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UniversePhysical-age modeling
Universe timeT+ 0 Myr

Model inspector

Instantaneous physical state and input parameters.

H–R diagram

Documentation index

Scientific approximations and project information, separate from the working catalogue.

01 / PROVENANCEModel sources

Edition identifiers and simulation metadata.

02 / SCOPELimitations & notices

Physical assumptions and composition handling.

03 / PROJECTData & project

Local data, documentation, credits and project links.

01

Model parameters

Metallicity model

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

ZAMS stellar result
Universe[Fe/H] 0
ZAMS temperature5,852.89 K

ZAMS classification

Sol

G1 VZAMS class

ZAMS / core hydrogen ignition · reached 50 Myr after formation

[Fe/H] 0
Evolutionary pathP05
Zero-age main sequenceZAMS measurements
Hover, focus, or tap a convertible measurement
Effective temperature5,852.89KConverted measurement5,579.74°C
Radius0.916686R☉Converted measurement637,738.109km
Mass1M☉Converted measurement1.988470e+30kg
Bolometric luminosity0.888417L☉Converted measurement3.400861e+26W

Structure & photometry

Core hydrogen0.7121mass fraction
Absolute Mbol4.868457mag
Apparent Mbol · 1 AU-26.703668mag
Mean density1.83022g/cm³
Calculation detailsPhysical model & calibration
Calculation traceFollow mass and composition metadata 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 · CompositionMetadata only

No generic temperature or radius multiplier is applied to the base stellar track.

03 · Stellar trackG1 V

P05 reaches ZAMS / core hydrogen ignition after 50 Myr.

04 · ZAMS result5,852.89 K

0.916686 R☉ · 1 M☉ · 0.888417 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.

Plot settings Frame & reference stars
Formation fade Logarithmic axes Birth-to-delisting path
Plot shape
Fit screen
Bolometric luminosity (L☉)
Add a Universe star to plot it here.
Effective temperature (K) · hotter to cooler
How to read this diagram

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 catalogue

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

Manage

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.

Composition is retained as descriptive metadata in Universe mode. The old generic [Fe/H] and Population III temperature/radius multipliers have been removed, so the base System 5 track is unchanged by this selection.

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.

