Reto Trappitsch¹, Patrick Boehnke^2,3, Thomas Stephan^2,3, Myriam Telus⁴, Michael R. Savina¹, Olivia Pardo^2,3, Andrew M. Davis^2,3,5, Nicolas Dauphas^2,3,5, Michael J. Pellin^2,3,5,6, and Gary R. Huss⁷
Astrophysical Journal Letters 857, L2 Link to Article [DOI: 10.3847/2041-8213/aabba9]
¹Lawrence Livermore National Laboratory, Nuclear and Chemical Sciences Division, 7000 East Avenue, L-231, Livermore, CA 94550, USA
²The University of Chicago, Department of the Geophysical Sciences, 5734 South Ellis Avenue, Chicago, IL 60637, USA
³Chicago Center for Cosmochemistry, Chicago, IL, USA
⁴University of California Santa Cruz, Earth and Planetary Sciences, 1156 High Street, Santa Cruz, CA 95064, USA
⁵The University of Chicago, Enrico Fermi Institute, Chicago, IL 60637, USA
⁶Argonne National Laboratory, Materials Science Division, 9700 South Cass Avenue, Argonne, IL 60439, USA
⁷Hawai’i Institute of Geophysics and Planetology, School of Ocean, Earth Science and Technology, University of Hawai’i at Mānoa, 1680 East-West Road, POST 602, Honolulu, HI 96822, USA

Establishing the abundance of the extinct radionuclide ⁶⁰Fe (half-life 2.62 Ma) in the early solar system is important for understanding the astrophysical context of solar system formation. While bulk measurements of early solar system phases show a low abundance consistent with galactic background, some in situ measurements by secondary ion mass spectrometry (SIMS) imply a higher abundance, which would require injection from a nearby supernova (SN). Here we present in situ nickel isotopic analyses by resonance ionization mass spectrometry (RIMS) in a chondrule from the primitive meteorite Semarkona (LL3.00). The same chondrule had been previously analyzed by SIMS. Despite improved precision compared to SIMS, the RIMS nickel isotopic data do not reveal any resolved excesses of ⁶⁰Ni that could be unambiguously ascribed to in situ ⁶⁰Fe decay. Linear regression of ⁶⁰Ni/⁵⁸Ni versus ⁵⁶Fe/⁵⁸Ni yields an initial ⁶⁰Fe/⁵⁶Fe ratio for this chondrule of (3.8 ± 6.9) × 10⁻⁸, which is consistent with both the low initial value found by bulk measurements and the low end of the range of initial ratios inferred from some in situ work. The same regression also gives a solar initial ⁶⁰Ni/⁵⁸Ni ratio, which shows that this sample was not disturbed by nickel mobilization, thus agreeing with a low initial ⁶⁰Fe/⁵⁶Fe ratio. These findings agree with a re-evaluation of previous SIMS measurements of the same sample. Supernova injection of ⁶⁰Fe into the solar system or its parental cloud material is therefore not necessary to account for the measured solar system’s initial amount of ⁶⁰Fe.

Larry R. Nittler, Conel M. O’D. Alexander, Nan Liu¹, and Jianhua Wang
Astrophysical Journal Letters 856, L24 Link to Article [DOI: 10.3847/2041-8213/aab61f]
Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015, USA
¹Present address: Dept. of Physics, Washington University, 1 Brookings Drive, St. Louis, MO 63130, USA.

We report the identification of 19 presolar oxide grains from the Orgueil CI meteorite with substantial enrichments in ⁵⁴Cr, with ⁵⁴Cr/⁵²Cr ratios ranging from 1.2 to 56 times the solar value. The most enriched grains also exhibit enrichments at mass-50, most likely due in part to ⁵⁰Ti, but close-to-normal or depleted ⁵³Cr/⁵²Cr ratios. There is a strong inverse relationship between ⁵⁴Cr enrichment and grain size; the most extreme grains are all <80 nm in diameter. Comparison of the isotopic data with predictions of nucleosynthesis calculations indicate that these grains most likely originated in either rare, high-density Type Ia supernovae (SN Ia), or in electron-capture supernovae (ECSN), which may occur as the end stage of evolution for stars of mass 8–10 M _⊙. This is the first evidence for preserved presolar grains from either type of supernova. An ECSN origin is attractive, as these likely occur much more frequently than high-density SN Ia, and their evolutionary timescales (~20 Myr) are comparable to those of molecular clouds. Self-pollution of the Sun’s parent cloud from an ECSN may explain the heterogeneous distribution of n-rich isotopic anomalies in planetary materials, including a recently reported dichotomy in Mo isotopes in the solar system. The stellar origins of three grains with solar ⁵⁴Cr/⁵²Cr, but anomalies in ⁵⁰Cr or ⁵³Cr, as well as of a grain enriched in ⁵⁷Fe, are unclear.

