Planetary Science
Mars
The Red Planet — cold, dusty, with the largest volcano and canyon in the solar system
Mars is the fourth planet from the Sun — half Earth's diameter, 11% of its mass, with a thin CO₂ atmosphere (~1% of Earth's pressure). Famous for the iron oxide ("rust") that gives its red color, the largest volcano in the solar system (Olympus Mons, 22 km tall), the largest canyon (Valles Marineris, 4000 km long), polar ice caps, and seasonal global dust storms. Currently host to multiple rovers and orbiters; future target for human exploration.
- Diameter6,779 km (53% Earth)
- Mass6.4 × 10²³ kg (10.7% Earth)
- Distance from Sun1.52 AU (227.9 million km, average)
- Year length687 Earth days
- Day length24h 37min (sol)
- Surface gravity3.71 m/s² (38% Earth's)
- Atmosphere95% CO₂; ~600 Pa surface pressure
- MoonsPhobos and Deimos (small, captured asteroids likely)
Interactive visualization
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Mars at a glance
| Property | Mars | Earth | Ratio |
|---|---|---|---|
| Diameter | 6,779 km | 12,742 km | 0.53 |
| Mass | 6.4 × 10²³ kg | 5.97 × 10²⁴ kg | 0.107 |
| Surface gravity | 3.71 m/s² | 9.81 m/s² | 0.38 |
| Atmospheric pressure | ~600 Pa | 101,325 Pa | 0.006 (0.6%) |
| Mean surface T | -65°C | 15°C | — |
| Day length | 24h 37min | 24h | 1.027 |
| Year length | 687 days | 365.25 days | 1.881 |
| Distance from Sun | 1.52 AU | 1.0 AU | 1.52 |
| Number of moons | 2 (Phobos, Deimos) | 1 (Moon) | — |
The thin atmosphere
| Component | Mars | Earth |
|---|---|---|
| CO₂ | 95% | 0.04% |
| N₂ | 2.6% | 78% |
| Argon | 1.9% | 0.93% |
| O₂ | 0.16% | 21% |
| Water vapor | 0.03% | 0-4% |
Pressure varies seasonally as polar CO₂ freezes/sublimates — cycle moves ~25% of atmosphere between solid and gaseous phases.
Major surface features
| Feature | Description |
|---|---|
| Olympus Mons | 22 km tall shield volcano; largest in solar system |
| Tharsis Bulge | Volcanic plateau; cluster of huge volcanoes |
| Valles Marineris | 4000 km canyon; 7 km deep |
| Hellas Basin | 2300 km diameter impact crater; 7 km deep |
| Polar ice caps | Water ice + frozen CO₂; seasonal variations |
| Northern lowlands | Smoother terrain; possibly ancient ocean basin |
| Southern highlands | Heavily cratered; older terrain |
Exploration timeline
| Mission | Year | Achievement |
|---|---|---|
| Mariner 4 | 1965 | First flyby; 21 photos |
| Viking 1, 2 | 1976 | First landers; soil tests |
| Pathfinder/Sojourner | 1997 | First successful rover |
| Spirit, Opportunity | 2004 | Long-duration rovers |
| Curiosity | 2012 | Nuclear-powered, still operating |
| InSight | 2018 | Marsquake measurements |
| Perseverance + Ingenuity | 2021 | Sample collection, helicopter flight |
| Tianwen-1 (China) | 2021 | Orbiter + lander + rover |
JavaScript — Mars calculations
// Mars constants
const M_MARS = 6.4171e23;
const R_MARS = 3389.5e3;
const G = 6.674e-11;
// Surface gravity
const g_mars = G * M_MARS / (R_MARS * R_MARS);
console.log(`Mars g: ${g_mars.toFixed(3)} m/s²`); // 3.71
// Weight on Mars vs Earth
function weightOnMars(earth_weight_N) {
return earth_weight_N * 0.378;
}
console.log(`Person 700N on Earth weighs ${weightOnMars(700).toFixed(0)}N on Mars`);
// Escape velocity
const v_escape = Math.sqrt(2 * G * M_MARS / R_MARS);
console.log(`Mars escape: ${(v_escape/1000).toFixed(2)} km/s`); // 5.03
// Solar flux at Mars vs Earth
const solar_flux_earth = 1361; // W/m²
const solar_flux_mars = solar_flux_earth / (1.524 * 1.524);
console.log(`Solar flux at Mars: ${solar_flux_mars.toFixed(0)} W/m²`); // ~586
// Year length from Kepler's 3rd
const T_earth = 365.25;
const T_mars = T_earth * Math.pow(1.524, 1.5);
console.log(`Mars year: ${T_mars.toFixed(0)} days`); // 687
// Distance traveled by orbiting Mars
const orbit_radius = 1.524 * 1.496e11;
const mars_orbit_speed = Math.sqrt(G * 1.989e30 / orbit_radius);
console.log(`Mars orbital speed: ${(mars_orbit_speed/1000).toFixed(2)} km/s`); // 24.1
Why Mars matters
- Astrobiology. Best candidate for past or current extraterrestrial life in solar system.
