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  2. Orbit of Mars - Wikipedia

    en.wikipedia.org/wiki/Orbit_of_Mars

    Extra-close oppositions of Mars happen every 15 to 17 years, when we pass between Mars and the Sun around the time of its perihelion (closest point to the Sun in orbit). The minimum distance between Earth and Mars has been declining over the years, and in 2003 the minimum distance was 55.76 million km, nearer than any such encounter in almost ...

  3. Mars - Wikipedia

    en.wikipedia.org/wiki/Mars

    Mars's average distance from the Sun is roughly 230 million km (143 million mi), and its orbital period is 687 (Earth) days. The solar day (or sol) on Mars is only slightly longer than an Earth day: 24 hours, 39 minutes, and 35.244 seconds. [185] A Martian year is equal to 1.8809 Earth years, or 1 year, 320 days, and 18.2 hours. [2]

  4. Astronomical unit - Wikipedia

    en.wikipedia.org/wiki/Astronomical_unit

    Average distance from the Sun — Venus: 0.72 — Average distance from the Sun — Earth: 1.00 — Average distance of Earth's orbit from the Sun (sunlight travels for 8 minutes and 19 seconds before reaching Earth) — Mars: 1.52 — Average distance from the Sun — Jupiter: 5.2 — Average distance from the Sun — Light-hour: 7.2 ...

  5. Canonical units - Wikipedia

    en.wikipedia.org/wiki/Canonical_units

    In astrodynamics, canonical units are defined in terms of some important object’s orbit that serves as a reference. In this system, a reference mass, for example the Sun’s, is designated as 1 “canonical mass unit” and the mean distance from the orbiting object to the reference object is considered the “canonical distance unit”.

  6. Ecliptic coordinate system - Wikipedia

    en.wikipedia.org/wiki/Ecliptic_coordinate_system

    Ecliptic longitude or celestial longitude (symbols: heliocentric l, geocentric λ) measures the angular distance of an object along the ecliptic from the primary direction. Like right ascension in the equatorial coordinate system, the primary direction (0° ecliptic longitude) points from the Earth towards the Sun at the March equinox. Because ...

  7. Titius–Bode law - Wikipedia

    en.wikipedia.org/wiki/Titius–Bode_law

    The resulting values can be divided by 10 to convert them into astronomical units (AU), resulting in the expression: a = 0.4 + 0.3 × 2 n . {\displaystyle a=0.4+0.3\times 2^{n}~.} For the far outer planets, beyond Saturn , each planet is predicted to be roughly twice as far from the Sun as the previous object.

  8. Solar radius - Wikipedia

    en.wikipedia.org/wiki/Solar_radius

    Evolution of the solar luminosity, radius and effective temperature compared to the present-day Sun. After Ribas (2009) [3] The uncrewed SOHO spacecraft was used to measure the radius of the Sun by timing transits of Mercury across the surface during 2003 and 2006. The result was a measured radius of 696,342 ± 65 kilometres (432,687 ± 40 miles).

  9. Orders of magnitude (length) - Wikipedia

    en.wikipedia.org/wiki/Orders_of_magnitude_(length)

    1 astronomical unit (au); mean distance between Earth and Sun 10 12: 1 terameter (Tm) 1.3 Tm Optical diameter of Betelgeuse: 1.4 Tm Orbital distance of Saturn from Sun 2 Tm Estimated optical diameter of VY Canis Majoris, one of the largest-known stars: 5.9 Tm Orbital distance of Pluto from the Sun ~ 7.5 Tm Outer boundary of the Kuiper belt: 10 ...