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Journal articles on the topic 'Asteroid 16 Psyche'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Viikinkoski, M., P. Vernazza, J. Hanuš, H. Le Coroller, K. Tazhenova, B. Carry, M. Marsset, et al. "(16) Psyche: A mesosiderite-like asteroid?" Astronomy & Astrophysics 619 (November 2018): L3. http://dx.doi.org/10.1051/0004-6361/201834091.

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Context. Asteroid (16) Psyche is the target of the NASA Psyche mission. It is considered one of the few main-belt bodies that could be an exposed proto-planetary metallic core and that would thus be related to iron meteorites. Such an association is however challenged by both its near- and mid-infrared spectral properties and the reported estimates of its density. Aims. Here, we aim to refine the density of (16) Psyche to set further constraints on its bulk composition and determine its potential meteoritic analog. Methods. We observed (16) Psyche with ESO VLT/SPHERE/ZIMPOL as part of our large program (ID 199.C-0074). We used the high angular resolution of these observations to refine Psyche’s three-dimensional (3D) shape model and subsequently its density when combined with the most recent mass estimates. In addition, we searched for potential companions around the asteroid. Results. We derived a bulk density of 3.99 ± 0.26 g cm−3 for Psyche. While such density is incompatible at the 3-sigma level with any iron meteorites (∼7.8 g cm−3), it appears fully consistent with that of stony-iron meteorites such as mesosiderites (density ∼4.25 g cm−3). In addition, we found no satellite in our images and set an upper limit on the diameter of any non-detected satellite of 1460 ± 200 m at 150 km from Psyche (0.2% × RHill, the Hill radius) and 800 ± 200 m at 2000 km (3% × RHill). Conclusions. Considering that the visible and near-infrared spectral properties of mesosiderites are similar to those of Psyche, there is merit to a long-published initial hypothesis that Psyche could be a plausible candidate parent body for mesosiderites.

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2

Ferrais, M., P. Vernazza, L. Jorda, N. Rambaux, J. Hanuš, B. Carry, F. Marchis, et al. "Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid." Astronomy & Astrophysics 638 (June 2020): L15. http://dx.doi.org/10.1051/0004-6361/202038100.

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Context. Asteroid (16) Psyche is the largest M-type asteroid in the main belt and the target of the NASA Psyche mission. It is also the only asteroid of this size (D > 200 km) known to be metal rich. Although various hypotheses have been proposed to explain the rather unique physical properties of this asteroid, a perfect understanding of its formation and bulk composition is still missing. Aims. We aim to refine the shape and bulk density of (16) Psyche and to perform a thorough analysis of its shape to better constrain possible formation scenarios and the structure of its interior. Methods. We obtained disk-resolved VLT/SPHERE/ZIMPOL images acquired within our ESO large program (ID 199.C-0074), which complement similar data obtained in 2018. Both data sets offer a complete coverage of Psyche’s surface. These images were used to reconstruct the three-dimensional (3D) shape of Psyche with two independent shape modeling algorithms (MPCD and ADAM). A shape analysis was subsequently performed, including a comparison with equilibrium figures and the identification of mass deficit regions. Results. Our 3D shape along with existing mass estimates imply a density of 4.20 ± 0.60 g cm−3, which is so far the highest for a solar system object following the four telluric planets. Furthermore, the shape of Psyche presents small deviations from an ellipsoid, that is, prominently three large depressions along its equator. The flatness and density of Psyche are compatible with a formation at hydrostatic equilibrium as a Jacobi ellipsoid with a shorter rotation period of ∼3h. Later impacts may have slowed down Psyche’s rotation, which is currently ∼4.2 h, while also creating the imaged depressions. Conclusions. Our results open the possibility that Psyche acquired its primordial shape either after a giant impact while its interior was already frozen or while its interior was still molten owing to the decay of the short-lived radionuclide 26Al.

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3

Siltala, L., and M. Granvik. "Asteroid mass estimation with the robust adaptive Metropolis algorithm." Astronomy & Astrophysics 633 (January 2020): A46. http://dx.doi.org/10.1051/0004-6361/201935608.

