Universe timeT+ 0 Myr

Star Simulation

Simulate a star through its stellar life stages.

Input the mass and metallicity of a star, and this simulation will simulate the progression of stellar life. This is based on science* instead of CLT, surnames, and birth dates.

01

Inputs

Create a Universe star

Metallicity model
ZAMS temperature scale1×ZAMS radius scale1×

The first star will begin the simulation at T+0. Change this in Settings.

ZAMS stellar resultSol · zero-age main-sequence reference
Universe[Fe/H] 0
ZAMS temperature5,555.211 K

ZAMS classification

Sol

G7 VZAMS class

Main Sequence · reached 40.012471 Myr after formation

[Fe/H] 0
Evolutionary pathRGB → He ignition / clump / AGB
Zero-age main sequenceZAMS measurements
Hover, focus, or tap a convertible measurement
Effective temperature5,555.211KConverted measurement5,282.061°C
Radius0.853793R☉Converted measurement593,983.786km
Mass1M☉Converted measurement1.988470e+30kg
Luminosity0.625464L☉Converted measurement2.394276e+26W
Core hydrogen0.715414mass fraction
Absolute Mbol5.249494mag
Apparent Mbol · 1 AU-26.322631mag
Mean density2.265201g/cm³
Calculation traceFollow mass and metallicity from input to the ZAMS stellar resultUniverse model
A compact four-step ZAMS result path
01 · Input1 M☉

[Fe/H] 0 defines the starting composition model.

02 · Composition1× Teff

Radius scale 1× is applied to the mass-calibrated ZAMS base.

03 · Stellar trackG7 V

RGB → He ignition / clump / AGB reaches Main Sequence after 40.012471 Myr.

04 · ZAMS result5,555.211 K

0.853793 R☉ · 1 M☉ · 0.625464 L☉.

Realistic-scale time traveller

T+ 0 Myr

The Universe clock is paused.

Live stellar distribution

Hertzsprung–Russell diagram

View the positions of your stars on this graph.

0 plotted

Matching stars will appear here for one-click highlighting.

Search above, select a leaderboard star, or select its point in the diagram.

Formation fade Logarithmic axes Birth-to-delisting path
Plot shape
Fit screen
Luminosity (L☉)
Add a Universe star to plot it here.
Effective temperature (K) · hotter to cooler

Both axes are logarithmic. Select a point to highlight its birth-to-delisting trajectory; select it again to clear. Hold a point for one second to open its full specifications. Hover or focus for its name, SpectralC, Teff, and luminosity. Protostars and pre-main-sequence stars fade in as they form. Every Universe star follows one natural lifecycle: its final fade uses the physical-age interval corresponding to the reference track’s last 116.9–117 checkpoints, then the point, hover tag, and highlighted path delist together. Universe uses no alternate death-type selector. Values beyond 100–200,000 K or 10−6–107 L☉ are pinned to the nearest edge.

Live simulation registry

Stellar leaderboard

Universe stars follow the shared realistic-scale clock and are ranked by the selected physical property.

0 stars

No Universe stars added

Enter a display name and stellar mass above. The first simulation entry will begin at t+0 years.

Important model limitation

Scientific inaccuracy notice

Universe mode is an educational approximation based on representative, approximately solar-metallicity single-star tracks. A star’s real evolution depends on composition, rotation, mass loss, magnetic activity, multiplicity, and the exact stellar model.

The [Fe/H] temperature curve is a smooth game approximation informed by MIST/PARSEC. Finite-metallicity ZAMS radii use the Tout et al. (1996) fit; extreme metallicity bins are clamped to its calibrated range. Population III temperatures and massive-star radii use the workbook’s separate Schaerer-based model. Stage timing follows the physical-age track and is not recalibrated by metallicity.

Mass-to-spectrum mapping, stage timing, late-stage outcomes, temperature, radius, mass, luminosity, and hydrogen values may differ substantially from a matched stellar-model analysis. Displayed precision is computational precision, not physical certainty. Do not use these values for research, engineering, navigation, or safety-critical decisions.

Universe Stellar Simulation
01Local registry

Mass, metallicity, and star records remain in this browser.

02Stellar time travel

Move every saved star through realistic-scale stellar ages.

03Star records

Open profiles, H–R paths, measurements, and size comparisons.

*Science-based educational approximation; not a complete stellar-evolution model.

