A case study of the May 30, 2017, Italian fireball

Carbognani, A.; Barghini, D.; Gardiol, D.; Martino, M. Di; Valsecchi, G. B.; Trivero, P.; Buzzoni, A.; Rasetti, S.; Selvestrel, Danilo; Knapic, C.; Londero, E.; Zorba, Sonia; Volpicelli, C. A.; Carlo, Matteo Di; Vaubaillon, Jérémie; Marmo, C.; Colas, François; Valeri, Diego; Zanotti, Ferruccio; Morini, Marco; Demaria, P.; Zanda, B.; Bouley, Sylvain; Vernazza, Pierre; Gattacceca, J.; Rault, Jean-Louis; Maquet, Lucie; Birlan, Mirel

doi:10.1140/epjp/s13360-020-00254-6

Cited by 7 publications

(8 citation statements)

References 21 publications

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“…We used the method outlined in Carbognani et al (2020) to estimate the fireball atmospheric trajectory, its main physical parameters, and the best kinematic parameters in the terminal point of the luminous path. The atmospheric trajectory computation is performed according to the classical formulation reported in Ceplecha (1987) and Borovička (1990).…”

Section: Fireball Data Analysismentioning

confidence: 99%

“…7, has moderate eccentricity and low inclination on the Ecliptic, with a Tisserand invariant with respect to Jupiter equal to 4.1 ± 0.2, thus indicating that the progenitor meteoroid was of asteroidal origin. To find possible progenitor(s) of the Cavezzo meteorite, we followed the procedure described in Carbognani et al (2020), using the orbital similarity criterion D N introduced by Valsecchi et al (1999); the NEODyS database 10 conveniently lists the secular quantities used in D N for all Near-Earth Asteroids (NEAs) for which they are defined (Gronchi & Milani 2001). We use D N in the form:…”

Section: A Possible Progenitor Of the Cavezzo Meteoritementioning

confidence: 99%

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Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Gardiol

Barghini

Buzzoni

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 4th January 2020. The associated fireball was observed on the evening of New Year’s Day 2020 by eight all-sky cameras of the PRISMA fireball network, a partner of FRIPON. The computed trajectory had an inclination angle of approximately 68○ and a velocity at infinity of 12.8 km s−1. Together with the relatively low terminal height, estimated as 21.5 km, those values were indicating the significant possibility of a meteorite dropping event, as additionally confirmed by the non zero residual total mass. The strewn-field was computed taking into account the presence of two bright light flashes, revealing that the meteoroid had been very likely subject to fragmentation. Three days after the event, two samples, weighing 3.1 g and 52.2 g, were collected as a result of a dedicated field search and thanks to the involvement of the local people. The two pieces were immediately recognised as freshly fallen fragments of meteorite. The computed orbital elements, compared with the ones of known Near-Earth Asteroids from the NEODyS database, are compatible with one asteroid only; 2013 VC10. The estimated original mass of the meteoroid, 3.5 kg, and size, approximately 13 cm, is so far the smallest among the current 35 cases in which meteorites were recovered from precise strewn-field computation thanks to observational data. This result demonstrates the effectiveness of accurate processing of fireball network data even on challenging events generated by small size meteoroids.

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Section: Fireball Data Analysismentioning

confidence: 99%

Section: A Possible Progenitor Of the Cavezzo Meteoritementioning

confidence: 99%

Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Gardiol

Barghini

Buzzoni

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Based on the reported observations of meteors (Jeanne et al 2019;Gardiol et al 2021;Carbognani et al 2020), 80 km is the typical altitude at which a meteor begins to be observed, and it disappears around an altitude of 20 km as it comes apart in the atmosphere. The observation site is assumed at sea level, under the SCTP and with an observation wavelength λ 0 .…”

