Aubrite Pesyanoe: Clues to composition and evolution of the enstatite achondrite parent body

2020 ◽  
Vol 55 (12) ◽  
pp. 2670-2702
Author(s):  
C. A. Lorenz ◽  
M. A. Ivanova ◽  
F. Brandstaetter ◽  
N. N. Kononkova ◽  
N. G. Zinovieva
Keyword(s):  
Parent Body

Increasing Energy Ration of Bali Cattle to Improve Digestible Nutrient, Milk Yield and Milk Quality

2017 ◽  
Vol 3 (1) ◽  
pp. 7
Author(s):  
Ni Nyoman Suryani ◽  
I Wayan Suarna ◽  
Ni Putu Sarini ◽  
I Gede Mahardika
Keyword(s):  
Energy Intake ◽  
Milk Production ◽  
Milk Yield ◽  
Milk Fat ◽  
Block Design ◽  
Parent Body ◽  
Milk Quality ◽  
Metabolizable Energy ◽  
Increase Energy Intake ◽  
Bali Cattle

To determine the effect of energy levels on digestible nutrient, milk production and milk quality of 7 months pregnant Bali cattle, was the purpose of this study. The study was conducted in Bali, Province of Indonesia on 12 pregnant breeding phase of pre-calving (2 months before the birth) with the parent body weight 329-340 kg/head. The treatment given is four types of Metabolizable Energy (ME) levels: 2000, 2100, 2200 and 2300/kg respectively as treatment A, B, C, and D. All ration contain 10% of crude protein. Variables measured: energy intake, digestible nutrient, milk yield, and milk quality. This research is a randomized block design. The results showed that increase energy ration until 2300 kcal ME/kg would significantly (P<0.05) increase energy intake and highest at cattle consumed ratio D is 22239.55 kcal/day. However, digestible nutrient was not affected. Milk production increased with increasing energy rations and highest (P<0.05) at cattle received treatment D is 2179.83 ml/day compared to treatment A 936.67 ml/day. Milk fat and milk lactose also highest (P<0.05) in treatment D are 8.56% and 4.76% respectively. Based on these results, it can be concluded that increase energy ration will increase energy intake, milk yield and milk fat and milk lactose of Bali cattle. 

scholarly journals Organic matter and water from asteroid Itokawa

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Q. H. S. Chan ◽  
A. Stephant ◽  
I. A. Franchi ◽  
X. Zhao ◽  
R. Brunetto ◽  
...  
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Parent Body ◽  
Asteroid Belt ◽  
True Nature ◽  
Water Ice ◽  
Nanocrystalline Graphite ◽  
Terrestrial Water ◽  
Solar System Bodies ◽  
Small Dust

AbstractUnderstanding the true nature of extra-terrestrial water and organic matter that were present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which was the first mission that brought pristine asteroidal materials to Earth’s astromaterial collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD =  + 4868 ± 2288‰; δ15N =  + 344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and offers support for material mixing in the asteroid belt that occurred in scales from small dust infall to catastrophic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modified by D-enriched exogenous organics and water derived from a carbonaceous parent body.

scholarly journals A Petrologic and Noble Gas Isotopic Study of New Basaltic Eucrite Grove Mountains 13001 from Antarctica

Minerals ◽  
2021 ◽  
Vol 11 (3) ◽  
pp. 279
Author(s):  
Chuantong Zhang ◽  
Bingkui Miao ◽  
Huaiyu He ◽  
Hongyi Chen ◽  
P. M. Ranjith ◽  
...  
Keyword(s):  
Noble Gas ◽  
Research Work ◽  
Cosmic Ray ◽  
Parent Body ◽  
Chemical Compositions ◽  
Isotopic Study ◽  
Impact Processes ◽  
Antarctic Research ◽  
Formation And Evolution ◽  
Grove Mountains