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Context. The bulk density of an asteroid informs us about its interior structure and composition. To constrain the bulk density, one needs an estimated mass of the asteroid. The mass is estimated by analyzing an asteroid’s gravitational interaction with another object, such as another asteroid during a close encounter. An estimate for the mass has typically been obtained with linearized least-squares methods, despite the fact that this family of methods is not able to properly describe non-Gaussian parameter distributions. In addition, the uncertainties reported for asteroid masses in the literature are sometimes inconsistent with each other and are suspected to be unrealistically low. Aims. We aim to present a Markov-chain Monte Carlo (MCMC) algorithm for the asteroid mass estimation problem based on asteroid-asteroid close encounters. We verify that our algorithm works correctly by applying it to synthetic data sets. We use astrometry available through the Minor Planet Center to estimate masses for a select few example cases and compare our results with results reported in the literature. Methods. Our mass-estimation method is based on the robust adaptive Metropolis algorithm that has been implemented into the OpenOrb asteroid orbit computation software. Our method has the built-in capability to analyze multiple perturbing asteroids and test asteroids simultaneously. Results. We find that our mass estimates for the synthetic data sets are fully consistent with the ground truth. The nominal masses for real example cases typically agree with the literature but tend to have greater uncertainties than what is reported in recent literature. Possible reasons for this include different astrometric data sets and weights, different test asteroids, different force models or different algorithms. For (16) Psyche, the target of NASA’s Psyche mission, our maximum likelihood mass is approximately 55% of what is reported in the literature. Such a low mass would imply that the bulk density is significantly lower than previously expected and thus disagrees with the theory of (16) Psyche being the metallic core of a protoplanet. We do, however, note that masses reported in recent literature remain within our 3-sigma limits. Results. The new MCMC mass-estimation algorithm performs as expected, but a rigorous comparison with results from a least-squares algorithm with the exact same data set remains to be done. The matters of uncertainties in comparison with other algorithms and correlations of observations also warrant further investigation.

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4

Elkins-Tanton, Linda T. "Asteroid 16 Psyche: NASA's 14th Discovery Mission." Elements 14, no. 1 (February 1, 2018): 68. http://dx.doi.org/10.2138/gselements.14.1.68.

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5

Becker, Tracy M., Nathaniel Cunningham, Philippa Molyneux, Lorenz Roth, Lori M. Feaga, Kurt D. Retherford, Zoe A. Landsman, Emma Peavler, Linda T. Elkins-Tanton, and Jan-Erik Walhund. "HST UV Observations of Asteroid (16) Psyche." Planetary Science Journal 1, no. 3 (October 26, 2020): 53. http://dx.doi.org/10.3847/psj/abb67e.

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6

Binzel, Richard P., Schelte J. Bus, Shui Xu, Jessica Sunshine, Thomas H. Burbine, A. William Neely, and Robert W. Brown. "Rotationally Resolved Spectra of Asteroid 16 Psyche." Icarus 117, no. 2 (October 1995): 443–45. http://dx.doi.org/10.1006/icar.1995.1170.

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7

Siltala, Lauri, and Mikael Granvik. "Mass and Density of Asteroid (16) Psyche." Astrophysical Journal Letters 909, no. 1 (March 1, 2021): L14. http://dx.doi.org/10.3847/2041-8213/abe948.

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8

Shepard, Michael K., Katherine de Kleer, Saverio Cambioni, Patrick A. Taylor, Anne K. Virkki, Edgard G. Rívera-Valentin, Carolina Rodriguez Sanchez-Vahamonde, et al. "Asteroid 16 Psyche: Shape, Features, and Global Map." Planetary Science Journal 2, no. 4 (July 15, 2021): 125. http://dx.doi.org/10.3847/psj/abfdba.

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9

Shepard, Michael K., James Richardson, Patrick A. Taylor, Linda A. Rodriguez-Ford, Al Conrad, Imke de Pater, Mate Adamkovics, et al. "Radar observations and shape model of asteroid 16 Psyche." Icarus 281 (January 2017): 388–403. http://dx.doi.org/10.1016/j.icarus.2016.08.011.

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10

Avdellidou, C., M. Delbo’, and A. Fienga. "Exogenous origin of hydration on asteroid (16) Psyche: the role of hydrated asteroid families." Monthly Notices of the Royal Astronomical Society 475, no. 3 (February 9, 2018): 3419–28. http://dx.doi.org/10.1093/mnras/sty017.