Ryuki Hyodo and Hidenori Genda
Astrophysical Journal Letters 856, L36 Link to Article [DOI: 10.3847/2041-8213/aab7f0]
Earth-Life Science Institute/Tokyo Institute of Technology, 2-12-1 Tokyo, Japan

Observations and meteorites indicate that the Martian materials are enigmatically distributed within the inner solar system. A mega impact on Mars creating a Martian hemispheric dichotomy and the Martian moons can potentially eject Martian materials. A recent work has shown that the mega-impact-induced debris is potentially captured as the Martian Trojans and implanted in the asteroid belt. However, the amount, distribution, and composition of the debris has not been studied. Here, using hydrodynamic simulations, we report that a large amount of debris (~1% of Mars’ mass), including Martian crust/mantle and the impactor’s materials (~20:80), are ejected by a dichotomy-forming impact, and distributed between ~0.5–3.0 au. Our result indicates that unmelted Martian mantle debris (~0.02% of Mars’ mass) can be the source of Martian Trojans, olivine-rich asteroids in the Hungarian region and the main asteroid belt, and some even hit the early Earth. The evidence of a mega impact on Mars would be recorded as a spike of ⁴⁰Ar–³⁹Ar ages in meteorites. A mega impact can naturally implant Martian mantle materials within the inner solar system.

Yassir A. Abdu¹, Frank C. Hawthorne², and Maria E. Varela³
Astrophysical Journal Letters 856, L9 Link to Article [DOI: 10.3847/2041-8213/aab433]
¹Department of Applied Physics and Astronomy, University of Sharjah, P.O. Box 27272, Sharjah, United Arab Emirates
²Department of Geological Sciences, University of Manitoba, Winnipeg, MB R3T 2N2, Canada
³Instituto de Ciencias Astronómicas de la Tierra y del Espacio (ICATE) Avenida España 1512 sur, J5402DSP, San Juan, Argentina

We report the finding of nanodiamonds, coexisting with amorphous carbon, in carbonaceous-chondrite (CC) material from the Kapoeta achondritic meteorite by Fourier-transform infrared (FTIR) spectroscopy and micro-Raman spectroscopy. In the C–H stretching region (3100–2600 cm⁻¹), the FTIR spectrum of the Kapoeta CC material (KBr pellet) shows bands attributable to aliphatic CH₂ and CH₃ groups, and is very similar to IR spectra of organic matter in carbonaceous chondrites and the diffuse interstellar medium. Nanodiamonds, as evidenced by micro-Raman spectroscopy, were found in a dark region (~400 μm in size) in the KBr pellet. Micro-FTIR spectra collected from this region are dramatically different from the KBr-pellet spectrum, and their C–H stretching region is dominated by a strong and broad absorption band centered at ~2886 cm⁻¹ (3.47 μm), very similar to that observed in IR absorption spectra of hydrocarbon dust in dense interstellar clouds. Micro-FTIR spectroscopy also indicates the presence of an aldehyde and a nitrile, and both of the molecules are ubiquitous in dense interstellar clouds. In addition, IR peaks in the 1500–800 cm⁻¹ region are also observed, which may be attributed to different levels of nitrogen aggregation in diamonds. This is the first evidence for the presence of the 3.47 μm interstellar IR band in meteorites. Our results further support the assignment of this band to tertiary CH groups on the surfaces of nanodiamonds. The presence of the above interstellar bands and the absence of shock features in the Kapoeta nanodiamonds, as indicated by Raman spectroscopy, suggest formation by a nebular-condensation process similar to chemical-vapor deposition.

Oleksiy Golubov^1,2,3, Vladyslav Unukovych², and Daniel J. Scheeres¹
Astrophysical Journal Letters 857, L5 Link to Article [DOI: 10.3847/2041-8213/aaba15]
¹Department of Aerospace Engineering Sciences, University of Colorado at Boulder, 429 UCB, Boulder, CO 80309, USA
²School of Physics and Technology, V. N. Karazin Kharkiv National University, 4 Svobody Square, Kharkiv, 61022, Ukraine
³Institute of Astronomy of V. N. Karazin Kharkiv National University, 35 Sumska Street, Kharkiv, 61022, Ukraine

The evolution of rotation states of small asteroids is governed by the Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect, nonetheless some asteroids can stop their YORP evolution by attaining a stable equilibrium. The same is true for binary asteroids subjected to the binary YORP (BYORP) effect. Here we discuss a new type of equilibrium that combines these two, which is possible in a singly synchronous binary system. This equilibrium occurs when the normal YORP, the tangential YORP, and the BYORP compensate each other, and tidal torques distribute the angular momentum between the components of the system and dissipate energy. If unperturbed, such a system would remain singly synchronous in perpetuity with constant spin and orbit rates, as the tidal torques dissipate the incoming energy from impinging sunlight at the same rate. The probability of the existence of this kind of equilibrium in a binary system is found to be on the order of a few percent.

