Next Article in Journal
Testing Screening Mechanisms with Mass Profiles of Galaxy Clusters
Next Article in Special Issue
The NuGrid AGB Evolution and Nucleosynthesis Data Set
Previous Article in Journal
Hidden Conformal Symmetry in Higher Derivative Dynamics for the Kerr Black Hole
Previous Article in Special Issue
Recent Achievements of the ERNA Collaboration
 
 
Search for Articles:
Title / Keyword
Author / Affiliation / Email
Journal
Article Type
 
 
Advanced Search
 
Section
Special Issue
Volume
Issue
Number
Page
 
Journals
Universe
Volume 8
Issue 3
10.3390/universe8030156
universe-logo
Submit to this Journal Review for this Journal Propose a Special Issue
► Article Menu

Article Menu

share Share announcement Help format_quote Cite question_answer Discuss in SciProfiles thumb_up
...
Endorse textsms
...
Comment
first_page
settings
Order Article Reprints
Font Type:
Arial Georgia Verdana
Font Size:
Aa Aa Aa
Line Spacing:
Column Width:
Background:
Article

The Achievements of the RockStar Group (Perugia) on Astrophysical Modelling and Pallasite Geochemistry

by
Lisa Ricci
1,2,*,
Maurizio Petrelli
1,2,*,
Francesco Frondini
1,2,
Azzurra Zucchini
1,2,
Paola Comodi
1,
Andrea Bisciotti
2,3,
Diego Vescovi
4 and
Oscar Trippella
1,2
1
Dipartimento di Fisica e Geologia, Università degli Studi di Perugia, Via Pascoli, 06123 Perugia, Italy
2
INFN Sezione di Perugia, Via Pascoli, 06123 Perugia, Italy
3
Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara, Via Sagarat 1/C, 44122 Ferrara, Italy
4
Department of Physics, Goethe University Frankfurt, Max-von-Laue-Strasse 1, 60438 Frankfurt am Main, Germany
*
Authors to whom correspondence should be addressed.
Universe 2022, 8(3), 156; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8030156
Submission received: 10 December 2021 / Revised: 7 February 2022 / Accepted: 22 February 2022 / Published: 28 February 2022
(This article belongs to the Special Issue AGB Stars—In Honor of Professor Maurizio Busso on the Occasion of His 70th Birthday)
Browse Figures
Versions Notes

Abstract

:
In the present work we summarize the first achievements of the RockStar Group of the Department of Physics and Geology (at the University of Perugia, Italy), which is made of a strict collaboration between Physicists and Geologists on astrophysical and planetological studies. The RockStar Group acts on two research lines: (i) astrophysical modeling and (ii) mineralogical and geochemical studies of meteorites. In the first part of the article we review the recent results concerning the development of theoretical modeling of nucleosynthesis and mixing process in asymptotic giant branch. In the second part we report (1) the catalog of the Meteorite collection of University of Perugia and (2) major and trace elements mapping, performed through EPMA and LA-ICP-MS, of the Mineo pallasite, a unique sample hosted by the collection. The new data constrain the Mineo meteorite among the Main Group Pallasites and support the hypothesis of the “early giant impact” formation.

1. Introduction

Coupling the expertise from different scientific fields is nowadays mandatory to achieve new milestones, add knowledge and validate models. Astrophysical modeling takes significant advantage of geochemical investigations on meteorites [1,2,3], since they store, like a coffer, information about the early Solar System and its evolution [4,5]. Moreover, geochemical and structural investigations in minerals, crystals, and quasi-crystals can provide the basis for modeling the formation and the physical evolution of meteorites and planetary bodies [6,7,8,9,10].
In order to face cross-disciplines topics on astrophysical and planetological studies, a strict collaboration between Physicists and Geologists of the Department of Physics and Geology of the University of Perugia (Italy) has been set up naming this informal group RockStar Group.
In the present manuscript, we describe main activities and results of the RockStar Group, both in astrophysical modelling and meteorite classification, with particular focus on new geochemical data of the Mineo pallasite, a unique sample re-discovered during the initial stages of RockStar Group activities.

2. Roadmap of the RockStar Group

The RockStar Group started its activities in 2014, a few months after the founding of the Department of Physics and Geology of the University of Perugia (Italy) in 2013, when the previous Physics and Earth Sciences Departments merged, joining their well-established scientific traditions. The group has been initiated by Maurizio Busso (University of Perugia) and it has beneficiated by Maurizio’s mentorship for the first seven years. The first two years of activity have been directly funded by the University of Perugia, then the activities of the RockStar Group continued within the INFN (National Institute of Nuclear Physics) project named ERNA2.
The activities of the RockStar Group are mainly focused on two research topics: (i) the development of theoretical modeling of nucleosynthesis and mixing processes in asymptotic giant branch (AGB) and (ii) the classification and the mineralogical-geochemical study of meteorites.

3. Using Geochemical Data to Constraint Astrophysical Modeling

Astronomers have traditionally studied the stars through the inspection of their electromagnetic radiation emissions. However, since the mid-1980s, the analysis of primordial meteorites and presolar grains therein contained has paved the way for a new approach to studying the stars. These grains can be recovered within undifferentiated meteorites after chemical and physical separation from the hosting material [11] and preserve the chemical and isotopic composition of the stellar environments where they condensed, thus providing robust constraints on theoretical models of nucleosynthesis (see, e.g., [12]).
The isotopic compositions of presolar grains are determined in laboratories all over the world, e.g., [13,14,15,16,17]. A convenient source for accessing the data for a wide range of isotopic compositions and grain types is the “Presolar Grain Database” (PGD) maintained by the Department of Physics of Washington University in St. Louis [18,19]. It is a collection of spreadsheets containing the isotope data on presolar grains (SiC, Graphite, Oxides, and Silicates; [18,19]). As an example, the PGD for Mainstream SiC contains ~20,000 isotopic ratio measurements for Si and C, mainly determined by Nanoscale Secondary Ion Mass Spectrometry (NanoSims, e.g., [17]), and a few identifications of trace heavy elements, analyzed by Resonance Ionization Mass Spectrometry (RIMS, e.g., [20,21]). The majority of those grains (>90%), known as mainstream (MS) SiC grains, have been shown to provide crucial knowledge about the nucleosynthesis of the progenitor stars with higher accuracy (≲10%) than direct stellar observations (typically about a factor of two). Their typical C, N, and Si isotope ratios, as well as evidence of s-elements, i.e., elements heavier than iron made through the slow (s) neutron capture process (e.g., [22]) detected in a selection of them, indicate that they originated in asymptotic giant branch (AGB) stars (see [23] for a review). In this respect, theoretical modeling of nucleosynthesis and mixing processes in AGB stars can be empirically constrained using presolar MS SiC grains data (e.g., [24,25,26,27,28]).
A fundamental aspect of the RockStar project concerns providing the necessary theoretical support to future meteoritic analyses. In this regard, great attention has been paid to developing state-of-the-art nucleosynthesis models of low-mass (M < 3 M⊙) AGB stars. Since the seminal work of Busso et al. (2007) [29], the nuclear astrophysics group of Perugia has been deeply involved in theorizing a new paradigm in which the process occurring in those stars is driven by magnetohydrodynamic (MHD) phenomena [30]. Such efforts have recently culminated in a series of works showing that the proposed MHD scenario for the formation of the main neutron source in AGB stars, the so-called 13C pocket, can account for several observational constraints (e.g., [27]) and, in particular, for the isotopic abundance ratios of s-elements in presolar MS SiC grains of stellar origin [3,26,28].
Previous comparisons of s-process computations with isotopic ratios of s-elements in individual presolar SiC grains showed that the latter can be safely used to constrain the extension and the shape of the 13C pocket [24], but not the stellar metallicities of their parent AGB stars [25]. In this regard, the Si content of MS grains suggests that their progenitor star had either near-solar or slightly super-solar metallicity [31,32]; whereas, integrated approaches combining chemical and chemodynamical models of the Galaxy with dust yields from AGB models, revealed that the majority of presolar SiC grains come from AGB stars with M ~ 2 M⊙ and close-to-solar metallicity [33,34]. In Figure 1, we compare the latest Perugia model predictions [28] with available laboratory measurements of selected isotopic ratios for Sr, Zr, and Ba in presolar SiC grains. For the aforementioned reasons, the comparison is restricted to stellar models of 2 M⊙ and with metallicity [Fe/H] 1 between −0.15 and +0.1. In general, model predictions and grain data match fairly well, with the former reproducing almost all of the data spread. Thus, the proposed MHD-induced mechanism for driving mixing and neutron-capture processes in AGB stars offers a solid astrophysical interpretation for available s-elements isotopic ratios in presolar SiC grains from those stars.
Nonetheless, since the multielement and multi-isotope composition is known only for a small subset of the available meteoritic samples, the comparison is somewhat limited. For example, the PGD reports 18 samples where Ba and Zr isotopes are both determined. On the one hand, the Rockstar project aims to perform new SiC grain measurements to study the correlation between those particular isotope ratios that are, at present, poorly constrained and to test theoretical predictions against them. On the other hand, it also points toward understanding the cosmic origin of different classes of meteorites, containing metal-silicate aggregates of various species, as carbonaceous chondrites and pallasites (see Section 5).

