July 4, 2016 First Day of Spring on Mars & Juno Arrival at Jupiter". mars.nasa.gov . Retrieved 22 December 2021. Holt, John W.; Safaeinili, Ali; Plaut, Jeffrey J.; etal. (21 November 2008). "Radar Sounding Evidence for Buried Glaciers in the Southern Mid-Latitudes of Mars". Science. 322 (5905): 1235–1238. Bibcode: 2008Sci...322.1235H. doi: 10.1126/science.1164246. hdl: 11573/67950. ISSN 0036-8075. JSTOR 20145331. PMID 19023078. S2CID 36614186. Because Mars has no oceans and hence no " sea level", a zero-elevation surface had to be selected as a reference level; this is called the areoid [77] of Mars, analogous to the terrestrial geoid. [78] Zero altitude was defined by the height at which there is 610.5 Pa (6.105 mbar) of atmospheric pressure. [79] This pressure corresponds to the triple point of water, and it is about 0.6% of the sea level surface pressure on Earth (0.006 atm). [80] a b Jacqué, Dave (26 September 2003). "APS X-rays reveal secrets of Mars' core". Argonne National Laboratory. Archived from the original on 21 February 2009 . Retrieved 1 July 2006.

White Mars: A response to KSR’s MARS trilogy | Fantasy

As of 2023 [update], Mars is host to thirteen functioning spacecraft. Eight are in orbit : 2001 Mars Odyssey, Mars Express, Mars Reconnaissance Orbiter, MAVEN, ExoMars Trace Gas Orbiter, the Hope orbiter, and the Tianwen-1 orbiter. [238] [239] Another five are on the surface: the Mars Science Laboratory Curiosity rover, the Perseverance rover, the Ingenuity helicopter, the Tianwen-1 lander, and the Zhurong rover. [240]

Franklin Clarence Mars (September 24, 1883 – April 8, 1934) – founder of Mars, Inc. Invented the Milky Way bar.

Mars family - Wikipedia Mars family - Wikipedia

a b c d e f g h i The Five Principles of Mars [ permanent dead link]. Signed by Mars family members: Alexandra B. Airth, Christa M. Badger, Forrest E. Mars Jr., Frank E. Mars, Jacqueline B. Mars, John F. Mars, Michael J. Mars, Pamela D. Mars-Wright, Stephen M. Badger II, Valerie A. Mars, Victoria B. Mars. a b "Mars Opposition | Mars in our Night Sky". NASA's Mars Exploration Program . Retrieved 7 December 2021.Heldmann, Jennifer L.; etal. (7 May 2005). "Formation of Martian gullies by the action of liquid water flowing under current Martian environmental conditions" (PDF). Journal of Geophysical Research. 110 (E5): Eo5004. Bibcode: 2005JGRE..110.5004H. CiteSeerX 10.1.1.596.4087. doi: 10.1029/2004JE002261. hdl: 2060/20050169988. S2CID 1578727. Archived from the original (PDF) on 1 October 2008 . Retrieved 17 September 2008. 'conditions such as now occur on Mars, outside of the temperature-pressure stability regime of liquid water'... 'Liquid water is typically stable at the lowest elevations and at low latitudes on the planet because the atmospheric pressure is greater than the vapor pressure of water and surface temperatures in equatorial regions can reach 273 K for parts of the day [Haberle et al.., 2001]'

Mars - Wikipedia Mars - Wikipedia

The atmosphere of Mars consists of about 96% carbon dioxide, 1.93% argon and 1.89% nitrogen along with traces of oxygen and water. [2] [113] [107] The atmosphere is quite dusty, containing particulates about 1.5 μm in diameter which give the Martian sky a tawny color when seen from the surface. [114] It may take on a pink hue due to iron oxide particles suspended in it. [21] The concentration of methane in the Martian atmosphere fluctuates from about 0.24 ppb during the northern winter to about 0.65 ppb during the summer. [115] Estimates of its lifetime range from 0.6 to 4 years, [116] [117] so its presence indicates that an active source of the gas must be present. Methane could be produced by non-biological process such as serpentinization involving water, carbon dioxide, and the mineral olivine, which is known to be common on Mars, [118] or by Martian life. [119] Escaping atmosphere on Mars ( carbon, oxygen, and hydrogen) by MAVEN in UV [120] Carr, Michael H. (2006). The surface of Mars. Vol.6. Cambridge University Press. p.16. ISBN 978-0-521-87201-0. Above ground, nearer to base, are many telescopes as well as two wooden platforms to observe the heavens. Wood is a very suitable material to build with in the cold expanse of Dome C as no fungi that rot wood can survive. Andrews, Robin George (25 October 2023). "A Radioactive Sea of Magma Hides Under the Surface of Mars - The discovery helped to show why the red planet's core is not as large as earlier estimates had suggested it might be". The New York Times. Archived from the original on 25 October 2023 . Retrieved 26 October 2023. Mitchell, Karl L.; Wilson, Lionel (2003). "Mars: recent geological activity: Mars: a geologically active planet". Astronomy & Geophysics. 44 (4): 4.16–4.20. Bibcode: 2003A&G....44d..16M. doi: 10.1046/j.1468-4004.2003.44416.x.a b c d Mallama, Anthony; Hilton, James L. (October 2018). "Computing apparent planetary magnitudes for The Astronomical Almanac". Astronomy and Computing. 25: 10–24. arXiv: 1808.01973. Bibcode: 2018A&C....25...10M. doi: 10.1016/j.ascom.2018.08.002. S2CID 69912809. Researchers suspect much of the low northern plains of the planet were covered with an ocean hundreds of meters deep, though this theory remains controversial. [184] In March 2015, scientists stated that such an ocean might have been the size of Earth's Arctic Ocean. This finding was derived from the ratio of protium to deuterium in the modern Martian atmosphere compared to that ratio on Earth. The amount of Martian deuterium is eight times the amount on Earth, suggesting that ancient Mars had significantly higher levels of water. Results from the Curiosity rover had previously found a high ratio of deuterium in Gale Crater, though not significantly high enough to suggest the former presence of an ocean. Other scientists caution that these results have not been confirmed, and point out that Martian climate models have not yet shown that the planet was warm enough in the past to support bodies of liquid water. [185] Near the northern polar cap is the 81.4 kilometres (50.6mi) wide Korolev Crater, which the Mars Express orbiter found to be filled with approximately 2,200 cubic kilometres (530cumi) of water ice. [186] Proportion of water ice present in the upper meter of the Martian surface for lower (top) and higher (bottom) latitudes