: Recover net fuel consumption and explain the electron inventory.

Starting recap

The first two steps occur twice; helium-3 fusion returns two protons.

All lessons are open directly. Your saved experiments remain when you leave and return.

Try

Six supplied protons minus two returned gives four consumed.

Open the experiment

Predict

Does counting every input proton give net consumption?

Experiment

Compare 5 and 10 percent reservoirs at fixed one-unit photon demand, then cancel the paper reaction cards.

Trace fusion energy into a conditional fuel budget

Worked teaching model · synthetic values · Synthetic total mass 2.0×10³⁰ kg; the chosen accessible region has fixed hydrogen-1 mass fraction 0.70. Neutral-atom mass differences include electron bookkeeping. A restricted pp-I mean assigns 0.530 MeV per completion to escaping neutrinos. Remaining energy is assumed to support the specified average photon demand. Rates are required, not achieved; zero fuel supports zero duration. No actual stellar lifetime, reaction-rate, structure, mixing or evolution prediction is made.

Reset keeps your prediction, captures and practice history.

Build helium from hydrogen, then ask how much energy a specified fuel inventory could supply. The two controls change the hypothetical inventory and average photon demand; they do not change nuclear masses or calculate an actual stellar reaction rate.

pp-I worked mechanism · p = proton; n = neutron; e⁺ = positron; νe = neutrinoTwice: p + p → ²H (1p + 1n) + e⁺ + νeTwo weak conversions produce two neutrons and two escaping neutrinos.Twice: ²H + p → ³He (2p + 1n) + γγ denotes a gamma photon. Both intermediate helium-3 nuclei are used next.Once: ³He + ³He → ⁴He (2p + 2n) + p + pSix protons entered the preceding stages; two return. Net consumption: four.Also twice: e⁺ + e⁻ → photons. Surrounding electrons supply the e⁻.Cancel intermediates on paper. This chain is not one four-proton collision.Reaction count does not determine a rate; temperature and density are not modeled.

For the energy ledger, use four neutral hydrogen-1 atoms and one neutral helium-4 atom. This is consistent rest-mass bookkeeping for the net process, not neutral atoms inside the hot core. Four initial electrons account for two in the final atom and two annihilating with positrons. Do not add annihilation rest energy again. Plasma ionization and tiny neutrino rest-mass corrections are omitted.

Rest masses · common scale 0–4.1 u4 neutral H-11 neutral He-40 u4.1 uDifference 0.02869687 u ≈ 0.712% of initial fuel rest mass.Released energy · separate scale 0–27 MeV0 MeV27 MeVDeposited: 26.201 MeV; neutrinos: 0.530 MeV mean.Total: 26.731 MeV. Mass-energy is conserved.

The gold energy segment is the stipulated mean carried away by two pp neutrinos, not a fixed energy for each event or a universal average over all fusion branches. Deposited energy can thermalize before escaping as photons. Nearly all initial fuel rest mass remains in helium.

Hypothetical available inventory and required demand rates
QuantitySelected demandSame inventory, 1 nominal solar luminosity
Accessible region kg2.00000e+292.00000e+29
Hydrogen inventory kg1.40000e+291.40000e+29
Possible net completions2.09138e+552.09138e+55
Helium product rest mass kg1.39003e+291.39003e+29
Total released budget J8.95692e+438.95692e+43
Neutrino budget J1.77591e+421.77591e+42
Deposited budget J8.77933e+438.77933e+43
Prescribed photon demand W3.82800e+263.82800e+26
Required completions per second9.11894e+379.11894e+37
Required hydrogen processing kg/s6.10434e+116.10434e+11
Required rest-mass conversion kg/s4.34538e+94.34538e+9
Implied neutrino power at required rate W7.74338e+247.74338e+24
Conditional support duration Gyr7.267517.26751
Compare independent reservoirs · NOT a stellar time historyConditional support duration (Gyr) · solid/circle selected; dashed/square reference030609012015005101520Available core region (% of synthetic total mass)Hydrogen fraction fixed at 0.70. Long budget ≠ a physically predicted stellar lifetime.

Selected support budget: 7.26751 Gyr; same inventory at the reference demand: 7.26751 Gyr. The two curves coincide because their demands are equal. Each curve compares separate inventories; it does not show a core expanding over time.

Connect fuel, mass difference and power

Let q be the selected region percentage divided by 100. Available hydrogen mass is Mfuel = 0.70 × q × 2.0 × 10³⁰ kg. Count possible net completions as N = Mfuel / (4mH u), with mH = 1.00782503223 and u = 1.66053906892 × 10⁻²⁷ kg. The selected isotope mass differs from a natural-isotope average.

Mass defect per completion is Δm = (4mH − mHe)u, with mHe = 4.00260325413. Released energy is Qtotal = Δm c²; c = 299792458 m/s. Subtract the stipulated mean neutrino energy once: Qdeposit = Qtotal − Qν. One MeV = 1.602176634 × 10⁻¹³ J. Total deposited budget is N Qdeposit.

Divide that energy budget by prescribed average photon luminosity Lγ to obtain a duration in seconds. Divide by 31557600 and one billion to express Gyr. A required completion rate Lγ/Qdeposit is distinct from the amount of fuel. At 10% region and one nominal solar luminosity, 1.40 × 10²⁹ kg of hydrogen supplies about 8.77933 × 10⁴³ J deposited energy, a conditional 7.26751 Gyr budget.

This assumes all deposited energy supports the average photon demand, with no net storage change, mechanical loss or alternate source. Actual stellar temperature, density, mixing, luminosity history and other branches are absent. No present age, remaining lifetime or feasible reaction rate follows from this ratio.