Andrew McNeill, David E. Trilling, and Michael Mommert
Astrophysical Journal Letters 857, L1 Link to Article [DOI: 10.3847/2041-8213/aab9ab]
Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86011, USA

1I/’Oumuamua was discovered by the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS 1) on 2017 October 19. Unlike all previously discovered minor planets, this object was determined to have eccentricity e > 1.0, suggesting an interstellar origin. Since this discovery and within the limited window of opportunity, several photometric and spectroscopic studies of the object have been made. Using the measured light curve amplitudes and rotation periods we find that, under the assumption of a triaxial ellipsoid, a density range 1500 < ρ < 2800 kg m⁻³ matches the observations and no significant cohesive strength is required. We also determine that an aspect ratio of 6 ± 1:1 is most likely after accounting for phase-angle effects and considering the potential effect of surface properties. This elongation is still remarkable, but less than some other estimates.

Sean N. Raymond¹, Philip J. Armitage^2,3, and Dimitri Veras^4,5
Astrophysical Journal Letters 856, L7 Link to Article [DOI: 10.3847/2041-8213/aab4f6]
¹Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
²JILA, University of Colorado and NIST, 440 UCB, Boulder, CO 80309-0440, USA
³Department of Astrophysical & Planetary Sciences, University of Colorado, Boulder, CO 80309-0391, USA
⁴Department of Physics, University of Warwick, Coventry CV4 7AL, UK
⁵Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, UK

‘Oumuamua was discovered passing through our solar system on a hyperbolic orbit. It presents an apparent contradiction, with colors similar to those of volatile-rich solar system bodies but with no visible outgassing or activity during its close approach to the Sun. Here, we show that this contradiction can be explained by the dynamics of planetesimal ejection by giant planets. We propose that ‘Oumuamua is an extinct fragment of a comet-like planetesimal born a planet-forming disk that also formed Neptune- to Jupiter-mass giant planets. On its pathway to ejection ‘Oumuamua’s parent body underwent a close encounter with a giant planet and was tidally disrupted into small pieces, similar to comet Shoemaker–Levy 9’s disruption after passing close to Jupiter. We use dynamical simulations to show that 0.1%–1% of cometary planetesimals undergo disruptive encounters prior to ejection. Rocky asteroidal planetesimals are unlikely to disrupt due to their higher densities. After disruption, the bulk of fragments undergo enough close passages to their host stars to lose their surface volatiles and become extinct. Planetesimal fragments such as ‘Oumuamua contain little of the mass in the population of interstellar objects but dominate by number. Our model makes predictions that will be tested in the coming decade by the Large Synoptic Survey Telescope.

Bethany L. EHLMANN^1,2, Robert HODYSS², Thomas F. BRISTOW³, George R. ROSSMAN¹,Eleonora AMMANNITO^4,6, M. Cristina DESANCTIS⁵, and Carol A. RAYMOND²
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13103]
¹Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
²Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91125, USA
³Exobiology Branch, NASA Ames Research Center, Moffett Field, California 94035, USA
⁴Department of Earth Planetary and Space Sciences, University of California, Los Angeles, California 90095–1567, USA
⁵Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Rome, Italy
⁶Present address: Italian Space Agency (ASI), 00133 Rome, Italy
Published by arrangement with John Wiley & Sons

Mg‐phyllosilicate‐bearing, dark surface materials on the dwarf planet Ceres have NH₄‐bearing materials, indicated by a distinctive 3.06 μm absorption feature. To constrain the identity of the Ceres NH₄‐carrier phase(s), we ammoniated ground particulates of candidate materials to compare their spectral properties to infrared data acquired by Dawn’s Visible and Infrared (VIR) imaging spectrometer. We treated Mg‐, Fe‐, and Al‐smectite clay minerals; Mg‐serpentines; Mg‐chlorite; and a suite of carbonaceous meteorites with NH₄‐acetate to exchange ammonium. Serpentines and chlorites showed no evidence for ammoniation, as expected due to their lack of exchangeable interlayer sites. Most smectites showed evidence for ammoniation by incorporation of NH₄⁺ into their interlayers, resulting in the appearance of absorptions from 3.02 to 3.08 μm. Meteorite samples tested had weak absorptions between 3.0 and 3.1 μm but showed little clear evidence for enhancement upon ammoniation, likely due to the high proportion of serpentine and other minerals relative to expandable smectite phases or to NH₄⁺ complexing with organics or other constituents. The wavelength position of the smectite NH₄ absorption showed no variation between IR spectra acquired under dry‐air purge at 25 °C and under vacuum at 25 °C to −180 °C. Collectively, data from the smectite samples show that the precise center wavelength of the characteristic ~3.05 μm v₃absorption in NH₄ is variable and is likely related to the degree of hydrogen bonding of NH₄‐H₂O complexes. Comparison with Dawn VIR spectra indicates that the hypothesis of Mg‐saponite as the ammonium carrier phase is the simplest explanation for observed data, and that Ceres dark materials may be like Cold Bokkeveld or Tagish Lake but with proportionally more Mg‐smectite.