- Human exploration. Target for first crewed interplanetary mission (NASA Artemis-Mars, SpaceX).
- Comparative planetology. Why did Mars lose its atmosphere while Earth kept hers?
- Solar system formation. Mars provides a well-preserved record of early solar system.
- Resource utilization. Water ice, CO₂, regolith — basis for in-situ resource utilization (ISRU).
- Atmospheric science. Dust storms, CO₂ cycle inform Earth's climate science.
- Geology. Olympus Mons, Valles Marineris — unique geological structures on Mars.
Common misconceptions
- Mars looks "Earth-like in pictures." Misleading — atmosphere too thin, T too cold, radiation too high. Looks like cold desert in images, but is much more inhospitable.
- Dust storms are dangerous to rovers. Reduce solar power and visibility but rarely catastrophic. Wind force is low (thin atmosphere). Movie "The Martian" exaggerated this.
- Mars has water you can drink. Water exists as ice or trace vapor; no liquid surface water (boils at low pressure). Future colonists would extract from ice.
- Mars's red color is bright. Actually muted — like a desert plus dust haze. From space, Mars appears reddish-orange, not the saturated red sometimes shown.
- Phobos and Deimos are like Earth's Moon. They're tiny irregularly-shaped captured asteroids; not at all like our spherical Moon.
- Distance is constant. Mars's distance from Earth varies from ~55 million km (close approach) to ~400 million km (far side of Sun). Mission timing matters greatly.
Frequently asked questions
Why is Mars red?
Iron oxide (rust, Fe₂O₃) on the surface. Mars's surface contains 14-17% iron oxide minerals, much higher than Earth. Visible from space — gives Mars its characteristic ochre-red color. Wind redistributes fine dust globally; entire planet is reddish. Was probably grayer before; oxidation over billions of years gave it color.
Could humans live on Mars?
Not without major infrastructure. Atmosphere is 1% Earth's pressure (would need pressurized habitats), 95% CO₂ (no oxygen), surface T -65°C average (-140°C polar to +20°C equatorial daytime). Lethal radiation levels (no magnetic field shielding, thin atmosphere). Water ice exists at poles and subsurface — minable. SpaceX, NASA both targeting human Mars missions in 2030s-40s.
What's the largest volcano?
Olympus Mons — 22 km tall (2.5× Everest), 600 km wide. Largest volcano in the solar system. Shield volcano, like Hawaii's Mauna Kea but vastly bigger because Mars lacks plate tectonics — magma keeps erupting from same hotspot, building up massively over billions of years.
What's Valles Marineris?
The largest canyon in the solar system. 4000 km long, up to 200 km wide, 7 km deep. Stretches ~20% of Mars's circumference. Probably formed by tectonic stress related to Tharsis bulge (the Olympus Mons region). Compare: Grand Canyon is 446 km long, 1.6 km deep — Mars's canyon is ~10× longer, 4× deeper.
Was there ever water?
Yes, abundantly. Ancient Mars (3-4 billion years ago) had liquid water — rivers, lakes, possibly oceans. Evidence — riverbeds, lake floors, hydrated minerals (clays, sulfates). Today: water exists as ice (polar caps, subsurface) and small amounts in atmosphere. Ancient liquid water existed when Mars had thicker atmosphere, before losing it to space.
What about life?
Unknown. No definitive evidence yet. Past Mars (with water, milder climate) might have hosted microbes. Present Mars: harsh — UV, radiation, dryness. Possibility: subsurface life in liquid water aquifers. Mars Sample Return (planned) will bring back samples for detailed Earth-lab analysis. Methane fluctuations detected — could be biological or geological.
How are the moons different?
Phobos (22 km) and Deimos (12 km) — irregularly shaped, very small. Likely captured asteroids from main belt. Phobos orbits VERY close (9,377 km from Mars surface) and is spiraling inward — will crash or break apart in ~50 million years. Deimos is more distant and stable. Future Mars mission may use Phobos as base.