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 76 workbook sources
  1. “CVRS System 5.1.5 — Default automatic routing.” Charlotteverse Internal Documentation, 2026.Uses the checksum-pinned 5.1.3 source revision with stage-aware spectral qualifiers, covered WD handoff repairs and M3/M4 pre-WD thermal-shape proxies from the supplied 0.10/0.18-Msun Z=0.02 runs. The four revised metallicities are −0.10, 0.00, +0.10 and +0.25. Results identify their data as 5.1.5, 5 Beta 9 or Hybrid. Shared base sensitivity, shape corrections, qualifier thresholds and human-age clocks are labeled CVRS conventions/proxies, not new complete published evolution grids or measured spectra.
  2. “CVRS System 5 Beta 9 — Unupdated metallicity compatibility data.” Charlotteverse Internal Documentation, 2026.All previous selections, CSV imports and API calculations migrate to the 5.1.5 compatibility policy. Only metallicities without updated compatible data retain Beta 9 sources; mixed old/new brackets are Hybrid. There is no manual legacy-only mode. Beta 6 was a version-label error. This is a fictional stellar model, not a calibrated physical prediction.
  3. “CVRS System 5.2 — S-Stage Definitions.” Charlotteverse Internal Documentation, 2026.Earlier user-provided stage definitions. Active editions supply their embedded SVP codebooks.
  4. 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 9 white-dwarf radius relation.
  5. 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.
  6. 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.
  7. 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.
  8. 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.
  9. 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.
  10. 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.
  11. “MIST overview and grid scope / model-grid and EEP documentation.” MIST, mist.science. Accessed 31 Aug. 2026.
  12. “MIST solar-scaled models / stellar tracks.” arXiv, arxiv.org/abs/1604.08592. Accessed 31 Aug. 2026.
  13. “Equivalent Evolutionary Points (EEPs).” arXiv, arxiv.org/abs/1601.05144. Accessed 31 Aug. 2026.
  14. “Mamajek Mean Dwarf Spectral Sequence.” GitHub, raw.githubusercontent.com/emamajek/SpectralType/master/EEM_dwarf_UBVIJHK_colors_Teff.txt. Accessed 31 Aug. 2026.
  15. “Geneva rotating massive-star grid.” NASA Astrophysics Data System, ui.adsabs.harvard.edu/abs/2012A%26A...537A.146E/abstract. Accessed 31 Aug. 2026.
  16. “Galactic red-supergiant temperature scale.” arXiv, arxiv.org/abs/astro-ph/0504337. Accessed 31 Aug. 2026.
  17. “Super-AGB review.” arXiv, arxiv.org/abs/1703.06895. Accessed 31 Aug. 2026.
  18. “PARSEC-COLIBRI TP-AGB isochrones.” arXiv, arxiv.org/abs/1701.08510. Accessed 31 Aug. 2026.
  19. “Low-mass end of the main sequence.” arXiv, arxiv.org/abs/astro-ph/9701131. Accessed 31 Aug. 2026.
  20. “Modern post-AGB evolutionary models.” arXiv, arxiv.org/abs/1512.04129. Accessed 31 Aug. 2026.
  21. “Empirical late-K/M radius calibration.” arXiv, arxiv.org/abs/1501.01635. Accessed 31 Aug. 2026.
  22. “Post-AGB timescale review.” arXiv, arxiv.org/abs/1910.01013. Accessed 31 Aug. 2026.
  23. “Massive-star death and compact remnants.” arXiv, arxiv.org/abs/astro-ph/0212469. Accessed 31 Aug. 2026.
  24. “Spectroscopic evolution of massive main-sequence stars.” arXiv, arxiv.org/abs/1612.03044. Accessed 31 Aug. 2026.
  25. “Core-hydrogen-burning WNh phase.” arXiv, arxiv.org/abs/0802.1742. Accessed 31 Aug. 2026.
  26. “Charlotteverse Codex — Titles XI, XV, and non-Charlotte brown-dwarf rules.” Charlotteverse Internal Documentation, 2026.Internal source: CHARLOTTEVERSELAW_Rule92_Applied(2).docx
  27. “Ultracool-dwarf fundamental parameters.” arXiv, arxiv.org/abs/1508.01767. Accessed 31 Aug. 2026.
  28. “Brown-dwarf cooling models.” arXiv, arxiv.org/abs/astro-ph/9705201. Accessed 31 Aug. 2026.
  29. “Deuterium-burning mass limit.” arXiv, arxiv.org/abs/1008.5150. Accessed 31 Aug. 2026.
  30. “Galactic O-star calibration.” Astronomy & Astrophysics, www.aanda.org/articles/aa/abs/2005/24/aa2386-04/aa2386-04.html. Accessed 31 Aug. 2026.
  31. “Physical properties of Wolf–Rayet stars.” arXiv, arxiv.org/abs/astro-ph/0610356. Accessed 31 Aug. 2026.
  32. “LMC WN-star analysis.” arXiv, arxiv.org/abs/1401.5474. Accessed 31 Aug. 2026.
  33. “Pre-supernova progenitor appearances.” Astronomy & Astrophysics, www.aanda.org/articles/aa/abs/2013/10/aa21906-13/aa21906-13.html. Accessed 31 Aug. 2026.
  34. “Geneva rotating pre-supernova massive-star models.” arXiv, arxiv.org/abs/astro-ph/0406552. Accessed 31 Aug. 2026.
  35. “Wolf–Rayet progenitor of iPTF13bvn.” arXiv, arxiv.org/abs/1307.8434. Accessed 31 Aug. 2026.
  36. “MIST EEP track structure and phase definitions.” MIST, mist.science/read_mist_models_demo.html. Accessed 31 Aug. 2026.
  37. “PARSEC V2.0 low/intermediate-mass rotating tracks.” arXiv, arxiv.org/abs/2207.08642. Accessed 31 Aug. 2026.