4. The Meteorite Collection at the Department of Physics and Geology in Perugia and the Discovery of a Unique Sample

The second research line is the mineralogical and geochemical study of the meteorites available in the collection of the Department of Physics and Geology of Perugia University (Italy). The main goal of this activity is the classification of the samples, formerly classified according to the traditional scheme (stony meteorites, iron meteorites and stony irons), according to the recent classification scheme based on their degree of differentiation [35].
The Meteorite collection of University of Perugia was instituted in 1964 by the Italian Center for Meteorite Studies, in the Mineralogical Institute of University of Perugia (Italy). The collection started with only five samples, but the number of specimens rapidly increased reaching a total of 30 hand-size samples and numerous thin sections in December 1969, when the Mineralogical Institute of University of Perugia (Italy) published a catalog of the collection [36]. The catalog contains the list of samples and the picture, description and references of each sample (Figure 2).
During the following years, the collection has been enriched with several new specimens, but the original catalog has never been updated until 2014, when the Department of Physics and Geology of University of Perugia (Italy) started updating the catalog.
Nowadays, the collection hosts a total of 49 specimens of meteorites, including 29 chondrites, 11 achondrites, 6 primitive achondrites and 3 iron meteorite specimens not attributable to a single category due to the lack of information (Table A1). Furthermore, the collection includes numerous tektites, impactites, and metallic spherules.
On the total of available chondrite, 26 are ordinary. Among the ordinary chondrites, 11 belong to the H type, 13 are L-type chondrites and the remaining ones are of LL and L/LL type. Also, the collection stores 3 samples of world-famous carbonaceous chondrites: two samples of Allende and one of Vigarano [37,38].
During the update of the catalog in 2014, we discovered a piece of the rare Mineo pallasite. In detail, the Mineo pallasite was acquired by the Department of Earth Sciences of University of Perugia (Italy) in 1965 and it was roughly described by Baldanza (1965) [39] and Nagata (1979) [40]. At the present, the sample hosted by University of Perugia (Italy) is the only known sample available in public collections [41]. This sample deserve further studies since: (a) is one of only the two collected in Italy; (b) it is still poorly investigated.
In detail, we aim to provide new mineralogical and geochemical data of some poorly studied meteorites in order to infer some hypothesis about their origin. Within this framework, the main results concerned the Mineo pallasite, a rare pallasite whose only sample available in public collection is hosted by University of Perugia. This pallasite was never studied before 2018, when Zucchini et al. (2018) [41] reported a detailed description of the mineralogical features and some geochemical data of the specimen stored at the University of Perugia (Italy). After this first study, new geochemical data have been collected in the following years and will be presented in this article.

5. The Mineo Pallasite: A Unique Sample

Pallasites are stony-iron meteorites composed of silicate mineral phases, i.e., olivine always present and, in some cases, pyroxene, hosted in a metallic (Fe, Ni) groundmass [35,42]. Their origin is still debated with hypotheses ranging from the “early giant impact” proposed by Yang et al. (2010) [43] to the result of ferrovolcanic eruptions [44]. In the first scenario, Main Group (MG) pallasites would have been formed from an impact that mixed residual Ir-poor molten metallic Fe-Ni from the outermost part of a IIIAB-like core with olivine mantle fragment [44]. If the pallasite formation was related to ferromagmatism, as suggested by Johnson et al. 2019 [44], then pallasites may be intrusions of evolved core magmas into an olivine-rich mantle body [44].
The classification of Pallasites defines four different groups: (1) the Main Group pallasites (PMG), (2) the Eagle Station grouplet (ES), (3) pyroxene pallasites, and (4) the Milton ungrouped pallasite [35].
The Mineo pallasite is one of only the two collected in Italy [41] and belongs to the only four witnessed pallasite falls worldwide [45]. The Mineo fall occurred on 3 May 1826, when a bright meteor was observed over Sicily and a fall occurred near the town of Mineo [41]. To our knowledge, the sole portion (i.e., 42 g) of the Mineo meteorite that is of public access, belongs to the Department of Physics and Geology of University of Perugia (Italy).
Despite its uniqueness, the Mineo pallasite was not extensively studied before 2018, when Zucchini et al. (2018) [41] reported a detailed description of the mineralogical features and some geochemical data of the Mineo sample stored at the University of Perugia (Italy).
Zucchini et al. (2018) [41] observed an olivine-metallic portion of 65–35% by volume, respectively. The olivine composition is in the range Fo88-Fo84, and the metal phase is essentially composed of iron (Ni abundance of 5 ± 1 wt%, on average), taenite (Ni of ~20 wt%), barringerite, and schreibersite. Trace element chemical composition of the Mineo (Fe, Ni) metal shows enrichments in Ir, Re, and Os [41]. The distribution of the platinum group elements follows the same qualitative behavior of the IIIAB iron meteorites, which formed during the later fractional crystallization stages [41,46]. This evidence agrees with the well-documented link between pallasites and fractionated IIIAB irons [46]. In the Ga-Ge diagram (Figure 3), often used to discriminate between Eagle Station (ES) and Main Group (MG) pallasites [47], the Mineo pallasite plots in the MG field. As a consequence, the results reported by Zucchini et al. (2018) [41] allowed a preliminary classification of the Mineo meteorite to the PMG. Note that the olivine phase shows a compositional variability in terms of Fe and trace elements, to an extent that is known from only one other pallasite, Glorieta Mountain [41]. According to Zucchini et al. (2018) [41], most of the features observed in the Mineo pallasite are consistent with the “early giant impact”, theory proposed by Yang et al. (2010) [43]. Alternatively, the observed variations in olivine compositions might also derive from the crystallization in two differentiated parent bodies [41] or be the result of ferrovolcanic eruptions [44]. However, these hypotheses need to be verified by further analyses, such as the isotopic composition of the olivines, to discriminate their origin either from one or more parent bodies [41].
Besides the mechanism of pallasite formation, several studies focused on the origin of olivines and two main alternative hypotheses were proposed [48,49,50,51]. One possible origin is that they are cumulates from an originally molten asteroid and a second possibility is that they have a restitic origin. A third possibility is that they are cumulus grains plus a trapped melt component, but the modal pyroxene content is generally too low to support this hypothesis [48].

