Simulation of the capabilities of an orbiter for monitoring the entry of interplanetary matter into the terrestrial atmosphere

Bouquet, Alexis; Baratoux, D.; Vaubaillon, Jérémie; Gritsevich, Maria; Mimoun, David; Mousis, O.; Bouley, Sylvain

doi:10.1016/j.pss.2014.09.001

Cited by 42 publications

(42 citation statements)

References 27 publications

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“…There are various parameters that control the possibility to recover meteorite fragments, including impact velocity, impact angle, fragmentation in the atmosphere, and size of individual fragments, atmospheric entry of already fragmented material (e.g., Gritsevich and Koschny ; Bouquet et al. ), and subsequent weathering. In addition, meteorite fragments may be preserved within impact melt, as in the exceptional case of Morokweng (Maier et al.…”

Section: Discussionmentioning

confidence: 99%

“…In most impact events, and especially in large ones, the projectile is entirely melted and/or vaporized (Pierazzo and Melosh 2000) and it is generally not possible to find bolide fragments associated with impact structures. There are various parameters that control the possibility to recover meteorite fragments, including impact velocity, impact angle, fragmentation in the atmosphere, and size of individual fragments, atmospheric entry of already fragmented material (e.g., Gritsevich and Koschny 2011;Bouquet et al 2014), and subsequent weathering. In addition, meteorite fragments may be preserved within impact melt, as in the exceptional case of Morokweng (Maier et al 2006;Jourdan et al 2010).…”

Section: Coincidental Association Of Shatter Cones With Meteoritesmentioning

confidence: 99%

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The Agoudal (High Atlas Mountains, Morocco) shatter cone conundrum: A recent meteorite fall onto the remnant of an impact site

Aoudjehane

Kerni

Reimold

et al. 2016

Meteorit & Planetary Scien

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Associations between impact structures and meteorite occurrences are rare and restricted to very young structures. Meteorite fragments are often disrupted in the atmosphere, and in most cases, meteorite falls that have been decelerated by atmospheric drag do not form a crater. Furthermore, meteorites are rapidly weathered. In this context, the finding of shatter cones in Jurassic marly limestone in the same location as a recent (105 ± 40 ka) iron meteorite fall near the village of Agoudal (High Atlas Mountains, Morocco) is enigmatic. The shatter cones are the only piece of evidence of a meteorite impact in the area. The overlap of a meteorite strewn field with the area of occurrence of shatter cones led previous researchers to consider that the meteorite fall was responsible for the formation of shatter cones in the context of formation of one or several small (<100 m) impact craters that had since been eroded. Shatter cones are generally not reported in association with subkilometer‐diameter impact craters. Here, we present new field observations and an analysis of the distribution and characteristics of shatter cones, breccia, and meteorites in the Agoudal area. Evidence for local deformation not related to the structural High Atlas tectonics has been observed, such as a vertical to overturned stratum trending N150‐N160. New outcrops with exposures of shatter cones are reported and extend the previously known area of occurrence. The area of in situ shatter cones (~0.15 km2) and the strewn field of meteorites are distinct, although they show some overlap. The alleged impact breccia is revealed as calcrete formations. No evidence for a genetic relationship between the shatter cones and the meteorites can be inferred from field observations. The extent of the area where in situ shatter cones and macrodeformation not corresponding to Atlas tectonic deformation are observed suggest that the original diameter of an impact structure could have been between at least 1–3 km. For typical erosion rates in the Atlas region (~0.08 cm yr−1), the period of time required for the erosion of such a structure (1.25–3.75 Ma) is much larger than the age of the meteorite fall. This line of reasoning excludes a genetic link between the shatter cones and the meteorite fall and indicates that the observed shatter cones belong to an ancient impact structure that has been almost entirely eroded.

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Section: Discussionmentioning

confidence: 99%

Section: Coincidental Association Of Shatter Cones With Meteoritesmentioning

confidence: 99%

The Agoudal (High Atlas Mountains, Morocco) shatter cone conundrum: A recent meteorite fall onto the remnant of an impact site

Aoudjehane

Kerni

Reimold

et al. 2016

Meteorit & Planetary Scien

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“…As previously stated, if we were to assume values for, say, density and shape in Equation 2, it is possible to then calculate the entry mass of a meteoroid using α. Further assuming the shape change coefficient of the body can give a final mass using the β value and Equation 3 (with luminosity values, µ can be determined following Bouquet et al, 2014). Here we plot a series of bounding curves for a given set of assumptions on the α-β diagram.…”

