Orbit of Mars

Mars has an orbit with a semimajor axis of 1.524 astronomical units (228 million km), and an eccentricity of 0.0934.[1][2] The planet orbits the Sun in 687 days[3] and travels 9.55 AU in doing so,[4] making the average orbital speed 24 km/s.

Orbit of Mars relative to the orbits of inner Solar system planets

The eccentricity is greater than that of every other planet except Mercury, and this causes a large difference between the aphelion and perihelion distances—they are 1.6660 and 1.3814 AU.[5]

Changes in the orbit

Mars is in the midst of a long-term increase in eccentricity. It reached a minimum of 0.079 about 19 millennia ago, and will peak at about 0.105 after about 24 millennia from now (and with perihelion distances a mere 1.3621 astronomical units). The orbit is at times near circular: it was 0.002 1.35 million years ago, and will be about 0.01 a million years into the future. The maximum eccentricity between those two minima is 0.12.[6]

Oppositions

Mars reaches opposition when there is a 180° difference between the geocentric longitudes of it and the Sun. At a time near opposition (within 8½ days) the Earth–Mars distance is as small as it will get during that 780-day synodic period.[7] Every opposition has some significance because Mars is visible from Earth all night, high and fully lit, but the ones of special interest happen when Mars is near perihelion, because this is when Mars is also nearest to Earth. One perihelic opposition is followed by another either 15 or 17 years later. In fact every opposition is followed by a similar one 7 or 8 synodic periods later, and by a very similar one 37 synodic periods (79 years) later.[8] In the so-called perihelic opposition Mars is closest to the Sun and is particularly close to Earth: Oppositions range from about 0.68 AU when Mars is near aphelion to only about 0.37 AU when Mars is near perihelion.[9]

Close approaches to Earth

Mars comes closer to Earth than any other planet save Venus at its nearest—56 million km is the closest distance between Mars and Earth, whereas the closest Venus comes to Earth is 40 million km. The minimum distance between Earth and Mars has been declining over the years, and in 2003 the minimum distance was 55.76 million km, nearer than any such encounter in almost 60,000 years (57,617 BC). The record minimum distance between Earth and Mars in 2729 will stand at 55.65 million km. In the year 3818, the record will stand at 55.44 million km, and the distances will continue to decrease for about 24,000 years.[10]

Historical importance

Until the work of Johannes Kepler (1571–1630), a German astronomer, the prevailing belief was that the sun and planets orbited the earth. In 1543, Nicolaus Copernicus had proposed that all the planets orbited in circles around the sun, but his theory did not give very satisfactory predictions and was largely ignored. When Kepler studied his boss Tycho Brahe's observations of Mars's position in the sky on many nights, Kepler realized that Mars's orbit could not be a circle. After years of analysis, Kepler discovered that Mars's orbit was likely to be an ellipse, with the Sun at one of the ellipse's focal points. This, in turn, led to Kepler's discovery that all planets orbit the Sun in elliptical orbits, with the Sun at one of the two focal points. This became the first of Kepler's three laws of planetary motion.[11][12]

Accuracy/predictability

From the perspective of all but the most demanding, the path of Mars is simple. An equation in Astronomical Algorithms that assumes an unperturbed elliptical orbit predicts the perihelion and aphelion times with an error of "a few hours".[13] Using orbital elements to calculate those distances agrees to actual averages to at least five significant figures. Formulas for computing position straight from orbital elements typically do not provide or need corrections for the effects of other planets.[14]

For a higher level of accuracy the perturbations of planets are required. These are well known, and are believed to be modeled well enough to achieve high accuracy. These are all of the bodies that need to be considered for even many demanding problems. When Aldo Vitagliano calculated the date of close Martian approaches in the distant past or future, he tested the potential effect caused by the uncertainties of the asteroid belt models by running the simulations both with and without the biggest three asteroids, and found the effects were negligible.

Observations are much better now, and space age technology has replaced the older techniques. E. Myles Standish wrote: "Classical ephemerides over the past centuries have been based entirely upon optical observations:almost exclusively, meridian circle transit timings. With the advent of planetary radar, spacecraft missions, VLBI, etc., the situation for the four inner planets has changed dramatically." (8.5.1 page 10) For DE405, created in 1995, optical observations were dropped and as he wrote "initial conditions for the inner four planets were adjusted to ranging data primarily…"[15] The error in DE 405 is known to be about 2 km and is now sub-kilometer.[16]

Although the perturbations on Mars by asteroids have caused problems, they have also been used to estimate the masses of certain asteroids.[17] But improving the model of the asteroid belt is of great concern to those requiring or attempting to provide the highest-accuracy ephemerides.[18]

Orbital parameters

No more than five significant figures are presented in the following table of Mars's orbital elements. To this level of precision, the numbers match very well the VSOP87 elements and calculations derived from them, as well as Standish's (of JPL) 250-year best fit, and calculations using the actual positions of Mars over time.

