Lunar swirls

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Lunar Reconnaissance Orbiter Wide Angle Camera image of Reiner Gamma Reiner Gamma.jpg
Lunar Reconnaissance Orbiter Wide Angle Camera image of Reiner Gamma
Another view of Reiner Gamma swirls Reiner-gamma-clem1.jpg
Another view of Reiner Gamma swirls
Mare Ingenii Mare Ingenii 2075 med.jpg
Mare Ingenii
Swirls east of Firsov crater, from Apollo 10 AS10-30-4365 Swirls near Firsov crater.jpg
Swirls east of Firsov crater, from Apollo 10

Lunar swirls are enigmatic features found across the Moon's surface, which are characterized by having a high albedo, appearing optically immature (i.e. having the optical characteristics of a relatively young regolith), and (often) having a sinuous shape. Their curvilinear shape is often accentuated by low albedo regions that wind between the bright swirls. They appear to overlay the lunar surface, superposed on craters and ejecta deposits, but impart no observable topography. Swirls have been identified on the lunar maria and on highlands - they are not associated with a specific lithologic composition. Swirls on the maria are characterized by strong albedo contrasts and complex, sinuous morphology, whereas those on highland terrain appear less prominent and exhibit simpler shapes, such as single loops or diffuse bright spots.

Contents

Association with magnetic anomalies

The lunar swirls are coincident with regions of the magnetic field of the Moon with relatively high strength on a planetary body that lacks, and may never have had, an active core dynamo with which to generate its own magnetic field. Every swirl has an associated magnetic anomaly, but not every magnetic anomaly has an identifiable swirl. Orbital magnetic field mapping by the Apollo 15 and 16 sub-satellites, Lunar Prospector, and Kaguya show regions with a local magnetic field. Because the Moon has no currently active global magnetic field, these regional anomalies are regions of remnant magnetism; their origin remains controversial.[ citation needed ]

Formation models

There are three leading models for swirl formation. Each model must address two characteristics of lunar swirls formation, namely that a swirl is optically immature, and that it is associated with magnetic anomaly.

Models for creation of the magnetic anomalies associated with lunar swirls point to the observation that several of the magnetic anomalies are antipodal to the younger, large impact basins on the Moon. [1]

Cometary impact model

This model argues that the high albedo of the swirls is the result of an impact with a comet. The impact would cause scouring of the top-most surface regolith by the coma's turbulent flow of gas and dust, which exposed fresh material and redeposited the fine, scoured material in discrete deposits. [2] According to this model, the associated strong magnetic anomalies are the result of magnetization of near-surface materials heated above the Curie temperature through hyper-velocity gas collisions and micro-impacts as the coma impacted the surface. Proponents of the cometary impact model consider the occurrence of many swirls antipodal to the major basins to be coincidental or the result of incomplete mapping of swirl locations. [3] [4]

Solar wind shielding model

This model argues that swirls are formed because lighter-colored regolith is protected from the solar wind due to a magnetic anomaly. [5] The swirls represent exposed silicate materials whose albedos have been selectively preserved over time from the effects of space weathering via deflection of solar wind ion bombardment. According to this model, optical maturation of exposed silicate surfaces is a result of solar wind ion bombardment. This model suggests that swirl formation is a continuing process, which began after creation of the magnetic anomaly.

Mathematical simulations conducted in 2018 showed that lava tubes could have become magnetic as they cooled, which would provide a magnetic field consistent with the observations near the lunar swirls. [6]

Dust transport model

This model argues that weak electric fields created by interaction between the crustal magnetic anomalies and the solar wind plasma could attract or repel electrically charged fine dust. High–albedo feldspathic material is the dominant component of the finest particles of lunar soil. Electrostatic movement of dust lofted above the surface during terminator crossings could cause this material to preferentially accumulate and form the bright, looping swirl patterns. [7] [8]

Satellite measurements

Direct magnetic observations of the lunar swirls have been conducted by several lunar spacecraft, including Clementine and Lunar Prospector . The results of these observations are inconsistent with the Cometary impact model. [9] Further observations by the Lunar Reconnaissance Orbiter support the model that solar wind is being deflected by a magnetic field.[ citation needed ]

Spectral observations by the Moon Mineralogy Mapper instrument on Chandrayaan-1 confirmed that the lighter-colored regions are deficient in hydroxide, which also supports the hypothesis that solar wind is being deflected in the pale areas. [10]

As of 2018, a CubeSat mission concept is under study at NASA, with the goal of understanding the formation of the lunar swirls. The proposed Bi-sat Observations of the Lunar Atmosphere above Swirls , or BOLAS mission would involve two small satellites connected with a 25 km (16 mi) space tether. The lower CubeSat would orbit at an altitude of six miles above the surface. [11] [12]

