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Headshot of Emily Lakdawalla

Oppositions, conjunctions, seasons, and ring plane crossings of the giant planets

Posted By Emily Lakdawalla

07-07-2016 8:01 CDT

Topics: Neptune, explaining science, Saturn, Uranus, Jupiter

When are the solstices and equinoxes on the giant planets, and when are they best positioned for view from Earth? I ask these questions a lot as I write about Earth photos of giant planets, and I finally decided to gather the answers to those questions in a single post. I queried the JPL Horizons database for all the dates that I was looking for, figuring I'd save myself time looking up these dates for future posts. "Save myself time," ha! Famous last words. I spent all day playing with data tables and figuring out what they meant. In this post, I'll list orbital information for Neptune, Uranus, Saturn, and Jupiter. (If you're interested in Mars, here's an explainer on Mars' seasonal calendar; I'll cover Mars, Venus, and Mercury orbital events in a future post.)

One warning: the dates in this post, particularly ones many decades in the past or future, are approximate. Also, there are a variety of mathematical expressions and reference frames for the positions and orientations of the outer planets, and depending on which set you use, you could get answers that are different by a few days. The appearances of the outer planets don’t change very much within timescales of a few days anyway. 

Saturn from Pic du Midi Observatory, May 21, 2016

J.L. Dauvergne / E. Kraalkamp / F. Colas / S2P / IMCCE / OMP

Saturn from Pic du Midi Observatory, May 21, 2016
About a year before solstice and just a few days before opposition, Saturn presents its wide-open rings to Pic du Midi Observatory. Not only are the north polar hexagon and the Cassini division clearly visible, but so is the entire circumference of the narrower Encke gap, near the outer edge of the rings.

Some quick definitions: Opposition is when the Sun-Earth-planet angle is at a maximum, for planets beyond Earth; it's when the planet is opposite to the position of the Sun. The angle would be 180 degrees if all the planets' orbits were coplanar, but the orbits are all a little bit inclined with respect to each other. Opposition also happens near the date that Earth is closest to the planet within one synodic period (the time from one opposition to another). I usually think of opposition as being the best time to get photos of a planet because of the minimum distance, but although that may be true for Mars, relative proximity doesn't help you much with the giant planets. They are so far away that the relative closeness doesn't dramatically affect how big they appear. What opposition does for giant planet observers is to improve the opportunity that observers have to see them. When a planet is at opposition, it's up all night long, so you have a lot of dark sky time to observe it every night.

Conjunction is when the Sun-Earth-planet angle is at a minimum, that is, when the Sun and planet are very close to each other in the sky. Again, if the orbits were coplanar, the angle would be zero, but sometimes an outer planet passes above or below the Sun as seen from the Earth, not directly behind it, so the angle doesn’t go to zero. For one or two months around conjunction, it's impossible to observe an outer planet from Earth through conventional telescopes, and communications with spacecraft located at the planet are made difficult or impossible by the Sun's radio noise. Planetary missions plan for this by curtailing their transmission requirements during these periods.

A handy way to remember these first two terms is to remember that Earth is at the center. Opposition is when things are on opposite sides of the Earth; Conjunction is when they’re together. This may seem pre-Copernican, but that’s the point of origin of us stargazers, and therefore the origin of the terms.

Another event of interest for these planets is ring-plane crossings (usually abbreviated as "RPXs" or “RPCs”). For all these planets, the inner moons and rings orbit in (or very close to) a plane that's coincident with the planet's equator. Planetary equinoxes are defined by the Sun crossing the ring plane, just as the Sun crosses through our equator for Earth’s. Since Earth is located close to the Sun, we are usually on the same side of a planet's ring plane as the Sun is, so we see the rings illuminated most of the time. But because the orbits of the other planets and Earth have slightly different inclinations, Earth doesn't cross the ring plane on the same day that the Sun does, at equinox. For the period of time that Earth and the Sun are on different sides of the rings, Earth observers are treated to a very thin view of the shadowed side of the rings. In some years, the combination of Earth and planet's motions in their orbits means that Earth crosses the ring plane a total of three times around each equinox.

The synodic period of two orbiting bodies – in our case, the Earth and an outer planet – can be defined as the time between oppositions (or conjunctions). In other words, the time required for the two bodies to “line up” and return to the same relative orientation. Since the outer planets move much more slowly around the Sun than the Earth, the synodic period between the Earth and each outer planet is slightly more than one Earth year (and is of course different for each outer planet, as they move at different speeds). The Earth makes an orbit around the Sun in one year, but must then “catch up” to the planet as it has traveled in its own orbit.