Distances and eccentricity (AU) (million km)
Semimajor axis 1.5237227.9
Perihelion 1.3814206.7
Aphelion 1.6660249.2
Average[19] 1.5303228.9
Circumference 9.5531429
Closest approach to Earth 0.372755.76
Farthest distance from Earth 2.675400.2
Eccentricity 0.0934
Angles (°)
Inclination 1.850
Period (days) (years)
Orbital 687.01.881
Synodic 779.92.135
Speed (km/s)
Average 24.1
Maximum 26.5
Minimum 22.0

References
  1. Simon, J.L.; Bretagnon, P.; Chapront, J.; Chapront-Touzé, M.; Francou, G.; Laskar, J. (February 1994). "Numerical expressions for precession formulae and mean elements for the Moon and planets". Astronomy and Astrophysics. 282 (2): 663–683. Bibcode:1994A&A...282..663S.
  2. Jean Meeus, Astronomical Formulæ for Calculators. (Richmond, VA: Willmann-Bell, 1988) 99. Elements by F. E. Ross
  3. In ephemeris days of 86 400 seconds. The sidereal and anomalistic years are 686.980 days and 686.996 days long, respectively. (About a 20 minute difference). The sidereal year is the time taken to revolve around the Sun relative to a fixed reference frame. More precisely, the sidereal year is one way to express the rate of change of the mean longitude at one instant, with respect to a fixed equinox. The calculation shows how long it would take for the longitude to change 360 degrees at the given rate. The anomalistic year is the time span between successive perihelion or aphelion passages. This may be calculated in the same manner as the sidereal year, but the mean anomaly is used.
  4. Jean Meeus, Astronomical Algorithms (Richmond, VA: Willmann-Bell, 1998) 238. The formula by Ramanujan is accurate enough.
  5. The averages between 1850 and 2150. The extreme values in that range are 1.66635 and 1.38097 AU
  6. "Archived copy". Archived from the original on 2007-09-07. Retrieved 2007-07-20.CS1 maint: archived copy as title (link) Mars distance and eccentricity, using Solex. By its creator, Aldo Vitagliano
  7. The synodic period may be calculated as 1/(1/p-1/q), where p and q are the smaller and larger sidereal periods.
  8. The synodic period of Mars is 92.9 days longer than its sidereal period of 687.0 days. It has then moved forward 92.9/687.0 times 360, or 48.7 degrees. After seven oppositions it has moved forward 341 degrees, and after eight it has advanced 390 degrees; in the first case its longitude is different from one revolution by 19°, and by 30° in the second. So the situations will then be similar. Similar calculations show that the longitude changes only 2° after 37 oppositions.
  9. Sheehan, William (February 2, 1997). "Appendix 1: Oppositions of Mars, 1901–2035". The Planet Mars: A History of Observation and Discovery. University of Arizona Press. Archived from the original on June 25, 2010. Retrieved January 30, 2010.
  10. Meeus, Jean (March 2003). "When Was Mars Last This Close?" (PDF). Planetarian: 13.
  11. Carr, Michael H.; Malin, Michael C.; Belton, Michael J.S. (July 27, 2018). "Mars". Encyclopædia Britannica Online. p. 2.
  12. William Sheehan, The Planet Mars: A History of Observation and Discovery (Tucson, AZ: The University of Arizona Press, 1996) Chapter 1
  13. Meeus (1998) pp 269–270
  14. see, for example, Simon et al. (1994) p. 681
  15. Standish & Williams (2012). "CHAPTER 8: Orbital Ephemerides of the Sun, Moon, and Planets" (PDF). 2012 version of the Explanatory Supplement
  16. As noted in a 2008 JPL Memorandum regarding DE 421, "The error in the Earth and Mars orbits in DE 405 is now known to be about 2 km, which was good accuracy in 1997 but much worse than the current sub-kilometer accuracy."Folkner; et al. (2008). "The Planetary and Lunar Ephemeris DE421" (PDF). JPL Interoffice Memorandum IOM 343.R-08-003. p. 1
  17. "asteroid." Encyclopædia Britannica. Encyclopædia Britannica Online. Encyclopædia Britannica Inc., 2014. Web. 19 Aug. 2014. http://www.britannica.com/EBchecked/topic/39730/asteroid
  18. "The uncertainty in the Mars orbit for a one-year prediction is about 300 m, as required for the Mars Science Laboratory mission, but grows rapidly for times before and after the spacecraft observation time span due to the influence of asteroids with orbits near that of Mars. The predicted orbit and uncertainty depend greatly on the asteroid model used. "Folkner; et al. (2010). "Uncertainties in the JPL Planetary Ephemeris" (PDF). Proceedings of the Journées. p. 43.
  19. Average distance over times. Constant term in VSOP87. It corresponds to the average taken of many short, equal time intervals.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.