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11

Takir, Driss, Vishnu Reddy, Juan A. Sanchez, Michael K. Shepard, and Joshua P. Emery. "DETECTION OF WATER AND/OR HYDROXYL ON ASTEROID (16) Psyche." Astronomical Journal 153, no. 1 (December 28, 2016): 31. http://dx.doi.org/10.3847/1538-3881/153/1/31.

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12

Lupishko, D. F. "On the bulk density of the M-type asteroid 16 Psyche." Solar System Research 40, no. 3 (May 2006): 214–18. http://dx.doi.org/10.1134/s0038094606030051.

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13

Sanchez, Juan A., Vishnu Reddy, Michael K. Shepard, Cristina Thomas, Edward A. Cloutis, Driss Takir, Albert Conrad, Cain Kiddell, and Daniel Applin. "DETECTION OF ROTATIONAL SPECTRAL VARIATION ON THE M-TYPE ASTEROID (16) PSYCHE." Astronomical Journal 153, no. 1 (December 28, 2016): 29. http://dx.doi.org/10.3847/1538-3881/153/1/29.

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14

Kuzmanoski, M., and A. Kovačević. "Motion of the asteroid (13206) 1997GC22 and the mass of (16) Psyche." Astronomy & Astrophysics 395, no. 2 (November 2002): L17—L19. http://dx.doi.org/10.1051/0004-6361:20021444.

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15

Fatemi, Shahab, and Andrew R. Poppe. "Solar Wind Plasma Interaction with Asteroid 16 Psyche: Implication for Formation Theories." Geophysical Research Letters 45, no. 1 (January 8, 2018): 39–48. http://dx.doi.org/10.1002/2017gl073980.

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16

Landsman, Zoe A., Joshua P. Emery, Humberto Campins, Josef Hanuš, Lucy F. Lim, and Dale P. Cruikshank. "Asteroid (16) Psyche: Evidence for a silicate regolith from spitzer space telescope spectroscopy." Icarus 304 (April 2018): 58–73. http://dx.doi.org/10.1016/j.icarus.2017.11.035.

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17

Cantillo, David C., Vishnu Reddy, Benjamin N. L. Sharkey, Neil A. Pearson, Juan A. Sanchez, Matthew R. M. Izawa, Theodore Kareta, Tanner S. Campbell, and Om Chabra. "Constraining the Regolith Composition of Asteroid (16) Psyche via Laboratory Visible Near-infrared Spectroscopy." Planetary Science Journal 2, no. 3 (May 12, 2021): 95. http://dx.doi.org/10.3847/psj/abf63b.

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18

Peplowski, Patrick N., Jack T. Wilson, Morgan Burks, Andrew W. Beck, Insoo Jun, David J. Lawrence, and Zachary W. Yokley. "Cosmogenic radionuclide production modeling with Geant4: Experimental benchmarking and application to nuclear spectroscopy of asteroid (16) Psyche." Nuclear Instruments and Methods in Physics Research Section B: Beam Interactions with Materials and Atoms 446 (May 2019): 43–57. http://dx.doi.org/10.1016/j.nimb.2019.03.023.

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19

Matter, Alexis, Marco Delbo, Benoit Carry, and Sebastiano Ligori. "Evidence of a metal-rich surface for the Asteroid (16) Psyche from interferometric observations in the thermal infrared." Icarus 226, no. 1 (September 2013): 419–27. http://dx.doi.org/10.1016/j.icarus.2013.06.004.

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20

Drummond, Jack D., William J. Merline, Benoit Carry, Al Conrad, Vishnu Reddy, Peter Tamblyn, Clark R. Chapman, et al. "The triaxial ellipsoid size, density, and rotational pole of asteroid (16) Psyche from Keck and Gemini AO observations 2004–2015." Icarus 305 (May 2018): 174–85. http://dx.doi.org/10.1016/j.icarus.2018.01.010.

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21

Peplowski, Patrick N., Morgan Burks, John O. Goldsten, Samuel Fix, Lena E. Heffern, David J. Lawrence, and Zachary W. Yokley. "Radiation damage and annealing of three coaxial n-type germanium detectors: Preparation for spaceflight missions to asteroid 16 Psyche and Mars’ moon Phobos." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 942 (October 2019): 162409. http://dx.doi.org/10.1016/j.nima.2019.162409.