I'll start with the slowest-moving planet and move inward.

Neptune as seen by the Hubble Space Telescope

NASA, ESA, E Karkoschka, and H. Hammel

Neptune as seen by the Hubble Space Telescope
Neptune in natural color, with Proteus (top), Larissa (lower right), Despina (middle left) and Galatea (far left). The brightness of the moons has been enhanced to make them more visible. The data for this image was taken on April 29 and 30, 2005, just after the planet's southern summer solstice on MArch 6.


Neptune's years are 164 Earth years long, so its seasons last more than 40 years. Its last equinox was in on July 11, 1963. Southern summer solstice, with the Sun at its lowest latitude of 29.16 degrees south, was March 6, 2005 (photo above). The southern autumnal equinox doesn't arrive until April 4, 2046. Equinoxes are a good time to explore planets and their moons, because they're a period of rapid change in atmospheres and ring systems and you get to observe both poles of planets and moons. I hope we can get a mission to Neptune around the time of its equinox, or not long after.

Because Neptune is so very slow-moving, the dates of its oppositions and conjunctions only change by about two days, year over year. In the 1980s, oppositions were in June. From 1989 through 2001, they were in July. Since 2015, oppositions have been in September. In 2033 opposition will shift to October.

Keck's Changing View of Uranus (2007)

Imke de Pater, Seran Gibbard, Heidi Hammel / W. M. Keck Observatory

Keck's Changing View of Uranus (2007)
From 2001 to 2007, Uranus's motion around the Sun has brought spring to its northern hemisphere. These images taken through Keck II's K prime filter. The images also show how the Adaptive Optics system has improved over time. In the final image, the planet seems brighter because Earth (and Keck) are on the dark side of Uranus' rings; when the image was brightened to make the rings more easily visible, the planet was also brightened.


Uranus travels around the Sun about twice as fast as Neptune, with years lasting 84 Earth years, and seasons lasting more than 20 Earth years. Its northern vernal equinox was on December 7, 2007. There were ring plane crossings on May 2, 2007; August 16, 2007; and February 20, 2008. Its northern summer solstice will be on April 11, 2030. The next equinox will be in February 2050. Hey, wouldn't it be awesome if we built identical spacecraft to explore Uranus and Neptune in the 2040s while both planets are close to their stormy equinoxes and showing us both poles of all their moons?

One can dream.

Uranus' oppositions move four days later every year. Right now, they happen in October. It'll be November for most of the 2020s, and December through 2034. If you think about it, it makes sense that Uranus' and Neptune's oppositions and conjunctions are fairly close in time to each other -- Uranus and Neptune had to be lined up (hence, both near opposition at the same time) for the Voyager 2 flybys in the 1980s, and Uranus has been overtaking Neptune on its marginally faster inside track around the Sun ever since.

Hubble views Saturn ring plane crossing, 1995

Reta Beebe (New Mexico State University), D. Gilmore, L. Bergeron (STScI), NASA/ESA, Amanda S. Bosh (Lowell Observatory), Andrew S. Rivkin (Univ. of Arizona/LPL), the HST High Speed Photometer Instrument Team (R.C. Bless, PI), and NASA/ESA

Hubble views Saturn ring plane crossing, 1995
The Hubble Space Telescope captured Saturn on May 22, 1995 as the planet's magnificent ring system turned edge-on. This ring-plane crossing occurs approximately every 15 years when the Earth passes through Saturn's ring plane.


Saturn's years are 29.5 Earth years long, its seasons averaging 7.4 Earth years. The Pioneer and Voyager flybys, in 1979 to 1981, happened around the northern vernal equinox; the Cassini mission arrived just after the northern winter solstice in 2004. Here is a table of seasons for Saturn, beginning with the northern vernal equinox that happened before the launches of the Pioneers.


Ls=0 (spring equinox)

Ls=90 (summer solstice)

Ls=180 (autumn equinox)

Ls=270 (winter solstice)


22 Sep 1950

3 Jul 1958

16 Jun 1966

21 May 1973
Pioneer 11 flyby


3 Mar 1980
Voyager flybys

9 Dec 1987

19 Nov 1995

25 Oct 2002
Cassini arrived 2004


11 Aug 2009

23 May 2017

Cassini ends 2017

6 May 2025

10 Apr 2032


23 Jan 2039

31 Oct 2046

10 Oct 2054

13 Sep 2061


29 Jun 2068

12 Apr 2076

27 Mar 2084

1 Mar 2091

Here's a graphical explainer of Saturn's seasons:

Saturn's seasons

Ralph Lorenz

Saturn's seasons
This diagram shows the main events of Saturn's year, and where in the Saturnian year the Voyager 1 and Cassini missions occurred.

