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Random freezes, missing sound and display glitches usually trace back to one bad driver. Find and replace yours safely.Free scan · under a minuteTo compare exoplanets by habitability, use the same public catalog and parameter convention for every planet, then compare stellar energy received, planet size or mass, host-star properties, and orbital eccentricity—with uncertainties and sources visible. Treat a habitable-zone label or Earth Similarity Index (ESI) as a screening aid, not evidence that a planet is habitable or inhabited.
Start with a consistent, reproducible dataset
NASA’s Exoplanet Archive is a public, literature-linked starting point for planet and host-star parameters. Its tables support interactive filtering and export, and the archive also provides programmatic access. The archive describes its confirmed-planet criteria as focusing on objects with public planetary and orbital properties—usually from refereed papers—and an unambiguous planetary status. See the archive overview and its frequently asked questions.
- Choose the comparison set. Decide whether you are comparing confirmed planets, candidates, or planets in one system. Keep the categories separate unless you explicitly explain why they can be compared.
- Choose one archive table and solution convention. Use the same table and the same rule for selecting reported planet and stellar parameters throughout. Do not quietly mix values from unrelated published solutions.
- Record provenance. For each planet, save the archive row or identifier, the cited paper or solution, the values used, their uncertainties, and any missing fields. This makes the comparison repeatable and exposes differences that would otherwise look like precise disagreement.
Archive values can differ because published analyses may adopt different stellar parameters, which in turn affect derived planet values. Published Planetary Systems values can also differ from values in mission pipeline candidate tables. The archive FAQ explains these distinctions; a difference between entries is not necessarily an error, but it does mean the chosen solution must be documented.
Compare the inputs before using a score
A useful first-pass comparison starts with stellar flux relative to Earth and planet radius or mass. Add host-star temperature or type and orbital eccentricity when the selected catalog supplies them. NASA’s ESI explainer describes calculations that use stellar flux and either radius or mass; a published comparative method for transiting planets also considers transit and stellar properties, emitted-flux limits, eccentricity, albedo, and a penalty for large radii.
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| Axis | What to record | How to interpret it |
|---|---|---|
| Incident stellar flux | Flux relative to Earth, its uncertainty, and the selected habitable-zone boundaries | Shows how much stellar energy reaches the planet under the adopted solution; compare its position against a stated model, not a universal cutoff. |
| Planet size or mass | Radius or mass, uncertainty, and which measurement or solution is used | Provides context for whether a planet belongs in a rocky-planet comparison. A size or mass value alone does not establish composition or surface conditions. |
| Orbit | Eccentricity and uncertainty, if available | Indicates whether orbital distance varies substantially. Missing eccentricity is not evidence that the orbit is circular. |
| Host star | Temperature or type and the catalog solution used | Supplies context for interpreting the planet’s energy environment and highlights why consistent stellar parameters matter. |
| Uncertainty and provenance | Error bars, source citation, missing values, and selected solution | Shows how robust a comparison is. Do not replace missing or uncertain measurements with assumed precision. |
Keep the inputs alongside any summary score. For example, a planet can appear close to Earth on one physical measure while differing substantially in received energy, or have a poorly constrained value that makes its apparent ranking unstable. A transparent comparison lets readers see those trade-offs instead of hiding them behind one number.
Apply a habitable-zone screen, not a verdict
State which habitable-zone (HZ) model and boundaries you use, then describe a planet as inside or outside those boundaries under that model. The HZ is a simplified framework for identifying orbital regions where surface liquid-water oceans are not precluded under stated assumptions. It does not establish that surface water exists, or that a planet is suitable for life.
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Glaser and colleagues describe the HZ as a simplifying framework and distinguish its limits from the broader question of suitability for life. In particular, avoid calling it a “life zone.” If two planets fall near a boundary, show their flux uncertainties and avoid treating a model-dependent edge as an exact physical dividing line. See the 2026 discussion of euhabitability and the Habitable Zone framework.
Use ESI as a compact similarity measure
NASA describes the Earth Similarity Index as a physical similarity scale from 0 to 1. It is useful only as a compact way to summarize selected physical similarities; it is not a habitability probability or a measure of whether life exists. NASA notes that exoplanet measurements have uncertainties and rely on assumptions, that surface temperature is unknown, and that combining parameters does not determine habitability. Read the NASA ESI explainer and report the index with its inputs and their uncertainties, rather than presenting a rank as a conclusion.
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Methods can also depend on assumptions beyond the basic ESI inputs. Barnes, Meadows, and Evans’ 2015 comparative method considered multiple factors for transiting planets and reported a result for Kepler Objects of Interest under a circular-orbit assumption. That study-specific result is not a universal habitable-zone boundary or a general consensus cutoff; see the NASA Technical Reports Server record.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.What a catalog comparison cannot tell you
Catalog parameters do not directly characterize a planet’s atmosphere, surface pressure, water inventory, or biology. A first-pass screen can identify worlds worth investigating and clarify what is known about their orbits and sizes; it cannot establish the conditions at their surfaces. Assessing those conditions requires further observations and better constraints, especially on planetary atmospheres.
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For a reproducible result, publish the planet list, archive table and access date, selected solution and citations, comparison fields, uncertainties, missing values, HZ model, and any score formula. The archive states that its data are vetted and linked to original literature references; its FAQ describes use of archived published data for research with appropriate acknowledgements. Because tables and holdings can change, verify current entries in the archive when assembling a new comparison.
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