Al Bustan 


IC5146 - Cocoon
M5 - NGC5904
M8 - Lagoon Nebula
M16 - Eagle Nebula
M20 - Trifid
M27 - Dumbbell
M31 - Andromeda
M33 - Pinwheel
M42 - Orion
M45 - The Pleiades
M51 - Whirlpool
M57 - Ring
M63 - Sunflower
M64 - Black-Eye
M65 - NGC3623
M67 - NGC2682
M98 - NGC4192
M99 - Pinwheel
M100 - NGC4321
M101 - NGC5457
M104 - Sombrero
M105 - NGC3379
M106 - NGC4258
C/2004 Q2 - Machholz
NGC 891
NGC2024 - Flame
NGC2244 - Rosette
NGC6960 - Veil
The Mice - NGC4676






Jupiter is the largest planet of our solar system, at a distance of 5 A.U. from the Sun and revolves around it once every 12 years. It alone contains two-thirds of the mass in the Solar System outside of the Sun, 318 as much as the Earth. It is 11 times greater in diameter than the Earth and Its density is estimated to be 1.3 g/cm3.

Jupiter has many moons. Observations with a small telescope show four of its moons (Io, Europa, Ganymede and Calisto, discovered by Galileo in 1610) and reveal bands of clouds across its surface. Ganymede, at 5,276 km in diameter, is the largest satellite in the solar system and is larger than the planet Mercury. Some of Jupiter's moons revolve in the direction opposite from that of Jupiter's rotation (that is, retrograde), while other moons revolve prograde.


Jupiter and Io (photo by Cassini probe)

Jupiter chemical composition is almost entirely hydrogen and helium and, therefore, is closer to that of the Sun and stars than it is to that of the Earth. In Jupiter's outer parts, most of the hydrogen is in the form of hydrogen molecules (H2).Jupiter isn't solid, it has no crystal surface at all. At deeper and deeper levels, its gas gets denser and denser, eventually liquefying.

The most prominent feature of the visible cloud surface of Jupiter is a large reddish oval known as the Great Red Spot (GRS). It is about 13,000 km x 26,000 km, larger than the Earth, and drifts about slowly with respect to the clouds as the planet rotates. The GRS is a relatively stable feature, for it has been visible for over 350 years. It is an anticyclonic storm, because its center has high pressure,  with counterclockwise winds.

Jupiter rotates very quickly, once every 10 hours. Its rapid spin is a major reason for the colorful bands, which are clouds spread out parallel to the equator. They are in constant turmoil; the shapes and distribution of bands change in a mater of days. Due to Jupiter's rapid rotation, the effect that we call the Coriolis force is particularly strong. Computer models show that under such conditions, large vortices like the GRS are produced. When many unequal spots are produced, the stronger ones absorb the weaker ones until only a single vortice is left. Such vortices last a long time.

Jupiter has bright bands called "zones" and dark bands called "belts". The zones are rising gas, while the belts are falling gas. The colors we see in the belts may have to do with sulfur compounds in the middle clouds, or perhaps with organic molecules.

In what many observers called the most exciting week ever in astronomy, pieces of periodic Comet Shoemaker-Levy 9, D/1993 F2, crashed into Jupiter in July 1994.



Observer's Log

RA: 08h 49m 01.7s Dec: +18°39'33"
Heliocentric ecliptical coordinates: l: 140°25'20.4" b: +00°50'09.9" r: 5,341642
Geometric geocentric ecliptical coordinates: l: +129°35'21" b: +00°50'11" r: 5,340573
Mean geometric ecliptical coordinates: l: +129°35'13" b: +00°50'10" r: 5,340607
True equatorial coordinates: RA: 08h 49m 02s Dec: +18°39'34"
Physical Data: DE: 0,22°, DS: -0,17°, Position angle: 17,47°.
Longitude of central meridian:  System I: 82,92°, System II: 108,06°
Correction for phase: -0,51
Apparent equatorial diameter: 36,9
Apparent polar diameter: 34,5








Number of Frames: stack of 86 best frames out of 451

Exposure:  15 fps AVI

Equipment: LX200-12", F/20, Toucam Pro

Date: 03-03-28

Processed with K3CCDTools and Photoshop.











Number of Frames: stack of 133 best frames out of 669

Exposure:  5 fps AVI

Equipment: LX200-12", F/40, Toucam Pro

Date: 03-03-22

Processed with K3CCDTools and Photoshop.


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This site was last updated 2006-04-19                                                                                                          Site created and maintained by Jorge Lázaro