6. New Determinations on the Mineo Pallasite

In the following, we present new Electron Probe Micro Analysis (EPMA) and Laser Ablation-Inductively Coupled Plasma-Mass Spectrometry (LA-ICP-MS) data to characterize further the Mineo pallasite. The main aims are to examine the compositional variability highlighted by Zucchini et al. 2018 [41] through the elemental and trace element mapping of a selected olivine crystal within the Mineo pallasite and to evaluate the implications of the revealed geochemical signature for the origin of pallasites.

6.1. Methods

6.1.1. EPMA

The elemental distributions of Mg, Si, Fe, Ni within the Mineo pallasite were performed with EPMA-WDS JEOL 8200 Super Probe with 5 WDS (wavelength dispersive spectrometer) channels and one EDS (energy dispersive spectrometer) channel at the Electron Microprobe Laboratory of the Earth Science Department “Ardito Desio” (University of Milan, Italy). The resulting maps were reported in Figure 4. Maps were acquired (i) in WDS, with exception of Ni (acquired in EDS); (ii) as semi-quantitative, i.e., the color-scale is relative to the counts of each element; (iii) with acquisition time for each pixel of 30 ms; (iv) with a voltage of 15 kV.

6.1.2. LA-ICP-MS

Olivines were imaged following the line rastering technique proposed by Ubide et al. (2015) [52] to produce multi-elemental crystal maps. The analyses were performed by LA-ICP-MS at the Petro-Volcanology Research Group (PVRG) facility, Department of Physics and Geology (Perugia), using a Teledyne Photon Machine G2 laser system coupled to a Thermo Fisher Scientific iCAP-Q ICP-MS. Helium was used as carrier gas with Ar and N2 added after the ablation cell to avoid plasma destabilization and enhance the instrumental sensitivity. We used a spot size, scan speed, repetition rate, and fluence of 10 µm, 6 μm/s, and 15 Hz, 3.5 J/cm2, respectively. The NIST SRM610 [53] and the USGS BCR2G [53] have been used as calibrator and quality control, respectively. Under the reported analytical conditions, precision and accuracy are typically better than 10%. Crystal maps were finally produced using the Iolite [54]. LA-ICP-MS compositional maps in Figure 5.

6.2. Results and Discussion

EPMA element distribution maps (Figure 4) highlight quite fragmental olivines with not sharp crystal-metal rims. Fe and Mg distributions are relatively homogeneous within a single olivine grain. This allows to conclude that the Fe compositional variability observed in Zucchini et al. (2018) [41] is not the result of Fe chemical zoning within single olivine grains/crystals; on the contrary, it can be attributed to different grains/crystals in the Mineo pallasite. Along olivine rims, Fe and Mg show complex distributions, with zones enriched and depleted in Mg and Si, showing an inverse correlation to Fe and Ni. Both Mg and Si ranges between 0 and 70 counts per second, reaching higher values within olivines and lower ones in correspondence with the metallic phases. Fe and Ni appear correlated and constitute the metallic phase that surrounds olivines, but Fe ranges between 2 and 24 counts per second while Ni is from 0 to 10 counts per second.
LA-ICP-MS trace element distribution maps within olivine crystals (Figure 5) reveal a concentration gradient in Cr, with alternating enriched and depleted bands, attributable to an oscillatory zoning pattern. The concentration gradient in Ti is correlated with that of Cr. The trace element maps of Mineo olivine also highlight the presence of veinlets or cracks enriched in P, Fe and Ni (10–20 μm in width), which cross the entire analyzed area. In particular, Ni is extremely enriched in the P-rich veinlets, showing value up to 50 × 103 ppm. In contrast, the distributions of Cr and Ti appear to be independent from the P-rich veinlets. The origin of this feature may be either linked to shock [55], associated with partial melting [56] or could be related to terrestrial weathering [57]. The Cr concentration of Mineo olivines estimated by Zucchini et al. (2018) [41] ranges between 161 and 544 ppm and is, in average, 321 ± 173 ppm. Figure 6 shows that the Cr content within Mineo olivines is slightly higher than the Cr concentration in pallasitic olivines from literature (87–237 ppm, [57]) but is below that found on Mars and Moon [58] and the Cr/Mn ratio is in the range, or slightly higher, than other PMG. Furthermore, the Cr to Al molar ratio in the Mineo olivine is close to 1 (average = 1.4), in agreement with those estimated by Chernonozhkin et al. (2021) [57] for the majority of the analyzed pallasites.
To start assessing which scenario is most likely for the origin of olivines hosted in the Mineo pallasite, we compare the Fe/Mg versus Fe/Mn plot of Mineo olivines with those of other PMG (Figure 7). Mineo values fall in the same trend defined by Chernonozhkin et al. (2021) [57], suggesting a common history. Also, Cr content of olivines in the Mineo pallasite is in the same range of PMG. Finally, Mineo pallasite share the evidence of oscillatory Cr zoning with the Imilac pallasite. The cause of this oscillatory zoning is largely debated [57,59]. McKibbin et al. (2013) [59] suggest that the oscillatory zoning may be a superimposed feature and attributes pallasite olivines to a restitic origin, while Chernonozhkin et al. (2021) [57] provide multiple explanations, all related to magmatic processes, concluding that the existence of oscillatory zoning within an olivine leads to exclude the formation of the crystal as a mantle restite. As a conclusion, our data support a similar history of the Mineo pallasite with the Esquel, Seymchan, Fukang and CMS 040071 pallasites. Considering the model of Chernonozhkin [57], based on a chondritic starting Mn/Mg composition, the Mineo olivines’ origin may be attributed either to a fractional crystallization or accumulation. However, Mittlefehldt et al. (1999) [48] calculations show that a simple cumulus origin is implausible. The explanation of the Cr oscillatory zoning requires further investigations and the petrologic evolution of olivines remains matter of debate.

