Meteoroid Storms Detected on the Moon

Duennebier, F. K.; Nakamura, Y.; Latham, Gary V.; Dorman, H. J.

doi:10.1126/science.192.4243.1000

Cited by 25 publications

(16 citation statements)

References 5 publications

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“…Particles with masses 50 g to 1000 g (4 to 10 cm diameter at 2 g/cm 3 ) impact the Moon as often as 10 times/day (Duennebier et al 1976). LROC NAC observations (0.5 m/pixel) of (1) very young mare surfaces and (2) regions photographed using the Apollo 15-17 Panoramic Camera will be used to place estimates on the number of small craters (1 to 100 m diameter) that have formed from 1971-2010.…”

Section: Lroc Overview and Scientific Objectivesmentioning

confidence: 99%

Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview

et al. 2010

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The WAC is a 7-color push-frame camera (100 and 400 m/pixel visible and UV, respectively), while the two NACs are monochrome narrow-angle linescan imagers (0.5 m/pixel). The primary mission of LRO is to obtain measurements of the Moon that will enable future lunar human exploration. The overarching goals of the LROC investigation include landing site identification and certification, mapping of permanently polar shadowed and sunlit regions, meter-scale mapping of polar regions, global multispectral imaging, a global morphology base map, characterization of regolith properties, and determination of current impact hazards.

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Section: Lroc Overview and Scientific Objectivesmentioning

confidence: 99%

Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview

et al. 2010

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“…In a recent study Oberst and Nakamura (1987a,b) developed new methods to identify these clusters among the background of sporadic impacts. In addition to the seasonal time as in earlier studies (Duennebier et al, 1976;Dorman et al, 1978), Oberst and Nakamura also used the time of the lunar day, i.e., the lunar phase, at which impacts were detected for identification of clustering.…”

Section: Introductionmentioning

confidence: 99%

Possible relationship between the Farmington meteorite and a seismically detected swarm of meteoroids impacting the Moon

Oberst

1989

Meteoritics

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Abstract— The Farmington ordinary L5 chondrite with its uniquely short cosmic‐ray exposure age of less than 25 000 years may have been a member of a large meteoroid swarm which was detected by the Apollo seismic network when it encountered the Moon in June 1975. The association implies that the parent body of the Farmington meteorite was in an Earth‐crossing orbit at the time the swarm was formed. This supports the idea that at least some meteorites are derived from the observable population of Earth‐crossing asteroids.

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“…The apparent mass and time distributions of the impacting bodies have been studied by Duennebier and Sutton (1974b), Duennebier et al (1975bDuennebier et al ( , 1976, Dorman et al (1978) and Dainty et al (1975b). Characteristically, the impacts produce little shear wave energy since the source is theoretically purely compressional.…”

Section: Selection Of Eventsmentioning

confidence: 99%

“…Thermal moonquakes (Duennebier and Sutton, 1974a;Cooper and Kovach, 1975;Duennebier, 1976) are small events caused by thermal stresses and slumping, and are detectable only near the seismic stations. Nearsurface moonquakes Nakamura, 1977a, Lammlein, 1977Goins et al, 1978b) are probably shallow seismic events.…”

Section: 2 Review Of Previous Workmentioning

confidence: 99%

“…Finally, meteorite impacts, while not considered a seismic source on earth, account for some of the largest seismic sources on the moon (Duennebier and Sutton, 1974b;Duennebier et al, 1975bDuennebier et al, , 1976Dorman et al, 1978;Dainty et al, 1975b). Some of this research (Toksez et al, 1977;Goins et al, 1976aGoins et al, ,b, 1978b was conducted in conjunction with the work reported in this thesis, but only those aspects directly pertinent to the thesis problem will be discussed in detail.…”

Section: 2 Review Of Previous Workmentioning

confidence: 99%

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Lunar seismology: The internal structure of the Moon

Goins¹,

Dainty²,

Toksöz³

1981

J. Geophys. Res.

147

104

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Tables A1–A4 and Figures A1–A3 are available with entire articleon microfiche. Order from American Geophysical Union, 2000 Florida Avenue, N.W., Washington, D.C. 20009. Document J81‐003;$1.00. Payment must accompany order. The arrival times of direct P and S waves, measured on seismograms recorded from natural lunar seismic events, have been analyzed using linearized inversion and parameter search methods to simultaneously determine event locations, origin times, and structural parameters (seismic velocities). Polarization‐filtered record section plots are correlated with theoretical travel time curves to identify later phases and obtain additional structural and velocity information. Shear wave amplitudes plotted as a function of distance provide data on the existence and magnitude of seismic velocity gradients in the interior. These studies are used to delineate the structure of the moon below the crust to a depth of about 1100 km. This structure has been divided into an upper and a lower mantle. The upper mantle, from 60‐ to 400‐km depth, has average seismic wave velocities of Vp = 7.70 ±0.15 km/s and Vs = 4.45 ± 0.05 km/s with corresponding Q values (taken from the literature) of Qp ∼ 5000 and Qs ∼ 3000. The shear wave velocity decreases with a negative gradient of at most −6 × 10−4 km/s/km, implying a Vs variation of from 4.57 km/s at 60‐km depth to 4.37 km/s at 400‐km depth; this decrease can be accounted for by increasing temperature, and so no major compositional gradient is required in the upper mantle. A small negative P wave velocity gradient may also be present. Between 400‐ and 480‐km depth there is a transition zone with a sharply decreasing shear wave velocity and possibly an accompanying small decrease in Vp. The dominant shear velocity decrease may occur at a 480‐km interface and may represent a compositional change, although the effects of increased temperature cannot be totally ruled out. The lower mantle extends from 480‐km depth to at least 1100‐km depth; few seismic waves recorded by the lunar network penetrate below 1100 km. The average velocities are Vp = 7.6 ± 0.6 km/s and Vs = 4.2 ± 0.1 km/s. Q values (taken from the literature) are Qp ∼ 1500 and Qs ∼ 1000. Below 1100 km there is some indication that the attenuation may increase still further for shear waves, with Qs dropping to a few hundreds or less. This seismic model of the moon is well constrained, with uncertainties on the above values given explicitly by the analysis methods, and so it serves as a strong control on the present‐day lunar compositional and thermal structure.

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Meteoroid Storms Detected on the Moon

Cited by 25 publications

References 5 publications

Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview

Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview

Possible relationship between the Farmington meteorite and a seismically detected swarm of meteoroids impacting the Moon

Lunar seismology: The internal structure of the Moon

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