A planet is at opposition when the Sun and the planet are located at opposite directions as viewed from the Earth. At that time, the planet is best suited for observation for these three reasons:
- It is almost at its closest point to the Earth (but it is not at the same distance from Earth at each opposition)
- It is highest in the sky when the night is darkest
- Its disk is fully illuminated by the Sun
Only planets beyond the Earth's orbit can be at opposition. Mars, Jupiter, Saturn, Uranus and Neptune can be at opposition. The orbits of Mercury and Venus lie inside the orbit of the Earth, and therefore they can never be at opposition.
The difference between the time of Mars at opposition and the time of Mars closest to Earth may differ by a week or more, because of the eccentricities of the orbits of Earth and Mars (i.e. that they are ellipses rather than circles).
When a planet is at opposition, it rises at sunset og sets at sunrise, just like the full Moon. At high latitudes, oppositions during the winter are usually better suited for observation than oppositions during the summer. This is because the planet is higher in the sky at oppositions during the winter. Moreover, the sky is not completely dark in the summer nights at high latitudes.
Mars is closest to the Earth at oppositions in August, which is during the summer of the northern hemisphere, but observed from higher northern latitudes, Mars is at those times low in the sky. Thus, and because the sky is not completely dark, from Norway it is more favourable to observe oppositions well after the beginning of September and in October, even if Mars is not quite as large and bright.
The following diagram is a representation of Mars at opposition in the years 2018–2033. Further down are diagrams for the years from 1892 until about 2300. The yellow central dot represents the Sun. The blue dots represent the Earth, and the red dots represent Mars. The black, horizontal line is directed toward the vernal point. The red line marks the perihelion of Mars (orbital point closest to the Sun), and the blue line marks the aphelion of the Earth (orbital point farthest from the Sun). The grey circle is the average distance from the Sun to Mars.
Distances (between centres of the celestial bodies) are to scale, but sizes of the Sun and the planets are not.
The year ranges of the diagrams overlap somewhat.
1800
1900
Year (and later): 1901 · 1911 · 1920 · 1928 · 1937 · 1946 · 1956 · 1965 · 1973 · 1982 · 1993
2000
Year (and later): 2001 · 2010 · 2018 · 2027 · 2037 · 2046 · 2054 · 2063 · 2072 · 2082 · 2091 · 2099
2100
Year (and later): 2108 · 2119 · 2127 · 2136 · 2144 · 2153 · 2163 · 2172 · 2180 · 2189 · 2198
2200
Year (and later): 2208 · 2217 · 2225 · 2234 · 2245 · 2253 · 2262 · 2270 · 2279 · 2289 · 2298
2300
Mars at opposition 1899–2315
Distances in kilometres are rounded to the nearest 1 000 km.
The new table below is calculated with a method of higher accuracy. A selection of the times has been checked against accurate numbers from Jean Meeus: Astronomical Tables of the Sun, Moon and Planets (2015); the greatest error is ±1 minute. The declinations in the selection are exactly the same as those in the book. There might be minor errors in the last two decimal places of the distances (astronomical units) or the last digits before 000 in the kilometre columns.
Note: The times are in Terrestrial Time. Terrestrial Time is a uniform timescale that can be used in calculations of astronomical phenomena. Universal Time (UT) and Greenwich Mean Time (GMT) depend on the rotation of the Earth and are not uniform. Terrestrial Time is only accurately obtained by observations, but one can, to a certain degree of accuracy, extrapolate (calculate values outside a range of known values) into the future.
The difference between Terrestrial Time and Universal Time is called ΔT. Conversion from Terrestrial Time to Universal Time is done by subtracting ΔT. Approximate values of ΔT, from Astronomical Tables of the Sun, Moon and Planets:
Year | ΔT |
---|---|
1900 | 0 minutes |
1990 | 1 minute |
2080 | 4 minutes |
2200 | 8 minutes |
2300 | 13 minutes |
Explanations
- AU = astronomical unit. The mean distance between the Sun and the Earh is 1 AU.
- Mag. = apparent magnitude, which in this context means brightness. The lesser the number, the brighter the light. Remember that −2 is less than −1, as in the thermometer scale.
Idea for the diagrams
- Ian Ridpath: Stars & Planets (2007), page 354
- Norsk Astronomisk Selskap: Astronomi (1/2020), page 30
Sources
- Jean Meeus: Astronomical Algorithms (1998)
- Jan-Erik Ovaldsen and Jan Teuber: Himmelkalenderen 2008, page 198
In other languages
- Mars i opposition (Danish)
- Mars i opposisjon (Norwegian)