7. Conclusions

In the present work, the preliminary achievements of the RockStar Group of the Department of Physics and Geology (University of Perugia, Italy) can be summarized as follow:
  • Astrophysical modelling. In recent years, an extended study on the nature of the mixing processes in AGB stars was pursued by the astrophysics group of Perugia led by Maurizio Busso. Latest nucleosynthesis models considering the activation of the 13C neutron source in AGB stars as a by-product of magnetically-induced mixing episodes were shown to explain several observational constraints on s-processing. In particular, magnetic models for low-mass stars with close-to-solar metallicity can reproduce the peculiar isotopic ratios of trace heavy elements measured in presolar SiC coming from ancient AGB stars.
  • Geochemical mapping of Mineo pallasites. The results from Zucchini et al. (2018) [41] allowed a preliminary classification of the Mineo meteorite to the PMG and showed a Fe compositional variability in olivines. In the present work, trace element distribution maps allowed to better constrain the geochemical variability showing that it can be attributed to different olivine grains/crystals and not to the chemical zonation within them. In fact, major element distribution maps highlight a relatively homogeneous distribution of Fe and Mg within olivine crystals and a more complex pattern along olivine rims, with zones enriched and depleted in Mg and Si, which show an inverse correlation to Fe and Ni. These characteristics confirm that Mineo belongs to the PMG and support the hypothesis of “early giant impact” formation theorized by Yang et al. 2010 [43]. Furthermore, trace element maps highlight also an oscillatory zoning pattern of Cr, but this behavior is not explained by a single model of olivine formation and further studies are needed in order to shed a light in the petrological evolution of pallasite olivines.
  • The meteorite collection. The specimens hosted by the Meteorite collection of the Department of Physics and Geology of Perugia University (Italy) have been classified according to the hierarchy introduced by Weisberg et al. (2006) [35].

Author Contributions

Conceptualization, L.R., M.P., F.F. and A.Z.; methodology, M.P.; validation, L.R., F.F., M.P.; investigation, M.P.; L.R.; data curation, L.R.; Writing—Original draft preparation, L.R., M.P., F.F., A.Z.; P.C.; A.B.; D.V.; O.T.; Writing—Review and editing, L.R.; F.F.; M.P.; D.V. supervision, F.F.; M.P. All authors have read and agreed to the published version of the manuscript.

Funding

This research was partially funded by the Department of Physics and Geology of the University of Perugia (Italy), Rockstar project and by INFN, section of Perugia, through funds provided by the Scientific Commission n. 3, ERNA2 (Nuclear Physics and Astrophysics).

Acknowledgments

D.V. acknowledges financial support from the German-Israeli Foundation (GIF No. I-1500-303.7/2019). L.R. wish to thank D. Albarn for his comments and constructive suggestions.

Conflicts of Interest

The authors declare no conflict of interest.

Appendix A

Table
Table A1. List of meteorite specimens hosted by the Meteorite collection of University of Perugia (Italy), classified following the scheme proposed by Weisberg et al. (2006) [35].
Table A1. List of meteorite specimens hosted by the Meteorite collection of University of Perugia (Italy), classified following the scheme proposed by Weisberg et al. (2006) [35].
Meteorite
Specimens		Traditional
Classification		Modern Classification [35]
NameCategoryCategoryClassClanGroupPetrologic TypeWeight (g)FallFindReferences
AlbaretochondriteChondritesOrdinaryH-L-LLL/LL47.471776 [60]
AllendechondriteChondritesCarbonaceousCV-CKCV344.871969 [61]
AllendechondriteChondritesCarbonaceousCV-CKCV393.971969 [61]
ArmelchondriteChondritesOrdinaryH-L-LLL550.9-1967[62]
AshmorechondriteChondritesOrdinaryH-L-LLH5104.1-1969[63]
BledsoechondriteChondritesOrdinaryH-L-LLH455.1-1970[64]
BondocmesosideriteAchondrites MES 30.2-1956[65]
BondocmesosideriteAchondrites MES 46.4-1956[65]
BoxholeoctahedriteAchondrites IIIAB 61.9-1937[66]
BoxholeoctahedriteAchondrites IIIAB 49.2-1937[66]
BrenhampallasiteAchondrites MG PAL 193-1882[67]
CallihamchondriteChondritesOrdinaryH-L-LLL648.6-1958[68]
Canyon diablooctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 118-1891[69]
Canyon diablooctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 104-1891[69]
Canyon diablooctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 135-1891[69]
Clovis (no 2)chondriteChondritesOrdinaryH-L-LLL637.9-1963[70]
Densmore (1879)chondriteChondritesOrdinaryH-L-LLL696.4-1879[71]
DimmittchondriteChondritesOrdinaryH-L-LLH3.748-1942[72]
Edmonson (a)chondriteChondritesOrdinaryH-L-LLL635.5-1955[73]
ErgheochondriteChondritesOrdinaryH-L-LLL5-1889 [74]
EtterchondriteChondritesOrdinaryH-L-LLL548.4-1965[66]
GibeonoctahedriteAchondrites IVA 82.2-1836[75]
GruverchondriteChondritesOrdinaryH-L-LLH463.8-1934[76]
HenburyoctahedriteAchondrites IIIAB 503-1931[77]
HobaataxiteAchondrites IVB 16.2-1920[78]
LakewoodchondriteChondritesOrdinaryH-L-LLL635-1955[79]
LandesoctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 81.49-1930[64]
Little River (b)chondriteChondritesOrdinaryH-L-LLH4/536.3-1965[80]
MessinachondriteChondritesOrdinaryH-L-LLL51616/07/1955 [81]
MineopallasiteAchondrites MG PAL 4203/05/1826 [41]
OdessaoctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 452.52- [82]
Otasawianoctahedrite doubtful Iron 634-1907[83]
Otasawianoctahedrite doubtful Iron 803-1907[83]
Pattioctahedrite 121922 [84]
Picachooctahedrite IIIAB 175.4-1952[85]
PlainschondriteChondritesOrdinaryH-L-LLH534.3-1964[62]
PlainschondriteChondritesOrdinaryH-L-LLH5228.3-1964[62]
Plainview (1917)chondriteChondritesOrdinaryH-L-LLH586.9-1917[76]
PotterchondriteChondritesOrdinaryH-L-LLL6124.6-1941[76]
PultuskchondriteChondritesOrdinaryH-L-LLH512-1868[76]
Roy (1933)chondriteChondritesOrdinaryH-L-LLL555.8-1933[86]
SallachondriteChondritesOrdinaryH-L-LLL620.47-1963[87]
ShawchondriteChondritesOrdinaryH-L-LLL6/750.655-1937[88]
SienachondriteChondritesOrdinaryH-L-LLLL5110.55-1794[89]
TolucaoctahedritePrimitive Achondrites WIN-IAB-IIICDIAB 142-1776[90]
Turtle RiveroctahedriteAchondrites IIIAB 133.38-1953[62]
Two butteschondriteChondritesOrdinaryH-L-LLH- - -
VigaranochondriteChondritesCarbonaceousCV-CKCV310.3-1910[38]
Wellman (c)chondriteChondritesOrdinaryH-L-LLH476.3-1964[91]
Universe 08 00156 i001 Stony meteorites. Universe 08 00156 i002 Iron meteorites. Universe 08 00156 i003 Story-iron meteorites.

Note

1
[Fe/H] ≡ log(Fe/H)star – log(Fe/H)Sun, where Fe/H is the ratio of the number (or mass) abundance of iron to that of hydrogen.