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22

Kenworthy, M. A., S. N. Mellon, J. I. Bailey, R. Stuik, P. Dorval, G. J. J. Talens, S. R. Crawford, et al. "The β Pictoris b Hill sphere transit campaign." Astronomy & Astrophysics 648 (April 2021): A15. http://dx.doi.org/10.1051/0004-6361/202040060.

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Aims. Photometric monitoring of β Pic in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of the gas giant planet β Pic b and the predicted transit of its Hill sphere to within a 0.1 au projected separation of the planet provided an opportunity to search for the transit of a circumplanetary disk (CPD) in this 21 ± 4 Myr-old planetary system. We aim to detect, or put an upper limit on, the density and nature of the material in the circumplanetary environment of the planet via the continuous photometric monitoring of the Hill sphere transit that occurred in 2017 and 2018. Methods. Continuous broadband photometric monitoring of β Pic requires ground-based observatories at multiple longitudes to provide redundancy and to provide triggers for rapid spectroscopic follow-up. These include the dedicated β Pic monitoring bRing observatories in Sutherland and Siding Springs, the ASTEP400 telescope at Concordia, and the space observatories BRITE and the Hubble Space Telescope (HST). We search the combined light curves for evidence of short-period transient events caused by rings as well as for longer-term photometric variability due to diffuse circumplanetary material. Results. We find no photometric event that matches with the event seen in November 1981, and there is no systematic photometric dimming of the star as a function of the Hill sphere radius. Conclusions. We conclude that the 1981 event was not caused by the transit of a CPD around β Pic b. The upper limit on the long-term variability of β Pic places an upper limit of 1.8 × 1022 g of dust within the Hill sphere (comparable to the ~100 km radius asteroid 16 Psyche). Circumplanetary material is either condensed into a disk that does not transit β Pic, condensed into a disk with moons that has an obliquity that does not intersect with the path of β Pic behind the Hill sphere, or is below our detection threshold. This is the first time that a dedicated international campaign has mapped the Hill sphere transit of an extrasolar gas giant planet at 10 au.

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23

Caldwell, Wendy K., Abigail Hunter, Catherine S. Plesko, and Stephen Wirkus. "Understanding Asteroid 16 Psyche’s composition through 3D impact crater modeling." Icarus 351 (November 2020): 113962. http://dx.doi.org/10.1016/j.icarus.2020.113962.

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24

Moura, T. S., O. C. Winter, A. Amarante, R. Sfair, G. Borderes-Motta, and G. Valvano. "Dynamical Environment and Surface Characteristics of Asteroid (16) Psyche." Monthly Notices of the Royal Astronomical Society, November 19, 2019. http://dx.doi.org/10.1093/mnras/stz3210.

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Abstract Radar observations show that (16) Psyche is one of the largest and most massive asteroids of the M-class located in the main belt, with a diameter of approximately 230 km. This fact makes Psyche a unique object since observations indicated an iron-nickel composition. It is believed that this body may be what was left of a metal core of an early planet that would have been fragmented over millions of years due to violent collisions. In this work we study a variety of dynamical aspects related to the surface, as well as, the environment around this asteroid. We use computational tools to explore the gravitational field generated by this body, assuming constant values for its density and rotation period. We then determine a set of physical and dynamical characteristics over its entire surface. The results include the geometric altitude, geopotential altitude, tilt, slope, among others. We also explore the neighborhood around the asteroid (16) Psyche, so that the location and linear stability of the equilibrium points were found. We found four external equilibrium points, two of them linearly stable. We confirmed the stability of these points by performing numerical simulations of massless particles around the asteroid, which also showed an asymmetry in the size of the stable regions. In addition, we integrate a cloud of particles in the vicinity of (16) Psyche in order to verify in which regions of its surface the particles are most likely to collide.

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25

Raducan, S. D., T. M. Davison, and G. S. Collins. "Morphological Diversity of Impact Craters on Asteroid (16) Psyche: Insight From Numerical Models." Journal of Geophysical Research: Planets 125, no. 9 (September 2020). http://dx.doi.org/10.1029/2020je006466.

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