Sources of less common meteorite type

According to recent publications (Marsset et al. 2024, Nature 634, 561; Brož et al. 2024, Nature 634, 566; Brož et al. 2024, A&A 689, A183), the primary sources of meteorites are young asteroid families. However, an open question remains as to what constitutes the sources of less common meteorite types (enstatite chondrites of types EL, EH, R chondrites, pallasites, and iron meteorites of types IAB, IIIAB, …). In the case of iron meteorites, the problem is particularly challenging, because their cosmic exposure ages are long (∼1, Gy; Smith et al. 2011, Meteorit. Planet. Sci. 54, 2951), which suggests that their parent bodies should be old asteroid families. Understanding the iron meteorites is essential, since radiometric dating indicates that they are the oldest differentiated meteorites, formed between 4.567 and 4.566 billion years ago (Kruijer et al. 2017, PNAS 114, 26), and thus represent remnants of the first generation of planetesimals. A related topic is being addressed within the GAČR grant (25–16789S; PI J. Hanuš).

To solve the problem, a multidisciplinary approach is required, which includes: identification of asteroid families (Nesvorný et al. 2015, in Asteroids III), simulation of their orbital evolution (Brož et al. 2011, MNRAS 414, 2716), simulation of their collisional evolution (Morbidelli et al. 2009, Icarus 204, 558), determination of their ages, transport into near-Earth space, determination of the collision probability with Earth and of the flux, comparison with meteorite statistics [1], comparison with the orbits of near-Earth objects (NEOs; Marsset et al. 2022, AJ 163, 165), comparison with pre-atmospheric orbits (Borovička et al. 2022, A&A 667, A158). Preliminarily selected candidates are M-type families associated with the asteroids: (22) Kalliope (Ferrais et al. 2022, A&A 662, A71; Brož et al. 2022, A&A 664, A69; Brož et al. 2023, A&A 676, A60), (135) Hertha, or (283) Brasilia [2]. In describing them, it is necessary to take into account the different strengths of iron and rocky materials, which influence the progress of the collisional cascade.

In parallel, it is necessary to study alternative models, where irons survive as small fragments from the first-generation of planetesimals, including discussion of the missing mantle material (olivine; Vazi et al. 2021, Nat. Comm. 12, 5443), where irons were implanted from the terrestrial zone during orbital instability (Avdellidou et al. 2024, Science 384, 348), or where irons formed along the Fe condensation line (Woitke et al. 2018, A&A 614, A1).

The student should have knowledge of the Linux operating system, programming in Fortran or C, programming in Python, the ability to study related subfields (celestial mechanics, meteorite chemistry), analytical skills, the ability to work independently as well as collaboratively with international experts (P. Vernazza, M. Marsset, A. Morbidelli, D. Nesvorný).

https://sirrah.troja.mff.cuni.cz/~mira/tmp/PhD_meteority/README_cz.pdf

References:

Marsset et al. 2024, Nature 634, 561.
Brož et al. 2024, Nature 634, 566.
Brož et al. 2024, A&A 689, A183.
Avdellidou et al. 2024, Science 384, 348.
Bischoff et al. 2011, Chemie der Erde, 101.
Borovička et al. 2022, A&A 667, A158.
Brož et al. 2011, MNRAS 414, 2716.
Brož et al. 2022, A&A 664, A69.
Brož et al. 2023, A&A 676, A60.
Eugster et al. 2006, in Meteorites and the Early Solar System II.
Ferrais et al. 2022, A&A 662, A71.
Kruijer et al. 2017, PNAS 114, 26.
Marsset et al. 2022, AJ 163, 165.
Morbidelli et al. 2009, Icarus 204, 558.
Nesvorný et al. 2015, in Asteroids III.
Patzer & Schultz 2011, Meteorit. Planet. Sci. 36, 947.
Smith et al. 2019, Meteorit. Planet. Sci. 54, 2951.
Swindle et al. 2014, Geol. Soc. London Spec. Publ. 378, 333.
Trieloff et al. 2022, Icarus 373, 114762.
Vazi et al. 2021, Nat. Comm. 12, 5443.
Woitke et al. 2018, A&A 614, A1.

[1] Meteoritics Bulletin Database, https://www.lpi.usra.edu/meteor/
[2] Asteroid (283) je typu C, ale jde o rodinu typu M poblíž