References

  1. Arnould, M.; Goriely, S. The p-process of stellar nucleosynthesis: Astrophysics and nuclear physics status. Phys. Rep. 2003, 384, 1–84. [Google Scholar] [CrossRef]
  2. Côté, B.; Eichler, M.; López, A.Y.; Vassh, N.; Mumpower, M.R.; Világos, B.; Soós, B.; Arcones, A.; Sprouse, T.M.; Surman, R.; et al. 129I and 247Cm in meteorites constrain the last astrophysical source of solar r-process elements. Science 2021, 371, 945–948. [Google Scholar] [CrossRef] [PubMed]
  3. Palmerini, S.; Trippella, O.; Busso, M.; Vescovi, D.; Petrelli, M.; Zucchini, A.; Frondini, F. s-Processing from MHD-induced mixing and isotopic abundances in presolar SiC grains. Geochim. Cosmochim. Acta 2018, 221, 21–36. [Google Scholar] [CrossRef] [Green Version]
  4. Vescovi, D.; Busso, M.; Palmerini, S.; Trippella, O.; Cristallo, S.; Piersanti, S.; Chieffi, A.; Limongi, M.; Hoppe, P.; Kratz, K.L. On the origin of Early Solar System Radioactivities: Problems with the Asymptotic Giant Branch and Massive Star Scenarios. Astrophys. J. 2018, 863, 115. [Google Scholar] [CrossRef]
  5. Busso, M. The Early Solar System. Astrophys. Space Sci. 2018, 453, 379–425. [Google Scholar] [CrossRef]
  6. Tommasini, S.; Bindi, L.; Petrelli, M.; Asimow, P.D.; Steinhardt, P.J. Trace Element Conundrum of Natural Quasicrystals. ACS Earth Sp. Chem. 2021, 5, 676–689. [Google Scholar] [CrossRef]
  7. Lenaz, D.; Schmitz, B. Crystal structure refinement of chromites from two achondrites, their T-f(O2) conditions, and implications. Meteor. Planet. Sci. 2017, 52, 1763–1775. [Google Scholar] [CrossRef]
  8. Lenaz, D.; Lughi, V.; Perugini, D.; Petrelli, M.; Turco, G.; Schmitz, B. MgAl2O4 spinels from Allende and NWA 763 carbonaceous chondrites: Structural refinement, cooling history, and trace element contents. Meteor. Planet. Sci. 2019, 54, 3089–3100. [Google Scholar] [CrossRef]
  9. Gemelli, M.; Di Rocco, T.; Folco, L.; D’Orazio, M. Parentage Identification of Differentiated Achondritic Meteorites by Hand-held Energy Dispersive X-Ray Fluorescence Spectrometry. Geostand. Geoanalytical Res. 2017, 41, 613–632. [Google Scholar] [CrossRef]
  10. Gemelli, M.; D’Orazio, M.; Folco, L. Chemical analysis of iron meteorites using a hand-held X-ray fuorescence spectrometer. Geostand. Geoanalytical Res. 2015, 39, 55–69. [Google Scholar] [CrossRef] [Green Version]
  11. Zinner, E. Stellar nucleosynthesis and the isotopic composition of presolar grains from primitive meteorites. Annu. Rev. Earth Planet. Sci. 1998, 26, 147–188. [Google Scholar] [CrossRef]
  12. Lugaro, M.; Davis, A.M.; Gallino, R.; Pellin, M.J.; Straniero, O.; Kappeler, F. Isotopic Compositions of Strontium, Zirconium, Molybdenum, and Barium in Single Presolar SiC Grains and Asymptotic Giant Branch Stars. Astrophys. J. Lett. 2003, 593, 486–508. [Google Scholar] [CrossRef] [Green Version]
  13. Hoppe, P.; Amari, S.; Zinner, E.; Ireland, T.; Lewis, R.S. Carbon, nitrogen, magnesium, silicon, and titanium isotopic compositions of single interstellar silicon grains from the Murchison carbonaceous chondrite. Astrophys. J. 1994, 430, 870–890. [Google Scholar] [CrossRef]
  14. Nittler, L.; Alexander, C.M.O.; Gallino, R.; Hoppe, P.; Nguyen, A.N.; Stadermann, F.J.; Zinner, E.K. Aluminium-, Calcium- and Titanium-rich Oxide Stardust in Ordinary Chondrite Meteorites. Astrophys. J. 2008, 682, 1450–1478. [Google Scholar] [CrossRef]
  15. Stephan, T.; Trappitsch, R.; Hoppe, P.; Davis, A.M.; Pellin, M.; Pardo, O.S. Molybdenum Isotopes in Presolar Silicon Carbide Grains: Details of s-process Nucleosynthesis in Parent Stars and Implications for r- and p-processes. Astrophys. J. 2019, 877, 101–116. [Google Scholar] [CrossRef]
  16. Nguyen, A.N.; Nittler, L.R.; Stadermann, F.J.; Stroud, R.M.; Alexander, C.M.O. Coordinated analyses of presolar grains in the Allan Hills 77307 and Queen Elizabeth Range 99177 Meteorites. Astrophys. J. 2010, 719, 166–189. [Google Scholar] [CrossRef] [Green Version]
  17. Liu, N.; Barosch, J.; Nittler, L.R.; Alexander, C.M.O.; Wang, J.; Cristallo, S.; Busso, M.; Palmerini, S. New Multielement Isotopic Compositions of Prelosar SiC Grains: Implications for Their Stellar Origins. Astrophys. J. 2021, 920, L26. [Google Scholar] [CrossRef]
  18. Hynes, K.M.; Gyngard, F. The presolar grain database. In Proceedings of the 40th Lunar Planetary Science Conference, Woodlands, TX, USA, 23–27 March 2009. [Google Scholar]
  19. Stephan, T.; Bose, M.; Boujibar, A.; Davis, A.M.; Dory, C.J.; Gyngard, F.; Hoppe, P.; Hynes, K.M.; Liu, N.; Nittler, L.R.; et al. The Presolar Grain Database Reloaded–Silicon Carbide. In Proceedings of the 51st Lunar and Planetary Science Conference, Woodlands, TX, USA, 10–16 March 2020. [Google Scholar]
  20. Nicolussi, G.; Davis, A.M.; Pellin, M.J.; Lewis, R.S.; Clayton, R.N.; Amari, S. s-Process Zirconium in Presolar Silicon Carbide Grains. Science 1997, 277, 1281–1284. [Google Scholar] [CrossRef] [Green Version]
  21. Trappitsch, R.; Stephan, T.; Savina, M.R.; Davis, A.M.; Pellin, M.J.; Rost, D.; Gyngard, F.; Gallino, R.; Bisterzo, S.; Cristallo, S.; et al. Simultaneous iron and nickel isotopic analyses of presolar silicon carbide grains. Geochim. Cosmochim. Acta 2018, 221, 87–108. [Google Scholar] [CrossRef]
  22. Busso, M.; Galliro, R.; Wasserburg, G.J. Nucleosynthesis in Asymptotic Giant Branch Stars: Relevance for Galactic Enrichment and Solar System Formation. Annu. Rev. Astron. Astrophys. 1999, 37, 239–309. [Google Scholar] [CrossRef] [Green Version]
  23. Zinner, E. Presolar grains. In Meteorites and Cosmochemical Processes, 2nd ed.; Davis Andrew, M., Ed.; Elsevier: Amsterdam, The Netherlands, 2014; Volume 1, pp. 181–213. [Google Scholar]
  24. Liu, N.; Savina, M.R.; Gallino, R.; Davis, A.M.; Bisterzo, S.; Gyngard, F.; Kappeler, F.; Cristallo, S.; Dauphas, N.; Pellin, M.J.; et al. Correlated strontium and barium isotopic compositions of acid-cleaned single mainstream silicon carbides from Murchison. Astrophys. J. 2015, 803, 12. [Google Scholar] [CrossRef] [Green Version]
