Published in the November 1999 issue of Universe
The comet may have gone, but Jupiter remains an object of interest to observe. It can be observed from the backyard, or even at a dark sky site. Indeed, my best view of Jupiter thus far came from Wiruna, the Society's dark sky site at Ilford, in the early hours of January 20, 1991 during a period of what must have been exceptional seeing. Some members may recall the view. The following is from my article "Return To Ilford", which appeared in the February/March 1991 issue of Universe.
"It was now well after midnight, and this bright "star" in the eastern sky had been catching our attention since late evening. Jupiter was very prominent tonight, being only a week away from opposition. A check of the Galilean satellite tables revealed that Io would be eclipsed tonight. We were also wondering whether Jupiter itself would occupy our attention until the eclipse. As we looked at Jupiter just before the eclipse, our minds were literally blown away.The memories of Jupiter in January 1991 are still strong.
"I, let alone anyone else present at Ilford that night, had never seen so much detail on Jupiter. Looking closely at the two main belts, we could see that they were ragged.
"The belts, however, paled into insignificance when compared with the equatorial zone that lies between the two equatorial belts. David [Collis-Bird] described the equatorial zone as having been coloured by a child. Looking through the 20, 17 and 14 inch telescopes, there were streaks everywhere in this zone. Even through my 6 inch, the zone didn't look smooth.
"The appearance of Jupiter had an effect on everyone. It is rumoured that Steve [Mencinsky], who normally doesn't focus on anything within 10,000 light years, may indeed become a closet planetary observer... The view also brought Joe Cauchi and David away from their photography to join the observers. Tony [Buckley] was still talking about Jupiter the following morning."
Jupiter reached opposition on 24th October this year, and around this time, it is visible all night, although views are best made when the planet is higher up in the sky. Table 1 gives the dates of opposition of Jupiter from 1986 - 2012. On the left side of the table, one can see that Jupiter's brightness varies by as much as 0.5 magnitudes between different oppositions. This is because Jupiter, like Earth, passes through perihelion as well as aphelion during the course of its elliptical orbit around the Sun. Consequently, there are apparitions when Jupiter is closer to Earth than in other years. This year, Jupiter is at its closest to Earth since 1987, as shown on the right side of the table.
Looking at Jupiter through a telescope, three things will firstly come to mind:
Jupiter's cloud bands contrast quite well with each other, making them
easy to distinguish. The two most obvious belt features are the North Equatorial
Belt and the South Equatorial Belt, which are separated from each other
by the Equatorial Zone.
The Equatorial Zone is seldom situated evenly around Jupiter's equator,
and its width has been known to vary by nearly 10 degrees in latitude.
The region is known for rapid changes in the appearance of its details,
such that the appearance of features can change in a period as short as
a week. Whilst its colour is typically whitish, during the past century
it has had displayed tints of orange, dusky blue-green, blue-white, and
yellow-brown. It has been suggested that the reddish colouring of the Equatorial
Zone reappeared every 12 years (Jupiter's orbital period) whilst the darkness
of the North and South Equatorial Belts increased at perihelion and decreased
The North Equatorial Belt has been described as one of the most consistently
active regions on Jupiter. It is darker and narrower than the South Equatorial
Belt, and it has sometimes been seen to be divided into two or three non-continuous
components. Since the mid 1980s, an area of study has been intense blue
features found along the southern edge of the North Equatorial Belt, extending
even well into the southern part of the Equatorial Zone. Their existence
has been known since 1928, and they were photographed by the Voyager spacecraft.
Nevertheless, their nature has been largely ignored. There are now at least
a dozen such blue features along the Belt. Large aperture telescopes will
make the colour more obvious.
In contrast to the North Equatorial Belt, the South Equatorial Belt,
which usually consists of two well-defined components widely separated
by the non-continuous South Equatorial Belt Zone, is quite erratic in its
appearance, being very quiet for long periods (sometimes being invisible)
and then subject to sudden outbursts of activity that follow the fading
of the southern component. This activity is known as the South Equatorial
Belt Disturbance and has been described as "one of the most dramatic and
beautiful of all solar system phenomena" with a cyclical nature of around
3 years. In the presence of a clear South Equatorial Belt Zone and weak
South Equatorial Belt (southern component), it begins with a brilliant
white spot forming in the South Equatorial Belt Zone, and has sometimes
been so large that it can be seen projecting from the limb. Within a few
days, a small dark blob is "ejected" by the bright disturbance and is torn
apart by the South Equatorial Belt Zone's winds. The result is a long dark
filament. As material continues to erupt, small knots appear in both components
of the South Equatorial Belt, and as other spots erupt from the same longitude
position at which the first spot surfaced, the entire South Equatorial
Belt region is filled within a few weeks with a series of white ovals and
numerous dark knots.