Onsite investigations

NASA intends to send a rover to Reiner Gamma to obtain in-situ observations of the surface materials there. Funding for the Lunar Vertex mission, run by the JHU Applied Physics Laboratory, was selected for flight through the PRISM call for proposals. [13] [14] Delivery of the rover for the mission was included in the CLPS CP-11 task order. [15] The rover, carrying a multispectral microscope, will determine coarseness and brightness of surface particles and transmit its data to the lander, which will communicate with Earth-based handlers. [16] [17] [18]

See also

Related Research Articles

<span class="mw-page-title-main">Moon</span> Natural satellite orbiting Earth

The Moon is Earth's only natural satellite. It orbits at an average distance of 384,400 km (238,900 mi), about 30 times the diameter of Earth. Over time Earth's gravity has caused tidal locking, causing the same side of the Moon to always face Earth. Because of this, the lunar day and the lunar month are the same length, at 29.5 Earth days. The Moon's gravitational pull – and to a lesser extent, the Sun's – are the main drivers of Earth's tides.

<span class="mw-page-title-main">Solar wind</span> Stream of charged particles from the Sun

The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. This plasma mostly consists of electrons, protons and alpha particles with kinetic energy between 0.5 and 10 keV. The composition of the solar wind plasma also includes a mixture of materials found in the solar plasma: trace amounts of heavy ions and atomic nuclei of elements such as C, N, O, Ne, Mg, Si, S, and Fe. There are also rarer traces of some other nuclei and isotopes such as P, Ti, Cr, and 58Ni, 60Ni, and 62Ni. Superimposed with the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar latitude and longitude. Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field. The boundary separating the corona from the solar wind is called the Alfvén surface.

<span class="mw-page-title-main">Regolith</span> A layer of loose, heterogeneous superficial deposits covering solid rock

Regolith is a blanket of unconsolidated, loose, heterogeneous superficial deposits covering solid rock. It includes dust, broken rocks, and other related materials and is present on Earth, the Moon, Mars, some asteroids, and other terrestrial planets and moons.

<span class="mw-page-title-main">Mare Marginis</span> Lunar mare

Mare Marginis ; MAR-jin-iss) is a lunar mare that lies on the very edge of the lunar nearside. The selenographic coordinates of this feature are 13.3° N, 86.1° E, and the diameter is 358 km.

<i>Lunar Prospector</i> Third mission of the Discovery program; polar orbital reconnaissance of the Moon

Lunar Prospector was the third mission selected by NASA for full development and construction as part of the Discovery Program. At a cost of $62.8 million, the 19-month mission was designed for a low polar orbit investigation of the Moon, including mapping of surface composition including lunar hydrogen deposits, measurements of magnetic and gravity fields, and study of lunar outgassing events. The mission ended July 31, 1999, when the orbiter was deliberately crashed into a crater near the lunar south pole, after the presence of hydrogen was successfully detected.

<span class="mw-page-title-main">Descartes (crater)</span> Crater on the Moon

Descartes is a heavily worn lunar impact crater that is located in the rugged south-central highlands of the Moon. To the southwest is the crater Abulfeda. It is named after the French philosopher, mathematician and physicist René Descartes.

<span class="mw-page-title-main">Reiner Gamma</span> Geographical feature of the Moon

Reiner Gamma (γ) is a geographical feature of the Moon known as a lunar swirl. It is one of the most visible lunar swirls from Earth, visible from most telescopes. It was originally thought to be a lunar highland, but scientists eventually realized that it cast no shadow on the moon.

<span class="mw-page-title-main">Interplanetary medium</span> Material which fills the Solar System

The interplanetary medium (IPM) or interplanetary space consists of the mass and energy which fills the Solar System, and through which all the larger Solar System bodies, such as planets, dwarf planets, asteroids, and comets, move. The IPM stops at the heliopause, outside of which the interstellar medium begins. Before 1950, interplanetary space was widely considered to either be an empty vacuum, or consisting of "aether".

<span class="mw-page-title-main">Leibnitz (crater)</span> Lunar impact crater

Leibnitz is a huge lunar impact crater that is located in the southern hemisphere on the far side of the Moon. This formation is the same size as Clavius on the near side. It is located to the east-southeast of Mare Ingenii, and is joined to the northeast rim of Von Kármán. Attached to the eastern rim of Leibnitz is Davisson, and intruding into the southeast rim is Finsen. Farther to the west is the large Oppenheimer.

<span class="mw-page-title-main">Lunar water</span> Presence of water on the Moon

Lunar water is water that is present on the Moon. Diffuse water molecules in low concentrations can persist at the Moon's sunlit surface, as discovered by the SOFIA observatory in 2020. Gradually, water vapor is decomposed by sunlight, leaving hydrogen and oxygen lost to outer space. Scientists have found water ice in the cold, permanently shadowed craters at the Moon's poles. Water molecules are also present in the extremely thin lunar atmosphere.

<span class="mw-page-title-main">Gerasimovich (crater)</span> Lunar impact crater

Gerasimovich is a lunar impact crater on the far side of the Moon. It lies beyond the western limb, to the west-northwest of the immense Mare Orientale impact basin. The outer blanket of ejecta from this impact reaches nearly to the rim of Gerasimovich. Nearby craters of note include Houzeau to the north and the smaller Ellerman to the southeast.

