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For example, Jupiter has a synodic period of 398.8 days from Earth; thus, Jupiter's opposition occurs once roughly every 13 months. If the orbital periods of the two bodies around the third are called T 1 and T 2, so that T 1 < T 2, their synodic period is given by: [7]
Size of Jupiter compared to Earth and Earth's Moon. Jupiter is about ten times larger than Earth (11.209 R 🜨) and smaller than the Sun (0.102 76 R ☉). Jupiter's mass is 318 times that of Earth; [2] 2.5 times that of all the other planets in the Solar System combined.
For example: q= 3×(length of Mars) + 2×(length of Jupiter). (The term 'length' in this context refers to the ecliptic longitude, that is the angle over which the planet has progressed in its orbit in unit time, so q is an angle over time too. The time needed for the length to increase over 360° is equal to the revolution period.)
These satellites were the first celestial objects that were confirmed to orbit an object other than the Sun or Earth. Galileo saw Io and Europa as a single point of light on 7 January 1610; they were seen as separate bodies the following night. [11] Callisto: Jupiter IV o: 8 January 1610 p: 13 March 1610 Io: Jupiter I Europa: Jupiter II 1650s
<p>Jupiter is the largest planet in our Solar System, and the competition really isn't even close. It's an absolutely massive planet and it helped define what a gas giant planet truly is. Because ...
Rotation period with respect to distant stars, the sidereal rotation period (compared to Earth's mean Solar days) Synodic rotation period (mean Solar day) Apparent rotational period viewed from Earth Sun [i] 25.379995 days (Carrington rotation) 35 days (high latitude) 25 d 9 h 7 m 11.6 s 35 d ~28 days (equatorial) [2] Mercury: 58.6462 days [3 ...
The sun, Earth and Jupiter will nearly align perfectly in the solar system on Monday, Sept. 26, during an event that happens once every 13 months called the Jupiter opposition.
Derivative of −Δt. The axis on the right shows the length of the solar day. For Earth, the synodic day is not constant, and changes over the course of the year due to the eccentricity of Earth's orbit around the Sun and the axial tilt of the Earth. [3] The longest and shortest synodic days' durations differ by about 51 seconds. [4]