The North Temperate Belt is often more bluish than any of the other
belts on Jupiter, and is frequently divided into two narrow components.
When the North Temperate Belt has appeared as a single broad band, it is
sometimes followed by eruptions of dark spots. These features are very
rare, however, having only been seen in 1880, 1891, 1929, 1939, and 1964.
These spots usually last for only a few months, and it is worthwhile keeping
an eye on the area for any further outbreaks.
There have been several times when the South Temperate Belt has been darker than either the North or South Equatorial Belts, and in general it is a noticeable area of Jupiter. Outbreaks of white ovals lasting for long periods, dark spots, and general chaos are common in this region.
So far, we've just discussed various areas that circle the planet. However,
there are a number of individual features, some of which are transient
in nature, that are well worth observing.
The most famous feature on Jupiter is the Great Red Spot, a huge high-pressure system in the South Tropical Zone near the South Equatorial Belt that is believed to have first been seen by Robert Hooke in 1665 and Giovanni Cassini in 1666. In 1878, it became the most conspicuous marking on Jupiter and has been a key feature of Jupiter itself. Its cloudtops, while being reddish in general, have been described over time as being brick red, carrot orange, salmon pink, pale yellowish-grey, and even green-tinged white! Likewise, its dimensions have been known to vary.
Remember of course that the Great Red Spot will not necessarily be visible when you first turn your telescope to Jupiter. As the planet rotates, there is a 50% chance that the Great Red Spot may be on the other side of the planet when you look. However, if you record the time that you observe the Great Red Spot, it is easy to calculate the approximate time of near-future observing sessions when you will sight the Great Red Spot as a multiple of Jupiter's 10hr rotation period (likewise, if you don't observe the Great Red Spot, you'll know when it won't be visible).
For the observer with a telescope 20cm and more in aperture, here's
an interesting observational challenge: Interactions of the Great Red Spot
with features on the southern edge of the South Equatorial Belt, in the
South Tropical Zone, and on the northern edge of the South Temperate Belt,
often result in noticeable accelerations and decelerations of the features
when they encounter the Great Red Spot. Can you spot the changes?
Up until last year, one could write that three white ovals, called "BC", "DE", and "FA", are currently visible in the South Temperate Belt. Believed to be of a similar nature to the Great Red Spot (a high-pressure anti-cyclone), they were first observed in 1939 and 1940 in the South Temperate Zone, when they extended over 90 degrees in longitude. Their appearance quickened the rotation period of the South Temperate Current by 13 seconds from its normal period of 9 hours 55 minutes 20 seconds. Since their appearance, they have contracted in size, and brightened.
Last year, the ovals BC and DE suddenly merged, forming a larger oval BE, and now BE is closing in on the last remaining long-lived white oval, FA. The merger of BC and DE occurred during solar conjunction, so hopefully the merger of BE and FA will be more favourable. Depending on how long it takes for the merger to occur, the mission scientists behind the Galileo spacecraft, currently orbiting Jupiter, are interested to learn when the merger may occur so that Galileo can take images.
Although the White Oval mergers have been of considerable interest recently, there is a lot that has been observed on Jupiter. Here's a snapshot of some of the observed phenomena reported to the Association of Lunar and Planetary Observers (some of the features are only visible in CCD images)
The Great Red Spot was observed during winter to be small and pale. However, recent CCD images by American amateur Donald Parker do show a deepening red condensation that may be developing in the Great Red Spot. This could indicate a forthcoming revival - what will Spring and Summer reveal?
The South Temperate Belt is currently home to three of the dark spots which were seen during last year's apparition. Dark Spot # 6 is of particular interest to professional astronomers.
The South Equatorial Belt is seeing a lot of turbulence following the Great Red Spot. Beyond that, the Belt is relatively uniform in intensity. Through most Jovian longitudes, there is a thin rift that divides the South Equatorial Belt into north and south components - however, the south component is about three times thicker than the north component.