Section: Determining the Meteorite Fall Regionmentioning

confidence: 99%

“…The significant area between these two curves illustrates the sensitivity of the dynamic flight equations to meteoroid rotation. As a subsequent step, the shape change coefficient can be calculated for individual events from luminosity values following Bouquet et al (2014).…”

Section: Determining the Meteorite Fall Regionmentioning

confidence: 99%

Determining Fireball Fates Using the α–β Criterion

Sansom

Gritsevich

Devillepoix

et al. 2019

ApJ

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As fireball networks grow, the number of events observed becomes unfeasible to manage by manual efforts. Reducing and analysing big data requires automated data pipelines. Triangulation of a fireball trajectory can swiftly provide information on positions and, with timing information, velocities. However, extending this pipeline to determine the terminal mass estimate of a meteoroid is a complex next step. Established methods typically require assumptions to be made of the physical meteoroid characteristics (such as shape and bulk density). To determine which meteoroids may have survived entry there are empirical criteria that use a fireball's final height and velocity -low and slow final parameters are likely the best candidates. We review the more elegant approach of the dimensionless coefficient method. Two parameters, α (ballistic coefficient) and β (mass-loss), can be calculated for any event with some degree of deceleration, given only velocity and height information. α and β can be used to analytically describe a trajectory with the advantage that they are not mere fitting coefficients; they also represent the physical meteoroid properties. This approach can be applied to any fireball network as an initial identification of key events and determine on which to concentrate resources for more in depth analyses. We used a set of 278 events observed by the Desert Fireball Network to show how visualisation in an α -β diagram can quickly identify which fireballs are likely meteorite candidates.

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“…Recently, there has been a worldwide proliferation of instruments and networks dedicated to observing meteors, including international airborne campaigns (Vaubaillon, J. et al, 2015) and possible future space-based monitoring systems (Bouquet A., et al, 2014). There has been a corresponding rapid rise in high quality data accumulating annually.…”

Section: Introductionmentioning

confidence: 99%

Orbit determination based on meteor observations using numerical integration of equations of motion

Dmitriev

Lupovka

Gritsevich

2015

Planetary and Space Science

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Orbit determination based on meteor observations using numerical integration of equations of motion Dmitriev, Vasily Dmitriev , V , Lupovka , V & Gritsevich , M 2015 , ' Orbit determination based on meteor observations using numerical integration of equations of motion ' , Planetary and Space Science , vol. 117 , AbstractRecently, there has been a worldwide proliferation of instruments and networks dedicated to observing meteors, including international airborne campaigns (Vaubaillon, J. et al., 2015) and possible future space-based monitoring systems (Bouquet A., et al., 2014). There has been a corresponding rapid rise in high quality data accumulating annually. In this paper, we present a method embodied in a software program, which can effectively and accurately process these data in an automated mode and discover the pre-impact orbit and possibly the origin or parent body of a meteoroid or asteroid. The required input parameters are the topocentric pre-atmospheric velocity vector and the coordinates of the atmospheric entry point of the meteoroid, i.e. the beginning point of visual path of a meteor, in the an Earth centered-Earth fixed coordinate system, the International Terrestrial Reference Frame (ITRF). Our method is based on strict coordinate transformation from the ITRF to an inertial reference frame and on numerical integration of the equations of motion for a perturbed two-body problem. Basic accelerations perturbing a meteoroid's orbit and their influence on the orbital elements are also studied and demonstrated. Our method is then compared with several published studies that utilized variations of a traditional analytical technique, the zenith attraction method, which corrects for the direction of the meteor's trajectory and its apparent velocity due to Earth's gravity. We then demonstrate the proposed technique on new observational data obtained from the Finnish Fireball Network (FFN) as well as on simulated data. In addition, we propose a method of analysis of error propagation, based on general rule of covariance transformation.

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Simulation of the capabilities of an orbiter for monitoring the entry of interplanetary matter into the terrestrial atmosphere

Cited by 42 publications

References 27 publications

The Agoudal (High Atlas Mountains, Morocco) shatter cone conundrum: A recent meteorite fall onto the remnant of an impact site

The Agoudal (High Atlas Mountains, Morocco) shatter cone conundrum: A recent meteorite fall onto the remnant of an impact site

Determining Fireball Fates Using the α–β Criterion

Orbit determination based on meteor observations using numerical integration of equations of motion

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