Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.u41a..01l&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #U41A-01
Mathematics
Logic
[5430] Planetary Sciences: Solid Surface Planets / Interiors, [5494] Planetary Sciences: Solid Surface Planets / Instruments And Techniques, [6207] Planetary Sciences: Solar System Objects / Comparative Planetology, [7294] Seismology / Seismic Instruments And Networks
Scientific paper
On planetary bodies without atmosphere (e.g. the Moon, Jovian satellites, small bodies) or a planet with a weak atmosphere such as Mars, impacts of meteoroids are high potential seismic sources. During the Apollo seismic experiment on the Moon, impacts related seismic events were used to constrain the crustal structure, including estimates of lateral variations. (Chenet et al, EPSL, 2006) Moreover, the location and time of present-day lunar surface impacts with masses larger than about 1 kg can now be determined, as impacts generate light flashes observed from Earth with modest telescopes. The location of larger impacts (> 100 kg) can also be detected by High Resolution Optical Orbital cameras. As soon as they are located by these non-seismic methods, impacts become the only seismic sources that can be used by a single seismic station on a planet for inverting the interior structure. We review and present in this paper the main characteristics of the seismic source generated by an impact, in both amplitude and cutoff frequency, and compare these signals to shallow moonquakes as detected by Apollo. We focus on the largest impacts on the Moon, and show that they have a relatively low frequency cutoff frequency (< 1 Hz) associated with the shock wave generated during the impact. Both this cutoff frequency and the amplitude of the seismic wave allow us to constrain the mass and velocity of the impactor (Gudkova et al, Icarus, 2010, Kawamura et al, 2010). We then present mass-frequency models of impacts on the Moon from Apollo observations, and extrapolate these models to other planets and planetary bodies (Mars, Jovian satellites and small bodies). This allow us to constrain not only the expected amplitude of the micro-seismic noise associated with continuous impacts on airless planets (called the meteoritic hum, Lognonné et al, 2009) but also the expected detection frequency of impacts on future seismological missions, such as Moon missions (e.g. SELENE2, ILN, Lunette) or Mars missions (e.g. GEMS, NF or MarsNext). By using statistical simulation, the expected resolution in the seismic velocities models resulting from these future missions can be computed, and we illustrate this for the Moon (Yamada et al., 2010). We finally present and discuss new or exotic challenges such as impact seismology on small bodies or in-situ detection of the electromagnetic signals associated with impacts.
Blitz Céline
Gagnepain-Beyneix Jeannine
Garcia Raphaël F.
Gudkova T.
Johnson Clifton L.
No associations
LandOfFree
Impact seismology on terrestrial planets and Small bodies (Invited) does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Impact seismology on terrestrial planets and Small bodies (Invited), we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Impact seismology on terrestrial planets and Small bodies (Invited) will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1500280