Mare volcanism in the lunar farside Moscoviense region: Implication for lateral variation in magma production of the Moon

2009 ◽  
Vol 36 (21) ◽  
Author(s):  
Tomokatsu Morota ◽  
Junichi Haruyama ◽  
Chikatoshi Honda ◽  
Makiko Ohtake ◽  
Yasuhiro Yokota ◽  
...  
Keyword(s):  
The Moon ◽  
Lateral Variation ◽  
Lunar Farside ◽  
Mare Volcanism

scholarly journals Transformative science from the lunar farside: observations of the dark ages and exoplanetary systems at low radio frequencies

2020 ◽  
Vol 379 (2188) ◽  
pp. 20190564 ◽  
Author(s):  
Jack O. Burns
Keyword(s):  
Low Frequency ◽  
Dipole Antenna ◽  
The Moon ◽  
Dipole Antennas ◽  
Dark Ages ◽  
Exoplanetary Systems ◽  
Single Cross ◽  
Lunar Farside ◽  
Exotic Physics ◽  
Orbiting Spacecraft

The farside of the Moon is a pristine, quiet platform to conduct low radio frequency observations of the early Universe's Dark Ages, as well as space weather and magnetospheres associated with habitable exoplanets. In this paper, the astrophysics associated with NASA-funded concept studies will be described including a lunar-orbiting spacecraft, DAPPER, that will measure the 21 cm global spectrum at redshifts ≈40–80, and an array of low frequency dipoles on the lunar farside surface, FARSIDE, that would detect exoplanet magnetic fields. DAPPER observations (17–38 MHz), using a single cross-dipole antenna, will determine the amplitude of the 21 cm spectrum to the level required to distinguish the standard ΛCDM cosmological model from those produced by exotic physics such as nongravitational dark matter interactions. FARSIDE has a notional architecture consisting of 128 dipole antennas deployed across a 10 km area by a rover. FARSIDE would image the entire sky each minute in 1400 channels over 0.1–40 MHz. This would enable monitoring of the nearest stellar systems for the radio signatures of coronal mass ejections and energetic particle events, and would also detect the magnetospheres of the nearest candidate habitable exoplanets. In addition, FARSIDE would provide a pathfinder for power spectrum measurements of the Dark Ages. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades’.

scholarly journals Timing and duration of mare volcanism in the central region of the northern farside of the Moon

2011 ◽  
Vol 63 (1) ◽  
pp. 5-13 ◽  
Author(s):  
Tomokatsu Morota ◽  
◽  
Junichi Haruyama ◽  
Makiko Ohtake ◽  
Tsuneo Matsunaga ◽  
...  
Keyword(s):  
Central Region ◽  
The Moon ◽  
Mare Volcanism

Lunar stratigraphy

1977 ◽  
Vol 285 (1327) ◽  
pp. 549-553 ◽  
Keyword(s):  
Early History ◽  
Age Dating ◽  
The Moon ◽  
Relative Age ◽  
The Past ◽  
History Of ◽  
Basin Formation ◽  
Absolute Age ◽  
Mare Volcanism ◽  
The Impact

The lunar scene is a continuous panorama of ancient impact physiography. Multi-ringed circular basins and smaller craters scar the Moon’s highlands and provide evidence of a violent early history. Basin formation, the major material-transporting mechanism on the Moon, produces a deep inner depression, one or more benches, a basin rim, and radially lineated ejecta. Study of lunar photographs indicates that, on a relative age scale, subdued basin and crater features are older representations of younger, well-preserved forms. Absolute age dating of returned samples makes it feasible to calibrate this relative age scale. All the larger basins were formed during pre-Nectarian, Nectarian and Imbrian times, i.e. 4.6- 3.9 Ga ago. Following this major sculpturing episode, and during the Imbrian and Eratosthenian times, mare volcanism became the most important mode of deposition of lunar surface materials. Basaltic lavas from deep-seated sources flowed to partially fill the impact basins and cover their peripheral troughs and surrounding lowlands between 3.8 and 3.2 Ga ago. This occurred more frequently on the near side than on the far side, probably because the farside crust is thicker. During the past 1 Ga, i.e. Copemican time, only a small number of craters were formed in both highland and mare rocks. Successes and failures of photogeologists in studying lunar stratigraphy provide the necessary lessons for understanding the geological history of the terrestrial planets. This is particularly true since both Mars and Mercury display many types of features in common with the Moon.

scholarly journals Low Frequency Radio Astronomy from the Moon

1998 ◽  
Vol 11 (2) ◽  
pp. 988-989
Author(s):  
D.L. Jones ◽  
K.W. Weiler
Keyword(s):  
High Frequency ◽  
Angular Resolution ◽  
Low Frequency ◽  
High Angular Resolution ◽  
Radio Sources ◽  
The Moon ◽  
Interstellar Scintillation ◽  
Wide Range ◽  
Lunar Farside

AbstractThe radio sky at frequencies of several MHz and below is essentially unexplored with high angular resolution due to refraction and opacity in the Earth’s ionosphere. An interferometer array in space providing arcminute resolution images would allow a wide range of problems in solar, planetary, galactic, and extragalactic astronomy to be attacked. These include the evolution of solar and planetary radio bursts, interplanetary and interstellar scintillation, the distribution of low energy cosmic rays and diffuse ionized hydrogen in our galaxy, the determination of spectral turnover frequencies and magnetic field strengths in galactic and extragalactic radio sources, searches for “fossil” radio galaxies which are no longer detectable by high frequency surveys, and searches for new sources of coherent radio emission. In addition, it is likely that unexpected objects and emission processes will be discovered by such an instrument, as has often happened when high resolution observations first become possible in a new spectral region. The Moon can provide shielding from terrestrial interference (and from the Sun half of the time) and consequently the lunar farside surface offers an ideal site of a low frequency radio array.