Howardite-Eucrite-Diogenite (HED) meteorite clan is a potential group of planetary materials which provides significant clues to understand the formation and evolution of the solar system. Grove Mountains (GRV) 13001 is a new member of HED meteorite, recovered from the Grove Mountains of Antarctica by the Chinese National Antarctic Research Expedition. This research work presents a comprehensive study of the petrology and mineralogy, chemical composition, noble gas isotopes, cosmic-ray exposure (CRE) age and nominal gas retention age for the meteorite GRV 13001. The output data indicate that GRV 13001 is a monomict basaltic eucrite with typical ophitic/subophitic texture, and it consists mainly of low-Ca pyroxene and plagioclase with normal eucritic chemical compositions. The noble gas based CRE age of the GRV 13001 is approximately 29.9 ± 3.0 Ma, which deviates from the major impact events or periods on the HED parent body. Additionally, the U,Th-4He and 40K-40Ar gas retention ages of this meteorite are ~2.5 to 4.0 Ga and ~3.6 to 4.1 Ga, respectively. Based on the noble gases isotopes and the corresponding ages, GRV 13001 may have experienced intense impact processes during brecciation, and weak thermal event after the ejection event at approximately 30 Ma.

scholarly journals Carbonate assemblages in Cold Bokkeveld CM chondrite reveal complex parent body evolution

2021 ◽  
Author(s):  
Stefan Farsang ◽  
Ian A. Franchi ◽  
Xuchao Zhao ◽  
Timothy D. Raub ◽  
Simon A.T. Redfern ◽  
...  
Keyword(s):  
Parent Body ◽  
Cm Chondrite

scholarly journals The Impact of Initial Conditions in N-Body Simulations of Debris Discs

2015 ◽  
Vol 32 ◽  
Author(s):  
E. Thilliez ◽  
S. T. Maddison
Keyword(s):  
Numerical Simulations ◽  
Initial Conditions ◽  
Parent Body ◽  
Dust Trapping ◽  
Physical Context ◽  
Disc Width ◽  
Wide Range ◽  
Belt Width ◽  
New Generation ◽  
The Impact

AbstractNumerical simulations are a crucial tool to understand the relationship between debris discs and planetary companions. As debris disc observations are now reaching unprecedented levels of precision over a wide range of wavelengths, an appropriate level of accuracy and consistency is required in numerical simulations to confidently interpret this new generation of observations. However, simulations throughout the literature have been conducted with various initial conditions often with little or no justification. In this paper, we aim to study the dependence on the initial conditions of N-body simulations modelling the interaction between a massive and eccentric planet on an exterior debris disc. To achieve this, we first classify three broad approaches used in the literature and provide some physical context for when each category should be used. We then run a series of N-body simulations, that include radiation forces acting on small grains, with varying initial conditions across the three categories. We test the influence of the initial parent body belt width, eccentricity, and alignment with the planet on the resulting debris disc structure and compare the final peak emission location, disc width and offset of synthetic disc images produced with a radiative transfer code. We also track the evolution of the forced eccentricity of the dust grains induced by the planet, as well as resonance dust trapping. We find that an initially broad parent body belt always results in a broader debris disc than an initially narrow parent body belt. While simulations with a parent body belt with low initial eccentricity (e ~ 0) and high initial eccentricity (0 < e < 0.3) resulted in similar broad discs, we find that purely secular forced initial conditions, where the initial disc eccentricity is set to the forced value and the disc is aligned with the planet, always result in a narrower disc. We conclude that broad debris discs can be modelled by using either a dynamically cold or dynamically warm parent belt, while in contrast eccentric narrow debris rings are reproduced using a secularly forced parent body belt.