Section: Meteor Trajectographymentioning

confidence: 99%

Computation of the lateral shift due to atmospheric refraction

Labriji

Herscovici-Schiller

Cassaing

2022

A&A

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Context. Atmospheric refraction modifies the apparent position of objects in the sky. As a complement to the well-known angular offset, we computed the lateral translation that is to be considered for short-range applications, such as wavefront sensing and meteor trajectories. Aims. We aim to calculate the lateral shift at each altitude and study its variation according to meteorological conditions and the location of the observation site. We also pay special attention to the chromatism of this lateral shift. Moreover, we assess the relevance of the expressions present in the literature, which have been established neglecting Earth's curvature. Methods. We extracted the variation equations of refraction from the geometric tracing of a light ray path. A numerical method and a dry atmosphere model allowed us to numerically integrate the system of coupled equations. In addition to this, based on Taylor expansions, we established three analytic approximations of the lateral shift, one of which is the one already known in the literature. We compared the three approximations to the numerical solution. All these estimators are included in a Python 3.2 package, which is available online. Results. Using the numerical integration estimator, we calculated the lateral shift values for any zenith angle including low elevations. The shift is typically around 3 m at a zenith angle of 45 • , 10 m at 65 • , and even 300 m at 85 • . Next, the study of the variability of the lateral shift as a function of wavelength shows differences of up to 2% between the visible and near infrared. Furthermore, we show that the flat Earth approximation of the lateral shift corresponds to its first-order Taylor expansion. The analysis of the errors of each approximation shows the ranges of validity of the three estimators as a function of the zenith angle. The 'flat Earth' estimator achieves a relative error of less than 1% up to 55 • , while the new extended second-order estimators improves this result up to 75 • . Conclusions. The flat Earth estimator is sufficient for applications where the zenith angle is below 55 • (most high-resolution applications) but a refined estimator is necessary to estimate meteor trajectories at low elevations.

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“…2019; Carbognani et al. 2020). Other networks exist around the world—starting with the historic imaging and subsequent recovery of the Příbram meteorite in 1959 (Ceplecha 1961)—all of them working with substantially the same goals as PRISMA, that is, the detection of fireballs and when possible the recovery of associated meteorites.…”

Section: Introductionmentioning

confidence: 99%

Cavezzo—The double face of a meteorite: Mineralogy, petrography, and geochemistry of a very unusual chondrite

Pratesi

Cecchi

Greenwood

et al. 2021

Meteorit & Planetary Scien

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The Cavezzo meteorite, which fell on January 1, 2020, is the first meteorite detected and recovered by the Italian PRISMA Fireball Network. Two specimens, weighing 3.12 g (specimen 1) and 52.19 g (specimen 2), were collected 3 days after the bolide was observed, thanks to an effective media campaign that encouraged the involvement of local people. The two specimens of this meteorite have not only completely different lithological characteristics but also a different geochemistry and oxygen isotopic composition as well. Specimen 1 is anomalous both for the textural–structural features, varying seamlessly from chondritic to “achondritic,” and a very unusual modal mineralogy—such as the relatively high amount of olivine (63.1 vol%), plagioclase (18.2 vol%), high‐Ca pyroxene (10.3 vol%), and chlorapatite (2.1 vol%); and the unusually low content of low‐Ca pyroxene (5.8 vol%), metal (0.1 vol%), and troilite (much lesser than 0.1 vol%)—although the compositional values for olivine (Fa 24.24 mol%) and low‐Ca pyroxene (Fs 20.41 mol%) appear to be similar to those of the L chondrite group. Conversely, in specimen 2, not only the texture and the crystal chemistry but also the modal mineralogy (low‐Ca pyroxene much more abundant than high‐Ca pyroxene and occurrence of metal and sulfides) look like those of an ordinary L chondrite. The differences between the two specimens are also confirmed by geochemistry. The oxygen isotope composition of specimen 1 plots at the boundary between the H and L groups (δ17O‰ 3.250; δ18O‰ 4.736; Δ17O‰ 0.788) whereas specimen 2 plots at the boundary of the L and LL fields (δ17O‰ 3.737; δ18O‰ 4.957; Δ17O‰ 1.159). The bulk chemistry shows a different content of many minor and trace elements (including rare earth elements), such as a strong depletion of siderophile and chalcophile elements in specimen 1. The two specimens then do not contain fragments of each other, thus preventing us from classifying this “double face” meteorite as an ordinary chondrite breccia. In detail, specimen 1 can be considered a “xenolith” in which chondritic structure and igneous texture coexist without discontinuity, and therefore, it represents a previously unsampled portion of the L parent body. In summary, these findings support the classification of Cavezzo as an L5 anomalous chondrite.

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A case study of the May 30, 2017, Italian fireball

Cited by 7 publications

References 21 publications

Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Computation of the lateral shift due to atmospheric refraction

Cavezzo—The double face of a meteorite: Mineralogy, petrography, and geochemistry of a very unusual chondrite

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