The Equatorial Zone is quite active and is being described as being "veiled" or "dusky grey". South of the Equatorial Band, which is reported to be relative easy to see at some longitudes, the Equatorial Zone is darker and sparse in features. To the north, however, there are many festoons and loop festoons coming off the south edge of the North Equatorial Belt and extending to the Equatorial Band. These latter loop festoons appear as dark borders that enclose white ovals.
As suggested above, The North Equatorial Belt is active, and currently is home to a series of large Bays, some of which have become large enough to be mistaken for the Red Spot Hollow.
The North Temperate Belt is also active, and at most longitudes it is nearly as dark as the Equatorial belts.
Jupiter is home to 16 satellites. Were it not for the glare of Jupiter, the four Galilean satellites (so-called after the discoverer Galileo) would be easily visible to the naked eye. As it is, eagle-eyed observers have been known to sight the occasional outer satellite when Jupiter is at opposition.
Io, Europa, Ganymede, and Callisto are all visible with a small pair of binoculars, and a small telescope will provide a fine view of Jupiter and its four major moons, with their configuration changing noticeably over the space of an hour.
Careful study of the satellites at opposition will reveal that they are tiny discs rather than mere points of light. Owners of telescopes of aperture 25cm and upwards viewing under circumstances allowing for magnification of 400x plus, will reveal surface details under superb seeing. The best times to look are when the satellite is transiting Jupiter, since there is a reduced glare when seen against a light background. Indeed, Ganymede's polar frosts can reportedly be detected with a telescope of only 15cm aperture because they closely match the albedo of Jupiter's zones, giving Ganymede an elliptical rather than circular appearance. If atmospheric transparency is near the best end of the scale, you can even try to detect the colours of Jupiter's satellites. Io is yellow, Europa is off-white (making it a difficult satellite to see during transits), Ganymede is tawny grey, and Callisto is a dusky blue-grey.
Those of you who own a yearbook or read such magazines as Astronomy and Sky & Telescope will see the monthly tables that show the movements of the Galilean satellites around Jupiter. Thus, you can easily determine which moon is which. Looking at the diagrams, you'll notice that the orbital paths regularly cross Jupiter, and here is where some of the excitement surrounding the satellites comes into play. Because the plane of the Galilean satellite orbits lies almost in the same plane as Earth's orbit, we see each satellite (except Callisto on occasions) pass directly in front of Jupiter and the behind it on each orbit. The shadows cast by the satellites onto the face of Jupiter as they transit the disk can be seen as small black dots in any telescope. The satellites themselves appear as bright dots against Jupiter's dark belts.
However, when they are in front of the brighter zonal areas, they become harder to distinguish unless you know exactly where to look. It is often best to follow a satellite as it starts to cross the planet's face. Prior to the date of opposition, the shadow precedes the transiting satellite, i.e. it falls on the disc before the transit begins. After opposition, the shadows fall on Jupiter after the transit, and remain on the planet even when the satellite itself has finished its transit. On the other side of the orbit, the satellite is eclipsed by Jupiter. In the months leading up to opposition, a satellite approaching occultation can be seen to gradually fade away as it enters Jupiter's shadow. At opposition, the shadow is directly behind Jupiter as seen by us. After opposition, the shadow is now on the other side of Jupiter, and a satellite will reappear from eclipse at some distance from the limb of the planet.
All of these events (satellite transits, shadow transits, satellite eclipses and satellite occultations) are listed in some yearbooks and magazines, so it's worth checking these tables to prepare for the night's viewing.
Beyond The Galilean Moons
What about trying for the satellite Himalia? This faint moon of Jupiter (magnitude 14.6) is much further out from Jupiter than the Big Four. At best, it can be just over one degree in angular separation from Jupiter. To find Himalia, you will need to obtain the offset coordinates (available from the Astronomical Almanac) or perhaps some advanced software will have the details. Although the satellite was discovered photographically in 1904 with a 36 inch reflector, and while CCD images are your best bet for detecting the satellite, can you see it visually? Don't expect much movement, though, as the satellite takes 8 months to orbit Jupiter.
Observing Jupiter is so easy, and can be done at home with the simplest of telescopes. The satellite phenomena provide for exciting events as you see the Solar System "in action" - indeed, you're observing "a miniature Solar System". You'll be surprised how rewarding and fascinating it is.