hchondrites :: Young asteroid families as the primary source of meteorites

Here we present materials from the paper Young asteroid families as the primary source of meteorites by Brož, Vernazza, Marsset et al.

See the submitted paper, published paper, as well as accompanying paper by Marsset et al.! For those in a hurry, we have an 8-minute research summary that was presented at the DPS 2024 meeting.

Major results and implications ↓

H chondrites are from the Koronis2 and Karin families. Spectral classification (S) is compatible. Composition (H) is compatible. Albedo is correct. SFD is steep down-to the observational limit. Corresponding dust band is at 2.1° (Nesvorný et al. 2003). Pre-atmospheric meteorite orbits are close to this source. Both families are young (5.8, 7.6 My, respectively). CRE ages of meteorites are compatible. Cf. H-like NEOs are from Phocaea. LL chondrites are from Flora. LL-like NEOs are also from Flora. Our model matches Nneo(>1 km) as well as Nneo(>1 m). Our model was calibrated on the Vesta family. For a probability of coming from a source, see METEOMOD.

Supplementary animations →

An 8-minute research summary.	Fig. 2 The Koronis2 family is 7.6 My old from convergence of orbits.	Fig. 3 Excess of metre-sized bodies among young families with respect to large but old ones. Karin family. Cf. inverse vers.	Extended Data Fig. 1 Extrapolation of the observed SFD for the Koronis2 family. Cf. inverse vers.	Karin-like collision contributing to the abundance of H chondrites. Volumetric rendering, specific energy. Computed with Opensph.	Ditto for looong time span.	Ditto for particle rendering, |velocity|.	Shape model of (158) Koronis from DAMIT	Ditto for (832) Karin.	NWA 869 meteorite, ordinary chondrite, H5.

Supplementary files ↓

boulder/	Collisional models, initial conditions
main_belt_families_2021Jun/	Family indentification
nbody_backward/	Backward integrations
nbody_metresized/	Transport model, 1-m bodies
nbody_synthetic/	Transport model, 1-km bodies
Fig2.tar.gz	Fig. 2 data
Fig3.tar.gz	Fig. 3 data
FigA1.tar.gz	Extended Data Fig. 1 data
boulder_simplex_CRATERING.tar.gz	Boulder code, Monte-Carlo collisions (Morbidelli et al. 2009)
hcluster4.tar.gz	HCM algorithm
karin1.sph	Project for Opensph (Ševeček et al. 2019)
swift.tar.gz	SWIFT integrator (Levison & Duncan 1994)
swift_bs_f_omega.tar.gz	ditto, for initial conditions
swift_mvs2_fp_ye_YORP_FBR.tar.gz	ditto, for backward integrations
swift_rmvs3_fp_ye_yorp_20220227_GIT.tar.gz	ditto, for forward integrations
swift_rmvs3_fp_ye_YORP_STRENGTHREGIME.tar.gz	ditto, previous vers.
paper2.pdf	paper (submitted vers.)

‘Faint main belt’ figure ↓

Fig. 5 - ‘Faint main belt’, showing only bodies with absolute magnitudes close to the limit of the Catalina Sky Survey. The limit has been adjusted according to the minimum distances from the Sun and the Earth, H ≳ 19.25 + 5(log(2.2(1−0.1)) − log(2.2−1)) − 5(log(a(1−e)) + log(a−1)). For a = 1 au and e = 0.1, H = 19.25 mag. The proper semimajor axis ap versus eccentricity ep (bottom) and versus inclination sin Ip (top) are plotted, together with the locations of the mean-motion resonances (vertical lines), IRAS dust bands (horizontal lines) and some of the asteroid families51 (labels). Big and old asteroids are almost invisible here (for example, Vesta, Flora and Gefion). Small and young asteroids, which have a steep SFD, are prominent. Surprisingly, the distribution of faint bodies is irregular. The concentrations are directly related to the primary sources of meteorites: Massalia (L), Karin and Koronis2 (H), Veritas (CM) and others.