Universe roadmapModel expansion in progress

Additional tracks, endpoints, and interface parity are in development.

Universe Simulation · Operation Charlotte Dynamics

Copyright 2,026 A. D. OCharlotteD, all rights reserved.

Simulation informationUniverse stellar simulationPhysical-age calibrated tracks[Fe/H] + Population IIILocal browser registry

Charlotteverse acknowledgements

Credits

Software, visual-asset, workbook, stellar-color, planetary-atmosphere, and gravity-model acknowledgements.

01

Visual software and assets

SpaceEngine

Planet surface imagery and cosmic visual assets generated using SpaceEngine software.

SpaceEngine software modification code is credited to Cosmographic Software LLC.

Copyright © Cosmographic Software LLC. All rights reserved.

Used on this website for personal, non-commercial virtual exhibits in accordance with the SpaceEngine End User License Agreement.

02

Scientific model references

Stellar workbook sources

The simulation workbook draws on stellar-model grids, empirical calibrations, evolutionary literature, and the Charlotteverse Codex. References below use MLA 9 style.

View all 75 workbook sources
  1. “CVRS System 5 Beta 5.” Charlotteverse Internal Documentation, 2026.User-provided source workbook for revised dense age interpolation, 150 S stages, 20 variability profiles, expanded terminal-path sampling, state-aware quick cycles, and updated post-death remnant grids.
  2. “CVRS System 5.2 — S-Stage Definitions.” Charlotteverse Internal Documentation, 2026.User-provided scientific definitions for stages S001–S119 at [Fe/H] = 0.00; Beta 5 supplies the authoritative stage names and stages S120–S150 in its embedded SVP codebook.
  3. Nauenberg, Michael. “Analytic Approximations to the Mass-Radius Relation and Energy of Zero-Temperature Stars.” The Astrophysical Journal, vol. 175, 1972, p. 417, doi.org/10.1086/151568. Accessed 31 Aug. 2026.System 5 Beta 5 white-dwarf radius relation.
  4. Fontaine, Gilles, Pierre Brassard, and Pierre Bergeron. “The Potential of White Dwarf Cosmochronology.” Publications of the Astronomical Society of the Pacific, vol. 113, 2001, pp. 409–435, doi.org/10.1086/319535. Accessed 31 Aug. 2026.White-dwarf cooling, crystallization, and cooling-age context.
  5. Bédard, Antoine, et al. “Evolutionary Sequences of White Dwarfs.” 2020, www.astro.umontreal.ca/~bergeron/CoolingModels. Accessed 31 Aug. 2026.Modern mass-dependent DA/DB cooling sequences used by the workbook.
  6. Yakovlev, Dmitry G., and Craig J. Pethick. “Neutron Star Cooling.” Annual Review of Astronomy and Astrophysics, vol. 42, 2004, pp. 169–210, arxiv.org/abs/astro-ph/0402143. Accessed 31 Aug. 2026.Neutrino, photon, superfluid, and direct-Urca cooling regimes.
  7. Potekhin, Alexander Y., et al. “Thermal Luminosities of Cooling Neutron Stars.” Space Science Reviews, vol. 216, 2020, arxiv.org/abs/2006.15004. Accessed 31 Aug. 2026.Observed age-temperature spread and modern neutron-star cooling constraints.
  8. Hawking, Stephen W. “Particle Creation by Black Holes.” Communications in Mathematical Physics, vol. 43, 1975, pp. 199–220, doi.org/10.1007/BF02345020. Accessed 31 Aug. 2026.Nonzero Hawking temperature; stellar-mass values display as 0.000 K at three decimals.
  9. Kalirai, Jasonjot S., et al. “The Initial-Final Mass Relation: Direct Constraints at the Low-Mass End.” The Astrophysical Journal, vol. 676, 2008, pp. 594–609, arxiv.org/abs/0706.3894. Accessed 31 Aug. 2026.White-dwarf remnant-mass calibration in its applicable progenitor range.
  10. “MIST overview and grid scope / model-grid and EEP documentation.” MIST, mist.science. Accessed 31 Aug. 2026.
  11. “MIST solar-scaled models / stellar tracks.” arXiv, arxiv.org/abs/1604.08592. Accessed 31 Aug. 2026.