Anomalously porous boulders on (162173) Ryugu as primordial materials from its parent body

2021 ◽  
Author(s):  
N. Sakatani ◽  
S. Tanaka ◽  
T. Okada ◽  
T. Fukuhara ◽  
L. Riu ◽  
...  
Keyword(s):  
Parent Body

scholarly journals Accretion of a large LL parent planetesimal from a recently formed chondrule population

2020 ◽  
Vol 6 (16) ◽  
pp. eaay8641
Author(s):  
Graham H. Edwards ◽  
Terrence Blackburn
Keyword(s):  
Body Size ◽  
Size Distribution ◽  
Total Duration ◽  
Parent Body ◽  
Ordinary Chondrite ◽  
Minimum Size ◽  
Thermal Models ◽  
Early Stages ◽  
Chondritic Meteorites ◽  
Chondrule Formation

Chondritic meteorites, derived from asteroidal parent bodies and composed of millimeter-sized chondrules, record the early stages of planetary assembly. Yet, the initial planetesimal size distribution and the duration of delay, if any, between chondrule formation and chondrite parent body accretion remain disputed. We use Pb-phosphate thermochronology with planetesimal-scale thermal models to constrain the minimum size of the LL ordinary chondrite parent body and its initial allotment of heat-producing 26Al. Bulk phosphate 207Pb/206Pb dates of LL chondrites record a total duration of cooling ≥75 Ma, with an isothermal interior that cools over ≥30 Ma. Since the duration of conductive cooling scales with parent body size, these data require a ≥150-km radius parent body and a range of bulk initial 26Al/27Al consistent with the initial 26Al/27Al ratios of constituent LL chondrules. The concordance suggests that rapid accretion of a large LL parent asteroid occurred shortly after a major chondrule-forming episode.

60Fe–60Ni systematics in the eucrite parent body: A case study of Bouvante and Juvinas

2011 ◽  
Vol 75 (23) ◽  
pp. 7698-7706 ◽  
Author(s):  
Ghylaine Quitté ◽  
Christopher Latkoczy ◽  
Maria Schönbächler ◽  
Alex N. Halliday ◽  
Detlef Günther
Keyword(s):  
Parent Body

Compositional continuity of enstatite chondrites and implications for heterogeneous accretion of the enstatite chondrite parent body

1997 ◽  
Vol 61 (22) ◽  
pp. 4895-4914 ◽  
Author(s):  
Ping Kong ◽  
Tadashi Mori ◽  
Mitsuru Ebihara
Keyword(s):  
Parent Body ◽  
Enstatite Chondrite ◽  
Enstatite Chondrites

scholarly journals Meteoritic amino acids as chemical tracers of parent-body chemistries

2021 ◽  
Vol 502 (3) ◽  
pp. 4064-4073
Author(s):  
Y Ellinger ◽  
M Lattelais ◽  
F Pauzat ◽  
J-C Guillemin ◽  
B Zanda
Keyword(s):  
Amino Acids ◽  
Relative Stability ◽  
Density Functional ◽  
Minimum Energy ◽  
Protonated Form ◽  
Parent Body ◽  
Chemical Formula ◽  
Energy Principle ◽  
Chemical Tracers ◽  
Minimum Energy Principle

ABSTRACT The analysis of the organic matter of meteorites made it possible to identify over 70 amino acids (AA), including 8 of those found in living organisms. However, their relative abundances vary drastically with the type of the carbonaceous chondrite, even for isomers of same chemical formula. In this report, we address the question whether this difference may have its origin in the relative stability of these isomers according to the conditions they experienced when they were formed and after. To this end, we rely on the fact that for most of the species observed so far in the interstellar medium (ISM), the most abundant isomer of a given generic chemical formula is the most stable one (minimum energy principle, MEP). Using quantum density functional theory (DFT) simulations, we investigate the relative stability of the lowest energy isomers of alanine (Ala) and amino butyric acid (ABA) in the neutral, protonated, and zwitterionic structures together with corresponding nitrile precursors. It is shown that β-alanine and γ-ABA are the most stable in a protonated form, whereas α-AA are the most stable in the zwitterionic and nitrile structures. The different composition of the carbonaceous chondrites CIs and CMs could be linked to the chemical context of the aqueous alterations of the parent bodies.

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