Note that Saturn's perihelion occurs just after northern winter solstice, so, just like Mars, Saturn and its moons have shorter, warmer northern winters and longer, cooler northern summers, while the seasons in the south are more extreme.

Because Saturn's rings are so showy, ring-plane-crossing seasons are especially rewarding. The rings appear to "vanish" for the weeks that Earth is on the shadowed side of the rings. Here are all the equinoxes and related ring plane crossings from 1950 to 2090:

Earth RPX just before equinox

Saturn Equinox (Sun RPX)

Earth RPX just after equinox

Closest opposition to equinox

15 Sep 1950

22 Sep 1950


20 Mar 1951

2 Apr 1966

16 Jun 1966

28 Oct 1966
18 Dec 1966

20 Sep 1966

27 Oct 1979

3 Mar 1980

12 Mar 1980
23 Jul 1980

14 Mar 1980

22 May 1995
10 Aug 1995

19 Nov 1995

12 Feb 1996

15 Sep 1995


11 Aug 2009

4 Sep 2009

9 Mar 2009

23 Mar 2025

6 May 2025


21 Sep 2025

15 Oct 2038

23 Jan 2039

1 Apr 2039
9 Jul 2039

17 Mar 2039

6 May 2054
31 Aug 2054

10 Oct 2054

1 Feb 2055

16 Sep 2054


29 Jun 2068

25 Aug 2068

10 Mar 2068

14 Mar 2084

27 Mar 2084


23 Sep 2084

Saturn oppositions happen two weeks later every year. Saturn is at opposition today, June 3, 2016. Saturn was at opposition in January in 1975 and again in January in 2004 and will be again in January in 2034.

A rare triple moon shadow event on Jupiter

NASA, ESA, and the Hubble Heritage Team (STScI/AURA)

A rare triple moon shadow event on Jupiter
The Hubble Space Telescope caught Europa, Callisto, and Io transiting Jupiter and casting three shadows simultaneously on January 24, 2015. These events can be witnessed only once or twice per decade, near Jupiter's equinoxes. Because of the resonance of the orbits of Io, Europa, and Ganymede, it is not presently possible for all four moons to cast shadows on Jupiter at the same time.


With its low orbital inclination (about 3 degrees), seasons on Jupiter are somewhat irrelevant to Jupiter's weather and to the visible illumination of the poles of the planet and satellites. But seasonal variations at Jupiter do have one notable effect: whenever Earth is close to Jupiter's ring plane (near Jupiter's equinoxes), observers can witness mutual events, where the moons cross each other and the face of Jupiter. Jupiter's 12-year orbit means that these mutual event seasons happen once every six years. And also like at Saturn, there are some equinoxes where there are three, rather than one, ring plane crossings. Those are especially good years for mutual event observations, because Earth spends so much time very close to the ring plane. In addition to being fun to observe, mutual event observations help astronomers measure satellite orbital motions to very high precision. Another event associated with equinoxes is triple shadow transits, like the one above; they can only happen when Jupiter is close enough to equinox that wide-orbiting Callisto's shadow falls on the planet.

Jupiter oppositions are about 13 months apart. Jupiter observers talk about Jupiter "apparitions," a period of time around each opposition when Jupiter isn't lost in the Sun's glare. Here are all the oppositions since 1990 (when Hubble launched) and until 2040, with notes on which apparitions also have a ring plane crossing, and, therefore, opportunities to observe mutual events and triple shadow transits.

I hope this information is useful to people as it will be for me!

Acknowledgement: I'm very grateful to David Seal for his review and corrections on this post.

See other posts from July 2016


Read more blog entries about: Neptune, explaining science, Saturn, Uranus, Jupiter


salvi: 07/07/2016 03:14 CDT

Very nice compilation Emily. Especially in view of explaining the terminology for a layman.

morganism: 07/07/2016 04:20 CDT

Have a great break, but i found a non-space paper for you to peruse, on RGB image conversion to 3D

Rob : 07/09/2016 09:58 CDT

A wonderful article as always. However, I think you meant that Jupiter's obliquity is 3 degrees, not its orbital inclination.

John Sheff: 07/12/2016 04:51 CDT

Thanks for compiling all this information, Emily! It'll be immensely helpful to me not only as a planetary exploration buff but as an amateur astronomer and educator.

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