  12. “Equivalent Evolutionary Points (EEPs).” arXiv, arxiv.org/abs/1601.05144. Accessed 31 Aug. 2026.
  13. “Mamajek Mean Dwarf Spectral Sequence.” GitHub, raw.githubusercontent.com/emamajek/SpectralType/master/EEM_dwarf_UBVIJHK_colors_Teff.txt. Accessed 31 Aug. 2026.
  14. “Geneva rotating massive-star grid.” NASA Astrophysics Data System, ui.adsabs.harvard.edu/abs/2012A%26A...537A.146E/abstract. Accessed 31 Aug. 2026.
  15. “Galactic red-supergiant temperature scale.” arXiv, arxiv.org/abs/astro-ph/0504337. Accessed 31 Aug. 2026.
  16. “Super-AGB review.” arXiv, arxiv.org/abs/1703.06895. Accessed 31 Aug. 2026.
  17. “PARSEC-COLIBRI TP-AGB isochrones.” arXiv, arxiv.org/abs/1701.08510. Accessed 31 Aug. 2026.
  18. “Low-mass end of the main sequence.” arXiv, arxiv.org/abs/astro-ph/9701131. Accessed 31 Aug. 2026.
  19. “Modern post-AGB evolutionary models.” arXiv, arxiv.org/abs/1512.04129. Accessed 31 Aug. 2026.
  20. “Empirical late-K/M radius calibration.” arXiv, arxiv.org/abs/1501.01635. Accessed 31 Aug. 2026.
  21. “Post-AGB timescale review.” arXiv, arxiv.org/abs/1910.01013. Accessed 31 Aug. 2026.
  22. “Massive-star death and compact remnants.” arXiv, arxiv.org/abs/astro-ph/0212469. Accessed 31 Aug. 2026.
  23. “Spectroscopic evolution of massive main-sequence stars.” arXiv, arxiv.org/abs/1612.03044. Accessed 31 Aug. 2026.
  24. “Core-hydrogen-burning WNh phase.” arXiv, arxiv.org/abs/0802.1742. Accessed 31 Aug. 2026.
  25. “Charlotteverse Codex — Titles XI, XV, and non-Charlotte brown-dwarf rules.” Charlotteverse Internal Documentation, 2026.Internal source: CHARLOTTEVERSELAW_Rule92_Applied(2).docx
  26. “Ultracool-dwarf fundamental parameters.” arXiv, arxiv.org/abs/1508.01767. Accessed 31 Aug. 2026.
  27. “Brown-dwarf cooling models.” arXiv, arxiv.org/abs/astro-ph/9705201. Accessed 31 Aug. 2026.
  28. “Deuterium-burning mass limit.” arXiv, arxiv.org/abs/1008.5150. Accessed 31 Aug. 2026.
  29. “Galactic O-star calibration.” Astronomy & Astrophysics, www.aanda.org/articles/aa/abs/2005/24/aa2386-04/aa2386-04.html. Accessed 31 Aug. 2026.
  30. “Physical properties of Wolf–Rayet stars.” arXiv, arxiv.org/abs/astro-ph/0610356. Accessed 31 Aug. 2026.
  31. “LMC WN-star analysis.” arXiv, arxiv.org/abs/1401.5474. Accessed 31 Aug. 2026.
  32. “Pre-supernova progenitor appearances.” Astronomy & Astrophysics, www.aanda.org/articles/aa/abs/2013/10/aa21906-13/aa21906-13.html. Accessed 31 Aug. 2026.
  33. “Geneva rotating pre-supernova massive-star models.” arXiv, arxiv.org/abs/astro-ph/0406552. Accessed 31 Aug. 2026.
  34. “Wolf–Rayet progenitor of iPTF13bvn.” arXiv, arxiv.org/abs/1307.8434. Accessed 31 Aug. 2026.
  35. “MIST EEP track structure and phase definitions.” MIST, mist.science/read_mist_models_demo.html. Accessed 31 Aug. 2026.
  36. “PARSEC V2.0 low/intermediate-mass rotating tracks.” arXiv, arxiv.org/abs/2207.08642. Accessed 31 Aug. 2026.
  37. “CHARA early-type interferometry.” arXiv, arxiv.org/abs/1306.5937. Accessed 31 Aug. 2026.
  38. “MIST model grids.” MIST, mist.science/model_grids.html. Accessed 31 Aug. 2026.
  39. “A/F/G/K interferometric radii.” CaltechAUTHORS, authors.library.caltech.edu/records/d028v-bdb51. Accessed 31 Aug. 2026.
  40. “K/M interferometric radii.” arXiv, arxiv.org/abs/1208.2431. Accessed 31 Aug. 2026.
  41. “Main-sequence mass-radius-luminosity relations.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/479/4/5491/5056185. Accessed 31 Aug. 2026.
  42. “Kepler red-giant asteroseismic catalog.” arXiv, arxiv.org/abs/1802.04455. Accessed 31 Aug. 2026.
  43. “Red giants in eclipsing binaries.” arXiv, arxiv.org/abs/1609.06645. Accessed 31 Aug. 2026.
  44. “Theoretical tip-of-the-red-giant-branch calibration.” arXiv, arxiv.org/abs/astro-ph/9703186. Accessed 31 Aug. 2026.