Sources: isotope-specific masses from NIST hydrogen and helium; CODATA conversion constants; Berkeley pp-chain explanation; Fukugita and Peebles on neutrino energy; IAU nominal luminosity. Values use central reference constants without uncertainty propagation; displayed precision is not a new measurement.

Available hydrogen 1.4000e+29 kg; deposited budget 8.7793e+43 J; conditional support duration 7.2675 Gyr.

The prescribed photon demand would require 9.1189e+37 pp-I completions/s and 6.1043e+11 kg/s of hydrogen processing. These are demand-derived required rates, not actual output. The energy/power ratio is not a stellar lifetime prediction.

Captures preserve hypothetical fuel-region and photon-demand choices. Replaying calculates conditional energy budgets and required rates, not measured fusion output or actual stellar lifetimes.

Understand

Build the chain before counting the fuel

A stellar surface emits light, but a surface-radiation equation does not explain the energy source. This investigation follows one restricted nuclear pathway: the proton–proton I, or pp-I, chain. It connects a countable sequence of reactions to an energy budget. It does not calculate how rapidly a real core reacts.

Start with paper cards for protons, deuterons, helium-3 nuclei and helium-4 nuclei. A proton is a hydrogen nucleus. A deuteron contains one proton and one neutron; helium-3 contains two protons and one neutron; helium-4 contains two of each. Isotope names specify different neutron counts, not different chemical elements. Draw a separate place for emitted particles so they do not disappear from your accounting.

The Lawrence Berkeley National Laboratory pp-chain explanation supplies the physical sequence. Our cards and budget are teaching representations, not photographs of simultaneous reactions inside a star.

Follow three reactions and cancel intermediates

First, two protons produce a deuteron, a positron and an electron neutrino. This step occurs twice in the completed construction. A positron has positive charge and the electron’s mass; an electron neutrino is a different particle. The weak interaction permits the nuclear change involved here. It is not a chemical reaction that changes a proton’s charge by removing an orbital electron.

Next, each deuteron captures another proton and produces helium-3 plus a gamma photon. This step also occurs twice. Finally, two helium-3 nuclei combine to produce helium-4 and return two protons. Write the multiplicity beside every arrow before adding your cards.

Six protons entered the first two stages, but two came back in the final stage. Net consumption is therefore six minus two, or four protons. Cancel the deuterons and helium-3 nuclei because they are produced and subsequently consumed. The resulting nuclear inventory contains one helium-4 nucleus, two positrons and two electron neutrinos. A completed chain is not one four-proton collision.

Account for surrounding electrons

The energy ledger uses neutral atomic masses. Its net bookkeeping compares four neutral hydrogen-1 atoms with one neutral helium-4 atom, neutrinos and released energy. Real core material is ionized; the neutral-atom convention is an accounting choice, not a picture of intact hydrogen atoms in the core.

Count the four initial electrons. Two remain in the final neutral-helium inventory. Two annihilate with the two produced positrons, transferring rest energy into radiation. Because the tabulated atomic masses already include this net electron inventory, adding a separate electron-rest-mass bonus would double-count energy. Keep the nuclear reaction cards and neutral-atom mass ledger visibly distinct.

For your paper check, draw four electron marks beside the initial atoms. Connect two to helium and two to the annihilation step. Explain why there is no surplus electron to add to the final mass total. The neutrinos remain in the energy ledger even though this model assumes they escape.

Change the reservoir, not the nuclear identity

In the lab, leave prescribed average photon luminosity at one nominal solar luminosity. Compare available core regions of 5 and 10 percent. Predict which quantities double. Capture both cases: total hydrogen inventory and possible completions double, while energy per completed chain and the reaction diagram remain unchanged.

The reservoir setting does not change proton mass, select another fusion branch or measure a real core boundary. The Department of Energy pp-fusion summary provides nuclear-physics context. Energy released per completion is different from the probability or rate of that completion. Temperature, density and reaction physics would be needed to determine an achieved rate.

Transfer: repair a missing return arrow

An unfamiliar reaction worksheet counts twelve protons supplied to two completed pp-I constructions. It reports twelve protons permanently consumed and two helium-4 nuclei produced. Identify the omitted output and repair the net inventory before opening the explanation. This is public practice, not an independently assessed mastery task.

Check the fusion-chain transfer

Each construction returns two protons, so two constructions return four. Twelve supplied minus four returned gives eight protons consumed overall, producing two helium-4 nuclei. The complete nuclear ledger also has four positrons and four electron neutrinos. The neutral-atom energy ledger must account consistently for the corresponding electrons.

Apply

One completed pp-I construction consumes how many protons overall?

Public practice checks a specific claim. It does not establish independent mastery.

Explain why the reaction identity stays fixed while possible completions scale.

Continue

Completion requires a saved prediction, at least one capture and a reflection. Presence checks do not grade your reasoning.

Skipping retains experiments and awards no mastery.

Save a science backup or import one

Science work is stored locally in this browser, separately from mathematics and AI. It does not sync automatically. Use this science-only backup; this checkout's older all-subject export does not include science.

A legacy file is available only when the complete snapshot fits the 36 MB limit. For larger snapshots, prepare a complete file set below; never discard notebooks to make a smaller file.

Matching imported notebook drafts replace their current drafts. Omitted lessons and known first attempts remain. Export your current work first if you want to retain both drafts.

Complete file sets and course backups

A file set can hold more work than one science file. Keep its manifest and every part together. Each file is limited to 36 MB. This format needs this version of LearnAI or a compatible newer version; older versions can use only the legacy single-file backup above.

The set includes every saved science course and global continuation at this moment. Later edits need a new export. A conflicting tab exports its own visible work, which may differ from saved work in another tab.

0 file(s) selected. File order and filenames do not determine identity. Missing, changed or conflicting parts block the entire restore; no good part is applied by itself.

Science storage: loading. No account or remote computation is required.