  25. Liu, N.; Gallino, R.; Cristallo, S.; Bisterzo, S.; Davis, A.M.; Trappitsh, R.; Nittler, L.R. New Constrains on the Major Neutron Source in Low-mass AGB Stars. Astrophys. J. 2018, 865, 112. [Google Scholar] [CrossRef] [Green Version]
  26. Vescovi, D.; Cristallo, S.; Busso, M.; Liu, N. Magnetic-buoyancy-induced Mixing in AGB Stars: Presolar SiC Grains. Astrophys. J. 2020, 897, L25. [Google Scholar] [CrossRef]
  27. Busso, M.; Vescovi, D.; Palmerini, S.; Cristallo, S.; Delogu, V.A. s-processing in AGB Stars Revisited. III. Neutron Captures from MHD Mixing at Different Metallicities and Observational Constraints. Astrophys. J. 2021, 908, 55. [Google Scholar] [CrossRef]
  28. Palmerini, S.; Busso, M.; Vescovi, D.; Naselli, E.; Pidatella, A.; Mucciola, R.; Cristallo, S.; Mascali, D.; Mengoni, A.; Simonucci, S. Presolar Grain Isotopic Ratios as Costrains to Nuclear and Stellar Parameters of Asymptotic Giant Branch Star Nucleosynthetis. Astrophys. J. 2021, 921, 7. [Google Scholar] [CrossRef]
  29. Busso, M.; Wasserburg, G.J.; Nollett, K.M.; Calandra, A. Can Extra Mixing in RGB and AGB Stars Be Attributed to Magnetic Mechanisms? Astrophys. J. 2007, 671, 802–810. [Google Scholar] [CrossRef] [Green Version]
  30. Nucci, M.C.; Busso, M. Magnetohydrodynamics and Deep Mixing in Evolved Stars. Two- and Three-dimensional Analytical Models for Asymptotic Giant Branch. Astrophys. J. 2014, 787, 141. [Google Scholar] [CrossRef] [Green Version]
  31. Hoppe, P.; Annen, P.; Strebel, R.; Eberhardt, P.; Gallino, R.; Lugaro, M.; Amari, S.; Lewis, R.S. Meteoritic Silicon Carbide Grains with Unusual Si-Isotopic Compositions: Evidence for an Origin in Low-Mass, Low Metallicity Asymptotic Giant Branch Stars. Astrophys. J. 1997, 487, L101–L104. [Google Scholar] [CrossRef] [Green Version]
  32. Lewis, K.M.; Lugaro, M.; Gibson, B.K.; Pilkington, K. Decoding the message from meteoritic stardust silicon carbide grains. Astrophys. J. Lett. 2013, 768, L19. [Google Scholar] [CrossRef] [Green Version]
  33. Gail, H.-P.; Zhukovska, S.V.; Hoppe, P.; Trieloff, M. Stardust from Asymptotic Giant Branch Stars. Astrophys. J. 2009, 698, 1136–1154. [Google Scholar] [CrossRef] [Green Version]
  34. Cristallo, S.; Nanni, A.; Cescutti, G.; Minchev, I.; Liu, N.; Vescovi, D.; Gobrecht, D.; Piersanti, L. Mass and metallicity distribution of parent AGB stars of presolar SiC. Astron. Astrophys. 2020, 644, A8. [Google Scholar] [CrossRef]
  35. Weisberg, M.K.; McCoy, T.J.; Krot, A.N. Systematics and Evaluation of Meteorite Classification. In Meteorites and Early Solar System II; Lauretta, D.S., McSween, H.Y., Jr., Eds.; University of Arizona Press: Tucson, AZ, USA, 2006; pp. 19–52. [Google Scholar]
  36. Baldanza, B.; Cocco, G.; Levi-Donati, G.R. Meteoriti; Tipografia Porziuncola: Santa Maria degli Angeli, Italy, 1969. [Google Scholar]
  37. Grossman, L. Refractory Inclusions in the Allende Meteorite. Ann. Rev. Earth Planet. Sci. 1980, 8, 559–608. [Google Scholar] [CrossRef]
  38. Trevisani, E. History of the Vigarano meteorite (Emilia-Romagna, Italy) and recovery of an important part of the main mass. Rendiconti Lincei. 2011, 22, 315–326. [Google Scholar] [CrossRef]
  39. Baldanza, B. Italian meteorites. Mineral. Mag. 1965, 35, 214–232. [Google Scholar] [CrossRef]
  40. Nagata, N. Meteorite magnetism and the early solar system magnetic field. Phys. Earth Planet. Inter. 1979, 20, 324–341. [Google Scholar] [CrossRef]
  41. Zucchini, A.; Petrelli, M.; Frondini, F.; Petrone, C.M.; Sassi, P.; Di Michele, A.; Palmerini, S.; Trippella, O.; Busso, M. Chemical and mineralogical characterization of the Mineo (Sicily, Italy) pallasite: A unique sample. Meteorit. Planet. Sci. 2018, 53, 268–283. [Google Scholar] [CrossRef]
  42. Buseck, P.R. Pallasite meteorites—mineralogy, petrology and geochemistry. Geochim. Cosmochim. Acta 1977, 41, 711–740. [Google Scholar] [CrossRef]
  43. Yang, J.; Goldstein, J.I.; Scott, E.R.D. Main-group pallasites: Thermal history, relationship to IIIAB irons, and origin. Geochim. Cosmochim. Acta 2010, 74, 4471–4492. [Google Scholar] [CrossRef]
  44. Johnson, B.C.; Sori, M.M.; Evans, A.J. Ferrovolcanism on metal worlds and the origin of pallasites. Nat. Astron. 2019, 4, 41–44. [Google Scholar] [CrossRef] [Green Version]
  45. Grady, M.M. Catalog of Meteorites, 5th ed.; Cambridge University Press: Cambridge, UK, 2000. [Google Scholar]
  46. Mullane, E.; Alard, O.; Gounelle, M.; Russell, S. Laser ablation ICP-MS study of IIIAB irons and pallasites: Constraints on the behaviour of highly siderophile elements during and after planetesimal core formation. Chem. Geol. 2004, 208, 5–28. [Google Scholar] [CrossRef]
  47. Scott, E.R.D. Pallasites-Metal composition, classification and relationship with iron meteorites. Geochim. Cosmochim. Acta 1977, 41, 693–710. [Google Scholar] [CrossRef]
  48. Mittlefehldt, D.W. Geochemistry and origin of pallasite olivines. In Proceedings of the 30th Lunar and Planetary Science Conference, Houston, TX, USA, 15–19 March 1999. Abstract Number 1828. [Google Scholar]
  49. Mittlefehldt, D.W.; Herrin, J.S. Trace element compositions of pallasite olivine grains and pallasite origin. Meteorit. Planet. Sci. 2010, 73, 5386. [Google Scholar]
  50. Wasson, J.T.; Choi, B.-G. Main-group pallasites: Chemical composition, relationship to IIIAB irons, and origin. Geochim. Cosmochim. Acta 2003, 67, 3079–3096. [Google Scholar] [CrossRef]
  51. Mittlefehldt, D.W.; McCoy, T.J.; Goodrich, C.A.; Kracher, A. Non-chondritic meteorites from asteroidal bodies. In Planetary Materials; Papike, J.J., Ed.; Reviews in Mineralogy: Washington, DC, USA, 1998; Volume 36, pp. 4–195. [Google Scholar]
  52. Ubide, T.; McKenna, C.A.; Chew, D.M.; Kamber, B.S. High-resolution LA-ICP-MS trace element mapping of igneous minerals: In search of magma histories. Chem. Geol. 2015, 409, 157–168. [Google Scholar] [CrossRef]