<span class="mw-page-title-main">Geology of the Moon</span> Structure and composition of the Moon

The geology of the Moon is quite different from that of Earth. The Moon lacks a true atmosphere, and the absence of free oxygen and water eliminates erosion due to weather. Instead, the surface is eroded much more slowly through the bombardment of the lunar surface by micrometeorites. It does not have any known form of plate tectonics, it has a lower gravity, and because of its small size, it cooled faster. In addition to impacts, the geomorphology of the lunar surface has been shaped by volcanism, which is now thought to have ended less than 50 million years ago. The Moon is a differentiated body, with a crust, mantle, and core.

<span class="mw-page-title-main">Space weathering</span> Type of weathering

Space weathering is the type of weathering that occurs to any object exposed to the harsh environment of outer space. Bodies without atmospheres take on many weathering processes:

<span class="mw-page-title-main">Lunar soil</span> Rock dust covering the Moon

Lunar soil is the fine fraction of lunar regolith found on the surface of the Moon and contributes to the Moon's tenuous atmosphere. Lunar soil differs in its origin and properties significantly from terrestrial soil.

<span class="mw-page-title-main">Magnetic field of the Moon</span>

The magnetic field of the Moon is very weak in comparison to that of the Earth; the major difference is the Moon does not have a dipolar magnetic field currently, so that the magnetization present is varied and its origin is almost entirely crustal in location; so it's difficult to compare as a percentage to Earth. But, one experiment discovered that lunar rocks formed 1 - 2.5 billion years ago were created in a field of about 5 microtesla (μT), compared to present day Earth's 50 μT. During the Apollo program several magnetic field strength readings were taken with readings ranging from a low of 6γ (6nT) at the Apollo 15 site to a maximum of 313γ (0.31μT) at the Apollo 16 site, note these readings were recorded in gammas(γ) a now outdated unit of magnetic flux density equivalent to 1nT.

The Solar System Exploration Research Virtual Institute (SSERVI), originally the NASA Lunar Science Institute, is an organization, established by NASA in 2008, that supplemented and extended existing NASA lunar science programs. Supported by the NASA Science Mission Directorate (SMD) and the Exploration Systems Mission Directorate (ESMD), SSERVI is a NASA program office located at the NASA Ames Research Center and was modeled on the NASA Astrobiology Institute (NAI) with dispersed teams across the nation working together to help lead the agency's research activities related to NASA's human exploration goals. Competitively selected team investigations focused on one or more aspects of lunar science investigations of the Moon, from the Moon, and on the Moon.

<span class="mw-page-title-main">Lunar south pole</span> Southernmost point on the Moon

The lunar south pole is the southernmost point on the Moon. It is of interest to scientists because of the occurrence of water ice in permanently shadowed areas around it. The lunar south pole region features craters that are unique in that the near-constant sunlight does not reach their interior. Such craters are cold traps that contain fossil record of hydrogen, water ice, and other volatiles dating from the early Solar System. In contrast, the lunar north pole region exhibits a much lower quantity of similarly sheltered craters.

<span class="mw-page-title-main">Planetary science</span> Science of planets and planetary systems

Planetary science is the scientific study of planets, celestial bodies and planetary systems and the processes of their formation. It studies objects ranging in size from micrometeoroids to gas giants, aiming to determine their composition, dynamics, formation, interrelations and history. It is a strongly interdisciplinary field, which originally grew from astronomy and Earth science, and now incorporates many disciplines, including planetary geology, cosmochemistry, atmospheric science, physics, oceanography, hydrology, theoretical planetary science, glaciology, and exoplanetology. Allied disciplines include space physics, when concerned with the effects of the Sun on the bodies of the Solar System, and astrobiology.

<span class="mw-page-title-main">BOLAS (spacecraft)</span>

Bi-sat Observations of the Lunar Atmosphere above Swirls (BOLAS) is a spacecraft mission concept that would orbit the Moon at very low altitude in order to study the lunar surface. The concept, currently under study by NASA, involves two small identical CubeSat satellites connected vertically above the lunar surface by a 25 km long tether. The mission goal would be to understand the hydrogen cycle on the Moon, dust weathering, and the formation of lunar swirls.

<span class="mw-page-title-main">Lunar resources</span> Potential natural resources on the Moon

The Moon bears substantial natural resources which could be exploited in the future. Potential lunar resources may encompass processable materials such as volatiles and minerals, along with geologic structures such as lava tubes that, together, might enable lunar habitation. The use of resources on the Moon may provide a means of reducing the cost and risk of lunar exploration and beyond.

References

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  14. "Lunar Vertex". JHUAPL.
  15. "NASA Payloads for (CLPS PRISM) CP-11 – Intuitive Machines Nova-C Lander". NASA.
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See also