N. G. RUDRASWAMI¹, D. FERNANDES¹, Agnelo DE ARAUJO¹, M. SHYAM PRASAD¹,and S. TAYLOR²
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13105]
¹National Institute of Oceanography (Council of Scientific and Industrial Research), Dona Paula, Goa 403004, India
²Cold Regions Research and Engineering Laboratory, 72 Lyme Road, Hanover, New Hampshire 03755–1290, USA
Published by arrangement with John Wiley & Sons

We studied 149 pyroxenes from 69 pyroxene‐bearing micrometeorites collected from deep‐sea sediments of the Indian Ocean and South Pole Water Well at Antarctica, Amundsen‐Scott South Pole station. The minor elements in pyroxenes from micrometeorites are present in the ranges as follows: MnO ~0.0–0.4 wt%, Al₂O₃ ~0.0–1.5 wt%, CaO ~0.0–1.0 wt%, Cr₂O₃ ~0.3–0.9 wt%, and FeO ~0.5–4 wt%. Their chemical compositions suggest that pyroxene‐bearing micrometeorites are mostly related to precursors from carbonaceous chondrites rather than ordinary chondrites. The Fe/(Fe+Mg) ratio of the pyroxenes and olivines in micrometeorites shows similarities to carbonaceous chondrites with values lying between 0 and 0.2, and those with values beyond this range are dominated by ordinary chondrites. Atmospheric entry of the pyroxene‐bearing micrometeorites is expected to have a relatively low entry velocity of <16 km s⁻¹ and high zenith angle (70–90°) to preserve their chemical compositions. In addition, similarities in the pyroxene and olivine mineralogical compositions between carbonaceous chondrites and cometary particles suggest that dust in the solar system is populated by materials from different sources that are chemically similar to each other. Our results on pyroxene chemical compositions reveal significant differences with those from ordinary chondrites. The narrow range in olivine and pyroxene chemical compositions are similar to those from carbonaceous chondrites, and a small proportion to ordinary chondrites indicates that dust is largely sourced from carbonaceous chondrite‐type bodies.

Xiao Hu (胡晓)^1,2, Jonathan C. Tan^1,3, Zhaohuan Zhu (朱照寰)², Sourav Chatterjee⁴, Tilman Birnstiel⁵, Andrew N. Youdin⁶, and Subhanjoy Mohanty⁷

Astrophysical Journal 857, 20 Link to Article [DOI: 10.3847/1538-4357/aaad08]
¹Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
²Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 South Maryland Parkway, Las Vegas, NV 89154, USA
³Department of Physics, University of Florida, Gainesville, FL 32611, USA
⁴Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA
⁵University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, D-81679 Munich, Germany
⁶Department of Astronomy and Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
⁷Imperial College London, 1010 Blackett Lab, Prince Consort Rd., London SW7 2AZ, UK

Systems with tightly packed inner planets (STIPs) are very common. Chatterjee & Tan proposed Inside-out Planet Formation (IOPF), an in situ formation theory, to explain these planets. IOPF involves sequential planet formation from pebble-rich rings that are fed from the outer disk and trapped at the pressure maximum associated with the dead zone inner boundary (DZIB). Planet masses are set by their ability to open a gap and cause the DZIB to retreat outwards. We present models for the disk density and temperature structures that are relevant to the conditions of IOPF. For a wide range of DZIB conditions, we evaluate the gap-opening masses of planets in these disks that are expected to lead to the truncation of pebble accretion onto the forming planet. We then consider the evolution of dust and pebbles in the disk, estimating that pebbles typically grow to sizes of a few centimeters during their radial drift from several tens of astronomical units to the inner, 1 au scale disk. A large fraction of the accretion flux of solids is expected to be in such pebbles. This allows us to estimate the timescales for individual planet formation and the entire planetary system formation in the IOPF scenario. We find that to produce realistic STIPs within reasonable timescales similar to disk lifetimes requires disk accretion rates of ~10⁻⁹ M _⊙ yr⁻¹ and relatively low viscosity conditions in the DZIB region, i.e., a Shakura–Sunyaev parameter of α ~ 10⁻⁴.