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It is approximately 24 hours, 39 minutes, 35 seconds long. A Martian year is approximately 668.6 sols, equivalent to approximately 687 Earth days [1] or 1.88 Earth years. The sol was adopted in 1976 during the Viking Lander missions and is a measure of time mainly used by NASA when, for example, scheduling the use of a Mars rover. [2] [3]
The actual landing site was 0.900778° (19.8 km) east of that, corresponding to 3 minutes and 36 seconds later in local solar time. The date is kept using a mission clock sol count with the landing occurring on Sol 0, corresponding to MSD 47776 (mission time zone); the landing occurred around 16:35 LMST, which is MSD 47777 01:02 AMT.
If the Sun–Neptune distance is scaled to 100 metres (330 ft), then the Sun would be about 3 cm (1.2 in) in diameter (roughly two-thirds the diameter of a golf ball), the giant planets would be all smaller than about 3 mm (0.12 in), and Earth's diameter along with that of the other terrestrial planets would be smaller than a flea (0.3 mm or 0. ...
Solar cycle 12: 1878 – Dec 3.7 1883 – Dec 124 57 5-0 11-3 Solar cycle 13: 1890 – Mar 8.3 1894 – Jan 147 65 3-10 11-10 Solar cycle 14: 1902 – Jan 4.5 1906 – Feb 107 54 4-1 11-6 Solar cycle 15: 1913 – Jul 2.5 1917 – Aug 176 73 4-1 10-1 Solar cycle 16: 1923 – Aug 9.3 1928 – Apr 130 68 4-8 10-1 Solar cycle 17: 1933 – Sep 5.8 ...
The Solar System is traveling at an average speed of 230 km/s (828,000 km/h) or 143 mi/s (514,000 mph) within its trajectory around the Galactic Center, [3] a speed at which an object could circumnavigate the Earth's equator in 2 minutes and 54 seconds; that speed corresponds to approximately 1/1300 of the speed of light.
As part of the interplanetary magnetic field, the heliosphere shields the Solar System from significant amounts of cosmic ionizing radiation; uncharged gamma rays are, however, not affected. [1] Its name was likely coined by Alexander J. Dessler , who is credited with the first use of the word in the scientific literature in 1967. [ 2 ]
In astronomy, coordinate systems are used for specifying positions of celestial objects (satellites, planets, stars, galaxies, etc.) relative to a given reference frame, based on physical reference points available to a situated observer (e.g. the true horizon and north to an observer on Earth's surface). [1]
The lookback time, , is an age difference: the age of the universe now, , minus the age of the universe when an photon was emitted at a distant location, . The lookback time depends upon the cosmological model: = ′ (+ ′) (′) where = (+) + (+) + and means the present day density parameters for mass and is the cosmological constant. [8]