  53. Gao, S.; Xiaomin, L.; Yuan, H.; Hattendorf, B.; Gunther, D.; Chen, L.; Hu, S. Determination of forty two major and trace elements in USGS and NIST SRM glasses buy laser ablation-inductively coupled plasma-mass spectrometry. Geost. Newsl. 2002, 26, 181–196. [Google Scholar] [CrossRef]
  54. Paul, B.; Paton, C.; Norris, A.; Woodhead, J.; Hellstrom, J.; Hergt, J.; Greig, A. CellSpace: A module for creating spatially registered laser ablation images within the Iolite freeware environment. J. Anal. At. Spectrom. 2012, 27, 700–706. [Google Scholar] [CrossRef]
  55. Desrousseaux, A.; Doukhan, J.C.; Leroux, H.; Van Duysen, J.C. An analytical electron microprobe investigation of some pallasites. Phys. Earth Planet. Inter. 1997, 103, 101–115. [Google Scholar] [CrossRef]
  56. Van Roosbroek, N.; Debaille, V.; Pittarello, L.; Goderis, S.; Humayun, M.; Hecht, L.; Jourdan, F.; Spicuzza, M.J.; Vahanecke, F.; Claeys, P. The formation of IIE iron meteorites investigated by the chondrule-bearing Mont Dieu meteorite. Meteorit. Planet. Sci. 2015, 50, 1173–1196. [Google Scholar] [CrossRef] [Green Version]
  57. Chernonozhikin, S.M.; McKibbin, S.J.; Goderis, S.; Van Malderen, S.J.M.; Claeys, P.; Vanhaecke, F. New constrains on the formation of main group pallasites derived from in situ trace element analysis and 2D mapping of olivine and phosphate. Chem. Geol. 2021, 562, 119996. [Google Scholar] [CrossRef]
  58. Papike, J.J.; Kerner, J.M.; Shearer, C.K. Comparative planetary mineralogy: Valence state partitioning of Cr, Fe, Ti, and V among crystallographic sites in olivine, pyroxene, and spinel from planetary basalts. Am. Mineral. 2005, 90, 277–290. [Google Scholar] [CrossRef] [Green Version]
  59. McKibbin, S.; O’Neill, H.S.C.; Mallmann, G.; Halfpenny, A. LA-ICP-MS mapping of olivine from Brahin and Brenham meteorites: Complex elemental distributions in the pallasite olivine precursor. Geochim. Cosmochim. Acta 2013, 119, 1–17. [Google Scholar] [CrossRef]
  60. Marvin, U.B. Ernst Florens Friedrich Chladni (1756–1827) and the origins of modern meteorite research. Meteorit. Planet. Sci. 1996, 31, 545–588. [Google Scholar] [CrossRef]
  61. Marvin, U.B.; Wood, J.A.; Dickey, J.S., Jr. Ca-Al rich phases in the Allende meteorite. Earth Planet. Sci. Lett. 1960, 7, 346–350. [Google Scholar] [CrossRef]
  62. Krinov, E.L. Meteoritical Bullettin, No. 49. Meteoritics 1970, 5, 173–176. [Google Scholar]
  63. Clarke, R.S., Jr. Meteoritical Bullettin, No. 51. Meteoritics 1972, 7, 215–232. [Google Scholar] [CrossRef]
  64. Clarke, R.S., Jr. Meteoritical Bullettin, No. 52. Meteoritics 1974, 9, 101–121. [Google Scholar]
  65. Nininger, H.H. Meteorite with unique features. Science 1963, 139, 345–347. [Google Scholar] [CrossRef] [PubMed]
  66. Clarke, R.S., Jr. Meteoritical Bullettin, No. 53. Meteoritics 1975, 10, 133–158. [Google Scholar]
  67. Smith, J.V.; Steele, I.M.; Leitch, A. Mineral chemistry of the shergottites, naklites, chassigny, brachina, pallasites and urelites. J. Geophys. Res. 1983, 88, B229–B236. [Google Scholar] [CrossRef]
  68. Krinov, E.L. Meteoritical Bullettin, No. 30. Meteoritics 1964.
  69. Clarke, R.S., Jr. Meteoritical Bullettin, No. 54. Meteoritics 1974, 11, 69–93. [Google Scholar]
  70. Krinov, E.L. Meteoritical bullettin, No. 32. Meteoritics 1964, 1–5. [Google Scholar]
  71. Schneider, D.M.; Benoit, P.H.; Sears, D.W.G.; Jull, A.J.T. The Kansas University meteorite. Meteorit. Planet. Sci. 1997, 32, A149–A150. [Google Scholar] [CrossRef]
  72. Van Schmus, W.R.; Wood, J.A. A chemical-petrologic classification for the chondritic meteorites. Geochim. Cosmochim. Acta 1967, 31, 747–754. [Google Scholar] [CrossRef]
  73. Graham, A.L. The Meteoritical Bullettin, No 61. Meteoritics 1983, 18, 77–83. [Google Scholar]
  74. Baldanza, B.; Levi-Donati, G.R. Evidence of shock-metamorphic effects in the Ergheo meteorite. Mineral. Mag. 1971, 38, 197–204. [Google Scholar] [CrossRef]
  75. Wasson, J.T. The chemical classification of iron meteorites: I. A study of iron meteorites with low concentrations of gallium and germanium. Geochim. Cosmochim. Acta 1967, 31, 161–180. [Google Scholar] [CrossRef]
  76. Mason, B. Olivine composition in chondrites. Geochim. Cosmochim. Acta 1963, 27, 1011–1023. [Google Scholar] [CrossRef]
  77. Alderman, A.R. The meteorite craters at Henbury, Central Australia. Mineral. Mag. 1932, 23, 19–32. [Google Scholar] [CrossRef]
  78. Murdin, P. Encyclopedia of Astronomy & Astrophysics; CRC Press: Boca Raton, FL, USA, 2000. [Google Scholar]
  79. Levi, F.A. X-Ray Non distructive Examination of stony meteorites. Meteoritics 1981, 16, 348. [Google Scholar]
  80. Kiesl, W.; Herr, W. Determination of the trace elements, Ru, Pd, Re, Os, Ir, Au, As, Se and Sb in stony meteorites. Chem. Erde 1977, 36, 324–331. [Google Scholar]
  81. Baldanza, B.; Labruto, G. Di una meteorite litoide caduta a Messina nel luglio 1955 (Nota preliminare). Rend. Della Soc. Mineral. Ital. 1956, 12, 47–48. [Google Scholar]
  82. Krinov, E.L. Meteoritical bullettin, No. 37. Meteoritics 1966, 1–2. [Google Scholar]
  83. Baldanza, B.; Pialli, G. Dynamically deformed structures in some meteorites. Meteor. Res. 1968, 806–825. [Google Scholar]
  84. D’Orazio, M.; Folco, L.; Perchiazzi, N. The Bagnore iron meteorite (Tuscany, Italy): History, mineralogy, and chemical classification. Meteor. Planet. Sci. 2004, 39, A133–A138. [Google Scholar] [CrossRef]
  85. Rasmussen, K.L. Cooling rates of IIIAB iron meteorites. Icarus 1989, 80, 315–325. [Google Scholar] [CrossRef]
  86. Nininger, H.H. The great meteor of March 24, 1933. Pop. Astron. 1934, 42, 292–306. [Google Scholar]
  87. Krinov, E.L. Meteoritical Bullettin, No. 31. Meteoritics 1964.
  88. Fredriksson, K.; Mason, B. The Shaw meteorite. Geochim. Cosmochim. Acta 1967, 31, 1705–1709. [Google Scholar] [CrossRef]
  89. Baldanza, B.; Levi-Donati, G.R.; Wiik, H.B. The Siena meteorite: Mineralogy and chemistry. Mineral. Mag. 1969, 37, 34–44. [Google Scholar] [CrossRef]
  90. Scott, E.R.D.; Wasson, J.T. Chemical classification of iron meteorites-VIII. Groups IC.IIE, IIF and 97 other irons. Geochim. Cosmochim. Acta 1976, 40, 103–108. [Google Scholar] [CrossRef]