  45. “COLIBRI TP-AGB code.” arXiv, arxiv.org/abs/1305.4485. Accessed 31 Aug. 2026.
  46. “Modern O-star and early-B supergiant calibration.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/537/2/1197/7977024. Accessed 31 Aug. 2026.
  47. “Cygnus OB2 massive-star population.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/449/1/741/1324886. Accessed 31 Aug. 2026.
  48. “O7 spectral luminosity effects.” NASA/IPAC Extragalactic Database, ned.ipac.caltech.edu/level5/Gray/Gray4.html. Accessed 31 Aug. 2026.
  49. “Physical parameters of Galactic early-B supergiants.” Astronomy & Astrophysics, www.aanda.org/articles/aa/full/2006/04/aa3685-05/aa3685-05.html. Accessed 31 Aug. 2026.
  50. “Galactic B0–B5 supergiant spectroscopy.” arXiv, arxiv.org/abs/0801.4289. Accessed 31 Aug. 2026.
  51. “Core-collapse progenitor appearances.” arXiv, arxiv.org/abs/1308.4681. Accessed 31 Aug. 2026.
  52. “Red-supergiant progenitor luminosity limit.” arXiv, arxiv.org/abs/0809.1881. Accessed 31 Aug. 2026.
  53. “SN 2024ggi red-supergiant progenitor.” arXiv, arxiv.org/abs/2405.07699. Accessed 31 Aug. 2026.
  54. “SN 2008bk red-supergiant progenitor.” arXiv, arxiv.org/abs/1308.4393. Accessed 31 Aug. 2026.
  55. “SN 2023ixf progenitor analysis.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/534/1/271/7746773. Accessed 31 Aug. 2026.
  56. “Galactic early-B supergiants — detailed table/page.” Astronomy & Astrophysics, www.aanda.org/articles/aa/full/2006/04/aa3685-05/aa3685-05.right.html. Accessed 31 Aug. 2026.
  57. “B1 endpoint implementation / remnant-scale / simulation-cap rules.” Charlotteverse Internal Documentation, 2026.Internal workbook rules.
  58. “15-solar-mass pre-supernova red-supergiant model.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/445/3/2492/1053248. Accessed 31 Aug. 2026.
  59. “Super-AGB final fates.” arXiv, arxiv.org/abs/1410.5431. Accessed 31 Aug. 2026.
  60. “MIST table phase identifiers.” MIST, mist.science/README_tables.pdf. Accessed 31 Aug. 2026.
  61. “Modern post-AGB sequences — A&A paper.” Astronomy & Astrophysics, www.aanda.org/articles/aa/pdf/2016/04/aa26577-15.pdf. Accessed 31 Aug. 2026.
  62. “Planetary-nebula visibility timescale.” arXiv, arxiv.org/abs/1307.6189. Accessed 31 Aug. 2026.
  63. “Supernova-remnant lifetime.” NASA, imagine.gsfc.nasa.gov/ask_astro/snr.html. Accessed 31 Aug. 2026.
  64. “Supernova-remnant evolutionary phases.” NASA, imagine.gsfc.nasa.gov/science/objects/supernova_remnants.html. Accessed 31 Aug. 2026.
  65. “Montreal white-dwarf cooling tracks.” Montreal White Dwarf Database, www.montrealwhitedwarfdatabase.org/evolution.html. Accessed 31 Aug. 2026.
  66. “Old white-dwarf cooling models.” arXiv, arxiv.org/abs/1005.2170. Accessed 31 Aug. 2026.
  67. “Neutron-star cooling review.” Annual Reviews, www.annualreviews.org/content/journals/10.1146/annurev.astro.42.053102.134013. Accessed 31 Aug. 2026.
  68. “Thermal neutron-star ages.” arXiv, arxiv.org/abs/astro-ph/0702426. Accessed 31 Aug. 2026.
  69. “Black-hole persistence.” NASA, science.nasa.gov/universe/10-questions-you-might-have-about-black-holes. Accessed 31 Aug. 2026.
  70. “Hawking black-hole lifetime scaling.” PubMed Central, pmc.ncbi.nlm.nih.gov/articles/PMC11353257. Accessed 31 Aug. 2026.
  71. “Supernova-remnant observational context — NASA/Hubble.” NASA, science.nasa.gov/missions/hubble/supernova-remnant. Accessed 31 Aug. 2026.
  72. “Modern white-dwarf cooling context.” arXiv, arxiv.org/abs/2410.14014. Accessed 31 Aug. 2026.
  73. “Blue loops during stellar evolution.” arXiv, arxiv.org/abs/1502.04311. Accessed 31 Aug. 2026.
  74. “Tip-of-the-red-giant-branch theory.” arXiv, arxiv.org/abs/1706.09910. Accessed 31 Aug. 2026.
  75. “Red-supergiant review.” arXiv, arxiv.org/abs/2507.15960. Accessed 31 Aug. 2026.
03