scholarly journals SETI from the Moon: Avoiding Radio Pollution for Future Radio-Astronomy

1998 ◽  
Vol 11 (2) ◽  
pp. 996-999 ◽  
Author(s):  
J. Heidmann
Keyword(s):  
Radio Frequency ◽  
Radio Astronomy ◽  
High Sensitivity ◽  
Radio Frequency Interference ◽  
The Moon ◽  
Lunar Farside

AbstractBecause of the ever increasing human-made radio frequency interference (RFI), we propose to IAU a Resolution for protecting the well singled out lunar farside 100 km diameter SAHA crater from any future RFI for the scientific benefit of the coming decades high-sensitivity radioastronomy at large. Immediate and pragmatic action is strongly recommended. Our strategy, different from the ones of a recent ITU Recommendation, could increase our bargaining possibilities.

The motion of a lunar orbiter

1966 ◽  
Vol 25 ◽  
pp. 373
Author(s):  
Y. Kozai
Keyword(s):  
Degrees Of Freedom ◽  
Dimensional Space ◽  
Artificial Satellite ◽  
Equations Of Motion ◽  
Triaxial Ellipsoid ◽  
The Moon ◽  
Secular Motion ◽  
The Earth ◽  
Close Satellite ◽  
The Mean

The motion of an artificial satellite around the Moon is much more complicated than that around the Earth, since the shape of the Moon is a triaxial ellipsoid and the effect of the Earth on the motion is very important even for a very close satellite.The differential equations of motion of the satellite are written in canonical form of three degrees of freedom with time depending Hamiltonian. By eliminating short-periodic terms depending on the mean longitude of the satellite and by assuming that the Earth is moving on the lunar equator, however, the equations are reduced to those of two degrees of freedom with an energy integral.Since the mean motion of the Earth around the Moon is more rapid than the secular motion of the argument of pericentre of the satellite by a factor of one order, the terms depending on the longitude of the Earth can be eliminated, and the degree of freedom is reduced to one.Then the motion can be discussed by drawing equi-energy curves in two-dimensional space. According to these figures satellites with high inclination have large possibilities of falling down to the lunar surface even if the initial eccentricities are very small.The principal properties of the motion are not changed even if plausible values ofJ3andJ4of the Moon are included.This paper has been published in Publ. astr. Soc.Japan15, 301, 1963.

Laboratory Simulation of Lunar Luminescence

1962 ◽  
Vol 14 ◽  
pp. 441-444 ◽  
Author(s):  
J. E. Geake ◽  
H. Lipson ◽  
M. D. Lumb
Keyword(s):  
Science And Technology ◽  
Laboratory Simulation ◽  
The Moon ◽  
Physics Department ◽  
Luminescent Spectrum

Work has recently begun in the Physics Department of the Manchester College of Science and Technology on an attempt to simulate lunar luminescence in the laboratory. This programme is running parallel with that of our colleagues in the Manchester University Astronomy Department, who are making observations of the luminescent spectrum of the Moon itself. Our instruments are as yet only partly completed, but we will describe briefly what they are to consist of, in the hope that we may benefit from the comments of others in the same field, and arrange to co-ordinate our work with theirs.

Formation of Lunar Craters and Bright Rays as a Result of Meteorite Impacts

1962 ◽  
Vol 14 ◽  
pp. 415-418
Author(s):  
K. P. Stanyukovich ◽  
V. A. Bronshten
Keyword(s):  
Explosive Charge ◽  
The Moon ◽  
Meteorite Impacts ◽  
The Earth ◽  
Lunar Craters ◽  
The Impact

The phenomena accompanying the impact of large meteorites on the surface of the Moon or of the Earth can be examined on the basis of the theory of explosive phenomena if we assume that, instead of an exploding meteorite moving inside the rock, we have an explosive charge (equivalent in energy), situated at a certain distance under the surface.

The Origin of the Moon

1962 ◽  
Vol 14 ◽  
pp. 149-155 ◽  
Author(s):  
E. L. Ruskol
Keyword(s):  
Chemical Composition ◽  
Solar System ◽  
The Moon ◽  
The Earth ◽  
The Difference ◽  
Origin Of The Moon

The difference between average densities of the Moon and Earth was interpreted in the preceding report by Professor H. Urey as indicating a difference in their chemical composition. Therefore, Urey assumes the Moon's formation to have taken place far away from the Earth, under conditions differing substantially from the conditions of Earth's formation. In such a case, the Earth should have captured the Moon. As is admitted by Professor Urey himself, such a capture is a very improbable event. In addition, an assumption that the “lunar” dimensions were representative of protoplanetary bodies in the entire solar system encounters great difficulties.

The Origin of the Moon and its Relationship to the Origin of the Solar System

1962 ◽  
Vol 14 ◽  
pp. 133-148 ◽  
Author(s):  
Harold C. Urey
Keyword(s):  
Solar System ◽  
The Moon ◽  
The Past ◽  
The Earth ◽  
Short Period ◽  
Origin Of The Moon

During the last 10 years, the writer has presented evidence indicating that the Moon was captured by the Earth and that the large collisions with its surface occurred within a surprisingly short period of time. These observations have been a continuous preoccupation during the past years and some explanation that seemed physically possible and reasonably probable has been sought.

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