  38. “CHARA early-type interferometry.” arXiv, arxiv.org/abs/1306.5937. Accessed 31 Aug. 2026.
  39. “MIST model grids.” MIST, mist.science/model_grids.html. Accessed 31 Aug. 2026.
  40. “A/F/G/K interferometric radii.” CaltechAUTHORS, authors.library.caltech.edu/records/d028v-bdb51. Accessed 31 Aug. 2026.
  41. “K/M interferometric radii.” arXiv, arxiv.org/abs/1208.2431. Accessed 31 Aug. 2026.
  42. “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.
  43. “Kepler red-giant asteroseismic catalog.” arXiv, arxiv.org/abs/1802.04455. Accessed 31 Aug. 2026.
  44. “Red giants in eclipsing binaries.” arXiv, arxiv.org/abs/1609.06645. Accessed 31 Aug. 2026.
  45. “Theoretical tip-of-the-red-giant-branch calibration.” arXiv, arxiv.org/abs/astro-ph/9703186. Accessed 31 Aug. 2026.
  46. “COLIBRI TP-AGB code.” arXiv, arxiv.org/abs/1305.4485. Accessed 31 Aug. 2026.
  47. “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.
  48. “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.
  49. “O7 spectral luminosity effects.” NASA/IPAC Extragalactic Database, ned.ipac.caltech.edu/level5/Gray/Gray4.html. Accessed 31 Aug. 2026.
  50. “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.
  51. “Galactic B0–B5 supergiant spectroscopy.” arXiv, arxiv.org/abs/0801.4289. Accessed 31 Aug. 2026.
  52. “Core-collapse progenitor appearances.” arXiv, arxiv.org/abs/1308.4681. Accessed 31 Aug. 2026.
  53. “Red-supergiant progenitor luminosity limit.” arXiv, arxiv.org/abs/0809.1881. Accessed 31 Aug. 2026.
  54. “SN 2024ggi red-supergiant progenitor.” arXiv, arxiv.org/abs/2405.07699. Accessed 31 Aug. 2026.
  55. “SN 2008bk red-supergiant progenitor.” arXiv, arxiv.org/abs/1308.4393. Accessed 31 Aug. 2026.
  56. “SN 2023ixf progenitor analysis.” Monthly Notices of the Royal Astronomical Society, academic.oup.com/mnras/article/534/1/271/7746773. Accessed 31 Aug. 2026.
  57. “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.
  58. “B1 endpoint implementation / remnant-scale / simulation-cap rules.” Charlotteverse Internal Documentation, 2026.Internal workbook rules.
  59. “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.
  60. “Super-AGB final fates.” arXiv, arxiv.org/abs/1410.5431. Accessed 31 Aug. 2026.
  61. “MIST table phase identifiers.” MIST, mist.science/README_tables.pdf. Accessed 31 Aug. 2026.
  62. “Modern post-AGB sequences — A&A paper.” Astronomy & Astrophysics, www.aanda.org/articles/aa/pdf/2016/04/aa26577-15.pdf. Accessed 31 Aug. 2026.
  63. “Planetary-nebula visibility timescale.” arXiv, arxiv.org/abs/1307.6189. Accessed 31 Aug. 2026.
  64. “Supernova-remnant lifetime.” NASA, imagine.gsfc.nasa.gov/ask_astro/snr.html. Accessed 31 Aug. 2026.
  65. “Supernova-remnant evolutionary phases.” NASA, imagine.gsfc.nasa.gov/science/objects/supernova_remnants.html. Accessed 31 Aug. 2026.
  66. “Montreal white-dwarf cooling tracks.” Montreal White Dwarf Database, www.montrealwhitedwarfdatabase.org/evolution.html. Accessed 31 Aug. 2026.
  67. “Old white-dwarf cooling models.” arXiv, arxiv.org/abs/1005.2170. Accessed 31 Aug. 2026.
  68. “Neutron-star cooling review.” Annual Reviews, www.annualreviews.org/content/journals/10.1146/annurev.astro.42.053102.134013. Accessed 31 Aug. 2026.
  69. “Thermal neutron-star ages.” arXiv, arxiv.org/abs/astro-ph/0702426. Accessed 31 Aug. 2026.
  70. “Black-hole persistence.” NASA, science.nasa.gov/universe/10-questions-you-might-have-about-black-holes. Accessed 31 Aug. 2026.
  71. “Hawking black-hole lifetime scaling.” PubMed Central, pmc.ncbi.nlm.nih.gov/articles/PMC11353257. Accessed 31 Aug. 2026.
  72. “Supernova-remnant observational context — NASA/Hubble.” NASA, science.nasa.gov/missions/hubble/supernova-remnant. Accessed 31 Aug. 2026.
  73. “Modern white-dwarf cooling context.” arXiv, arxiv.org/abs/2410.14014. Accessed 31 Aug. 2026.
  74. “Blue loops during stellar evolution.” arXiv, arxiv.org/abs/1502.04311. Accessed 31 Aug. 2026.
  75. “Tip-of-the-red-giant-branch theory.” arXiv, arxiv.org/abs/1706.09910. Accessed 31 Aug. 2026.
  76. “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.
90 scientific and color references listed.

Charlotteverse development schedule

Roadmap

September 2026 additions and progress.

Release window

September 2026

Reference additions 04 and 05 are complete. Remaining plans may evolve during testing.

  1. 01
    Coming-soon Play Labs

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

    Planned
  2. 03
    More planet textures

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

    Planned
  3. 04
    More star reference objects

    The shared object catalog gains more recognizable stellar scale references.

    Completed
  4. 05
    Star references in the leaderboard

    Reference stars become available directly from leaderboard workflows.

    Completed