Color methodology

Stellar color index

Effective temperature → Planck blackbody spectrum → CIE 1931 XYZ matching → linear sRGB → sRGB transfer function → 8-bit RGB → hexadecimal color.

The sub-700 K #000000 behavior is an implementation visibility guardrail: it prevents a very weak visible tail from being normalized into a misleading bright color.

View color-science sources
  1. Ballesteros, F. J. “New Insights into Black Bodies.” arXiv, 2012, arxiv.org/abs/1201.1809. Accessed 31 Aug. 2026.Analytical effective-temperature ↔ Johnson B−V relationship.
  2. Wyman, Chris, Peter-Pike Sloan, and Peter Shirley. “Simple Analytic Approximations to the CIE XYZ Color Matching Functions.” Journal of Computer Graphics Techniques, vol. 2, no. 2, 2013, pp. 1–11, jcgt.org/published/0002/02/01. Accessed 31 Aug. 2026.Analytic approximations for the CIE x̄(λ), ȳ(λ), and z̄(λ) curves.
  3. International Commission on Illumination. “CIE 1931 Standard Colorimetric Observer: 2° Colour-Matching Functions.” CIE, doi.org/10.25039/CIE.DS.xvudnb9b. Accessed 31 Aug. 2026.Official CIE XYZ color-matching reference.
  4. National Institute of Standards and Technology. “Planck’s Law and Blackbody Spectral Radiance.” NIST, physics.nist.gov/cgi-bin/cuu/Value?c22ndrc. Accessed 31 Aug. 2026.Wavelength-dependent spectral output for effective temperature.
  5. World Wide Web Consortium. “CSS Color Module Level 4.” W3C, www.w3.org/TR/css-color-4. Accessed 31 Aug. 2026.D65 sRGB, XYZ conversion, transfer function, gamut handling, and hexadecimal output.
04

Planetary atmosphere methodology

Gas-giant coloration

The gas-giant palette weights observed ochre, tawny, cream, red-brown, pale-gold, and blue-gray families. Muted colors are common; vivid chromophore-rich variants and relatively clear blue-gray atmospheres are rarer.

These colors are an appearance model rather than a composition retrieval. Atmosphere, cloud, irradiation, particle-size, and viewing-phase effects can all change the visible spectrum.