  91. Sears, D.W.; Mills, A.A. Thermoluminescence and the terrestrial age of meteorites. Meteoritics 1974, 9, 47–67. [Google Scholar] [CrossRef]
Universe 08 00156 g001 550
Figure 1. Comparison between s-process models for AGB stars and presolar MS SiC grain data for Sr, Ba, and Zr. Isotopic ratios are expressed as part-per-mil deviations (δ) from the terrestrial value. Models are from Ref. [28] and refer to 2 M⊙ AGB stars at different metallicities, where magneto-hydrodynamic (MHD) processes induce the formation of the 13C pocket. Abundances are computed in stellar winds by considering 5% of mixing due to C-rich material transported to the envelope by magnetic blobs (see Ref. [28] for more details). Grain data are from the PDG database [19]. The picture is modified after Palmerini et al. (2021) [28].
Figure 1. Comparison between s-process models for AGB stars and presolar MS SiC grain data for Sr, Ba, and Zr. Isotopic ratios are expressed as part-per-mil deviations (δ) from the terrestrial value. Models are from Ref. [28] and refer to 2 M⊙ AGB stars at different metallicities, where magneto-hydrodynamic (MHD) processes induce the formation of the 13C pocket. Abundances are computed in stellar winds by considering 5% of mixing due to C-rich material transported to the envelope by magnetic blobs (see Ref. [28] for more details). Grain data are from the PDG database [19]. The picture is modified after Palmerini et al. (2021) [28].
Universe 08 00156 g001
Universe 08 00156 g002 550
Figure 2. Images of some specimens of the Meteorite collection of the University of Perugia (Italy) at different scales. (a) Vigarano; (b) Mineo; (c) Allende (images acquired by optical microscope); (d) Mineo (image acquired by EPMA).
Figure 2. Images of some specimens of the Meteorite collection of the University of Perugia (Italy) at different scales. (a) Vigarano; (b) Mineo; (c) Allende (images acquired by optical microscope); (d) Mineo (image acquired by EPMA).
Universe 08 00156 g002
Universe 08 00156 g003 550
Figure 3. Logarithmic Ga-Ge plot where Eagle Station (ES, red) and Main Group (MG, blue) pallasite fields are shown together with meteorite fields of IIIAB irons (dotted line) and IIE irons (segmented line). The Mineo data are in black (after Scott 1977 [47]). The picture is modified from Zucchini et al. (2018) [41]. (Color figure can be viewed at wileyonlinelibrary.com).
Figure 3. Logarithmic Ga-Ge plot where Eagle Station (ES, red) and Main Group (MG, blue) pallasite fields are shown together with meteorite fields of IIIAB irons (dotted line) and IIE irons (segmented line). The Mineo data are in black (after Scott 1977 [47]). The picture is modified from Zucchini et al. (2018) [41]. (Color figure can be viewed at wileyonlinelibrary.com).
Universe 08 00156 g003
Universe 08 00156 g004 550
Figure 4. Quantitative EPMA distribution maps of Mg, Fe, Si, Ni in a selected olivine crystal within the Mineo pallasite. The color-scale is relative to the counts of each element.
Figure 4. Quantitative EPMA distribution maps of Mg, Fe, Si, Ni in a selected olivine crystal within the Mineo pallasite. The color-scale is relative to the counts of each element.
Universe 08 00156 g004
Universe 08 00156 g005 550
Figure 5. Quantitative LA-ICP-MS distribution maps of Cr, Ti, P, Ni, Fe within an olivine crystal of the Mineo pallasite. The image on the top left indicates the area where the maps were acquired and the direction of the acquisition. The color-scale is relative to the parts per million of each element.
Figure 5. Quantitative LA-ICP-MS distribution maps of Cr, Ti, P, Ni, Fe within an olivine crystal of the Mineo pallasite. The image on the top left indicates the area where the maps were acquired and the direction of the acquisition. The color-scale is relative to the parts per million of each element.
Universe 08 00156 g005
Universe 08 00156 g006 550
Figure 6. Concentration of Cr (ppm) and Mn (ppm) in olivine from planetary basalts, compared with the concentration found within 8 PMG olivines [57] and Mineo pallasite olivines [41]. Modified after Papike et al. (2005) [58].
Figure 6. Concentration of Cr (ppm) and Mn (ppm) in olivine from planetary basalts, compared with the concentration found within 8 PMG olivines [57] and Mineo pallasite olivines [41]. Modified after Papike et al. (2005) [58].
Universe 08 00156 g006
Universe 08 00156 g007 550
Figure 7. Fe/Mg-Fe/Mn pallasite olivines plot. The picture is modified after Chernonozhkin et al. 2021. Chernonozhkin et al. 2021 [57] a Zucchini et al. 2018 [41] b.
Figure 7. Fe/Mg-Fe/Mn pallasite olivines plot. The picture is modified after Chernonozhkin et al. 2021. Chernonozhkin et al. 2021 [57] a Zucchini et al. 2018 [41] b.
Universe 08 00156 g007
Publisher’s Note: MDPI stays neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Share and Cite

MDPI and ACS Style

Ricci, L.; Petrelli, M.; Frondini, F.; Zucchini, A.; Comodi, P.; Bisciotti, A.; Vescovi, D.; Trippella, O. The Achievements of the RockStar Group (Perugia) on Astrophysical Modelling and Pallasite Geochemistry. Universe 2022, 8, 156. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8030156

AMA Style

Ricci L, Petrelli M, Frondini F, Zucchini A, Comodi P, Bisciotti A, Vescovi D, Trippella O. The Achievements of the RockStar Group (Perugia) on Astrophysical Modelling and Pallasite Geochemistry. Universe. 2022; 8(3):156. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8030156

Chicago/Turabian Style

Ricci, Lisa, Maurizio Petrelli, Francesco Frondini, Azzurra Zucchini, Paola Comodi, Andrea Bisciotti, Diego Vescovi, and Oscar Trippella. 2022. "The Achievements of the RockStar Group (Perugia) on Astrophysical Modelling and Pallasite Geochemistry" Universe 8, no. 3: 156. https://0-doi-org.brum.beds.ac.uk/10.3390/universe8030156

Note that from the first issue of 2016, this journal uses article numbers instead of page numbers. See further details here.

Article Metrics

Back to TopTop