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Sandbox Physics

Cosmic Reionization

How does starlight reionize cosmic hydrogen? Ultraviolet light escaping young galaxies ionizes intergalactic hydrogen. More escaped light grows the ionized volume; recombination uses some of that supply again. As neighbouring ionized regions meet, less neutral hydrogen remains to produce a 21 cm signal.

Move sources and compare ionized regions with their ideal radio signal.

Interactive modelCosmic Reionization
Ionized volume45.8%45.8\%
Redshift8.648.64
Mean ideal radio brightness14.3 mK14.3\,\mathrm{mK}
Recombinations per hydrogen nucleus0.1210.121
Scientific sources and fixed-record methods

The original synthetic fields and standalone Python methods include all five fixed records, 325 full-precision fields, provenance, licences and labelled numerical evidence. The scripts can inspect a field with the Python standard library or rerun the full fixed model with the declared numerical packages.

Download the fixed-source data and methods (3.90 MB ZIP)

Follow a photon from a galaxy to the gas

BackgroundYoung stars emit ultraviolet light. Some escapes the galaxy and can separate an electron from a hydrogen atom. Near a source, an ionized region grows into the surrounding neutral gas.

Why it mattersCounting emitted photons is only the beginning: electrons and protons can recombine, requiring another photon to maintain the same ionized volume.

Focus question
What changes the amount of ionized gas, and what changes its shape?
One-sentence intuition
In this uniform two-phase model, the source supply and common recombination budget fix the total ionized volume. Source positions decide where that volume is allocated. Moving sources can change the map without changing the global count.

Core mathematical model

Balance ionization and recombination

dQdt=fesc∑sN˙sNH−Qtrec,trec−1=CαBnˉH,0a−3\frac{dQ}{dt}=\frac{f_{\rm esc}\sum_s\dot N_s}{N_{\rm H}}-\frac{Q}{t_{\rm rec}},\qquad t_{\rm rec}^{-1}=C\alpha_{\rm B}\bar n_{{\rm H},0}a^{-3}

The ionized volume fraction grows with escaped light. Divide the escaped photon rate by the fixed number of hydrogen nuclei in the comoving box. Recombination acts in the fully ionized phase; expansion reduces its physical density. At full ionization, additional supply becomes surplus.

Keep all four counts

E=Q+R+U,⟨q⟩V=QE=Q+R+U,\qquad \langle q\rangle_V=Q

All counts are per hydrogen nucleus: escaped supply is split into retained ionizations, cumulative recombinations and surplus. The equal-volume cell mean must match retained ionizations at that same time. The scene distributes net new ionized volume instantaneously; it is not a finite-speed radiation front.

Read the remaining neutral gas

δTb(x)=T0(z)[1−q(x)],PT(k)=T0(z)2P1−q(k)\delta T_b(\mathbf x)=T_0(z)[1-q(\mathbf x)],\qquad P_T(k)=T_0(z)^2P_{1-q}(k)

This ideal radio map additionally assumes high neutral spin temperature, an optically thin coeval cube and a pure Hubble velocity gradient. It comes from the same completed cell field. The power chart averages only the declared four finite-box mode families.

Common difficulties

Half the volume is a phase statement

Typical misconceptionEvery atom is halfway ionized.

Better mental modelA cell contains a volume share of fully ionized gas and a share of neutral gas. This differs from treating every parcel as microscopically partially ionized, which changes recombination counting.

A changed shape can have the same mean

Typical misconceptionMoving two sources together must ionize more gas.

Better mental modelThe prescribed uniform budget is unchanged by source position. Overlap redistributes the available volume. Local density and local recombination would require additional physics.

A radio map needs its own assumptions

Typical misconceptionThe ionized gas temperature establishes the neutral spin temperature.

Better mental modelThey describe different gas and different physics. High neutral spin temperature is an extra idealization here; heating, spin coupling and an instrument are not calculated.

Run the experiment

  1. 01

    Watch neighbouring regions meet

    Let Bubbles meet play, then pause at an intermediate time.

    What to observe: The gold sources stay fixed while ionized volume grows. The neutral-hydrogen slice and photon counts refer to the same completed field and time.
  2. 02

    Compare a common cosmic time

    Compare Less light escapes and Gas recombines faster with Bubbles meet. Pause before changing a preset if you want to inspect the initial comparison.

    What to observe: Each preset starts at the same comparison time. Less supply or faster recombination leaves less ionized gas. Their saved scientific representative frames remain separately documented.
  3. 03

    Move the source pattern

    Drag a gold source, or compare Starlight spread out with Bubbles meet.

    What to observe: The topology and finite-mode power can change while the common global budget stays fixed. Dragging uses the visibly labelled coarse exploration.
  4. 04

    Keep the completed result

    Open Slice, resolution and download, move the slice, then download.

    What to observe: The result includes the whole three-dimensional Float64 cell field, settings, physical clock, counters and mode coefficients. Changing the viewing slice does not change those data.

Related experiments and articles

What this page links to directly

Starlight and intergalactic hydrogen · Reading path

Photons, ionized volume and a radio signal

Articles on this path that use this experiment, followed by the other experiments they suggest.

  1. ArticleHow starlight changes intergalactic hydrogen
  2. ArticleWhat does half ionized mean?
  3. ArticleSupplying photons to an expanding volume
  4. ArticleWhere the photons go when ionized bubbles meet
  5. ArticleReading ionized bubbles through neutral hydrogen
  6. ArticleRecompute a fixed-source ionization history
  7. ArticleReading HERA's 21 cm upper limits
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