View gas-giant coloration sources
  1. Irwin, Patrick G. J., et al. “Clouds and Ammonia in the Atmospheres of Jupiter and Saturn Determined From a Band-Depth Analysis of VLT/MUSE Observations.” Journal of Geophysical Research: Planets, vol. 130, 2025, e2024JE008622, doi.org/10.1029/2024JE008622. Accessed 31 Aug. 2026.True-color Jupiter and Saturn observations: common ochre appearance, white pure condensates, and light-blue aerosol-free models.
  2. Owen, Tobias, and Richard J. Terrile. “Colors on Jupiter.” Journal of Geophysical Research: Space Physics, vol. 86, no. A10, 1981, pp. 8797–8814, doi.org/10.1029/JA086iA10p08797. Accessed 31 Aug. 2026.Voyager-era evidence for stable latitude-linked white, tawny/brown, red, and blue-gray cloud coloration.
  3. Sudarsky, David, Adam S. Burrows, and Philip Pinto. “Albedo and Reflection Spectra of Extrasolar Giant Planets.” The Astrophysical Journal, vol. 538, no. 2, 2000, pp. 885–903, doi.org/10.1086/309160. Accessed 31 Aug. 2026.Temperature-dependent ammonia-, water-, clear-, alkali-, and silicate-cloud albedo classes.
  4. Sudarsky, David, Adam S. Burrows, and Ivan Hubeny. “Theoretical Spectra and Atmospheres of Extrasolar Giant Planets.” The Astrophysical Journal, vol. 588, no. 2, 2003, pp. 1121–1148, doi.org/10.1086/374331. Accessed 31 Aug. 2026.Atmospheric appearance dependencies on irradiation, clouds, mass, gravity, and composition.
  5. Burrows, Adam, David Sudarsky, and Ivan Hubeny. “Spectra and Diagnostics for the Direct Detection of Wide-Separation Extrasolar Giant Planets.” The Astrophysical Journal, vol. 609, no. 1, 2004, pp. 407–416, doi.org/10.1086/420974. Accessed 31 Aug. 2026.Consistent treatment of irradiation plus water and ammonia clouds in modeled giant-planet spectra.
  6. Sudarsky, David, et al. “Phase Functions and Light Curves of Wide-Separation Extrasolar Giant Planets.” The Astrophysical Journal, vol. 627, no. 1, 2005, pp. 520–533, doi.org/10.1086/430206. Accessed 31 Aug. 2026.Optical color varies with phase, cloud condensation, and cloud-particle size.
05

Interactive physics methodology

Gravity Simulator

Ball Drop uses classical radial free fall from rest. Acceleration changes continuously with center-to-center distance according to a = μ/r²; star mass and radius are converted from registry solar units using IAU nominal constants.

Tug of War sums Newtonian inverse-square acceleration from every fixed stellar anchor and advances a massless probe in two dimensions with velocity-Verlet integration. The visual spheres are normalized for legibility, while first-contact detection uses each star’s physical radius.

Atmosphere, drag, stellar motion and mutual star–star gravity, probe feedback, tidal deformation, post-impact behavior, and relativistic corrections are outside this model. Very large time multipliers intentionally trade short-timescale integration detail for speed.

View gravity-model sources
  1. International Astronomical Union. “Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties.” XXIX General Assembly, 2015, www.iau.org/common/Uploaded%20files/IAUGA2015-Resolution-B3-recommended-nominal-conversion.pdf. Accessed 31 Aug. 2026.Defines the exact nominal solar radius (6.957 × 10⁸ m) and nominal solar mass parameter (1.3271244 × 10²⁰ m³ s⁻²) used to convert registry values to SI units.
  2. NASA Engineering and Safety Center Academy. “Gravity Models: Inverse Square Gravitation.” NASA, nescacademy.nasa.gov/flightsim/2015/gravity. Accessed 31 Aug. 2026.Reference for the classical inverse-square acceleration model and the gravitational parameter μ = GM.
  3. NASA Goddard Space Flight Center. “Newton’s Law of Gravitation.” Neil Gehrels Swift Learning Center, NASA, imagine.gsfc.nasa.gov/observatories/learning/swift/classroom/law_grav_guide.html. Accessed 31 Aug. 2026.Derives acceleration from F = ma and F = GMm/r², showing that ideal free-fall acceleration is independent of the falling object’s mass.
89 scientific and color references listed.

Charlotteverse development schedule

Roadmap

Planned public additions for September 2026.

Release window

September 2026

In active design and development. Timing and exact behavior may evolve during testing.

  1. 01
    Coming-soon Play Labs

    Orbit Works moves from a locked preview into an active orbital experiment.

    Planned
  2. 02
    Charlotteverse chatbot

    An AI guide for site tools, registry records, and Charlotteverse reference material.

    Planned
  3. 03
    More planet textures

    Additional surface and atmospheric texture families expand CVRG/P variety.

    Planned
  4. 04
    More star reference objects

    The shared object catalog gains more recognizable stellar scale references.

    Planned
  5. 05
    Star references in the leaderboard

    Reference stars become available directly from leaderboard workflows.

    Planned