Pith. sign in

REVIEW 1 cited by

The discovery and characterization of minimoon 2024 PT$_5$

T0 review · reviewed 2026-08-12 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read 2024 PT5 is a newly discovered ~5 m minimoon captured by Earth for about 60 days, with colors and density resembling lunar rock and S-type asteroids.

arxiv 2411.08029 v2 pith:NZMVOTOF submitted 2024-11-12 astro-ph.EP

Bryce T. Bolin , Larry Denneau , Laura-May Abron , Robert Jedicke , Kristin Chiboucas , Carl Ingerbretsen , Brian C. Lemaux This is my paper · ORCID
classification astro-ph.EP
keywords minimoonsystemasteroidscaptureddiscoveryearth-moongeminilunar
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

An asteroid called 2024 PT5 was discovered in August 2024 by the ATLAS telescope in Sutherland, South Africa. Follow-up observations with the Gemini North telescope in Hawaii gave the object's brightness in four colors, g, r, i, and Z, and tracked its changing brightness over about 40 minutes. The orbit, computed from hundreds of astrometric measurements, shows that the object entered a temporary gravitational association with Earth on September 29, 2024, and left on November 25, a capture lasting only about 60 days. That makes it the shortest-lived minimoon known, and it did not complete a full loop around Earth.

The colors place 2024 PT5 close to lunar rock samples and to Sv-type asteroids, two groups that are hard to tell apart with only four broadband measurements. Assuming an albedo of 0.21, the absolute magnitude of 28.6 implies a diameter near 5 meters. The orbit fit also detects a small nongravitational acceleration from sunlight, which gives an area-to-mass ratio of about 7e-5 m2/kg. Combining that with the diameter yields a density of roughly 3.9 g/cm3, within the range of rocky materials. A separate comparison with a model of near-Earth asteroid sources favors the inner Main Belt (88% probability) but does not exclude a lunar impact origin.

The paper's claims are mostly transparent about uncertainties, but the derived size and density depend on an assumed albedo and an assumed phase law for converting brightness to absolute magnitude, and the rotation period of about 2600 seconds is inferred from a short time series. The spectral match statement has a minor internal inconsistency between a figure caption and the reported chi-square values.

Extended reading notes

Core claim

2024 PT5 is a newly discovered minimoon, temporarily captured by the Earth-Moon system from 2024 September 29 to November 25 (~60 days, the shortest known capture, with no complete revolution), whose measured colors (g-r=0.58, r-i=0.29, i-z=-0.27) best match lunar rock samples and Sv-type asteroids, whose absolute magnitude 28.64±0.04 gives a diameter of 5.4±1.2 m for an assumed albedo of 0.21, and whose radiation-pressure-fitted area-to-mass ratio implies a density of 3.9±2.1 g/cm3, compatible with a rocky composition.

Load-bearing premise

The density result rests on the fitted area-to-mass ratio AMR=7.02±2.05e-5 m2/kg being a true radiation-pressure signal rather than an artifact of the assumed ~1-arcsec astrometric uncertainties or unmodeled systematic errors; the AMR is only a ~3.4-sigma detection and the density also scales with the assumed albedo (0.21) and the adopted phase function when converting photometry to H. If the astrometric error model or the albedo assumption is wrong, the derived diameter and density fail with it.

Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The paper's physical characterization relies on two assumed quantities (albedo and phase coefficient G), a fitted dynamical parameter (AMR), and several domain assumptions about phase functions, radiation-pressure modeling, population-model applicability, and color representativeness. It introduces no invented entities. The central minimoon discovery rests on standard astrometry and does not depend on these assumptions.

free parameters (3)
  • Visible geometric albedo pv = 0.21 (primary), 0.14 (lunar alternative), 0.1 (conservative)
    Diameter D=5.4±1.2 m and density 3.9±2.1 g/cm3 scale directly with the assumed albedo; albedo is not measured, only inferred from S-complex/lunar spectral analogs (§4).
  • Phase coefficient G = 0.2
    Used in the Bowell et al. (1988) phase function to compute H=28.64±0.04; the paper notes the H uncertainty is underestimated because the phase function is unknown (§3.2).
  • Area-to-mass ratio (AMR) = 7.02e-5 ± 2.05e-5 m2/kg
    Free parameter in the 7-parameter Find_Orb least-squares fit including solar radiation pressure; its value drives the density estimate (§3.1, Table 1).
assumptions (6)
  • domain assumption The H-G phase function (Bowell et al. 1988) with G=0.2 is valid for 2024 PT5 at phase angle 84.4 deg.
    Invoked in Eq. 1 (§3.2) to compute H; the paper cautions the H uncertainty is underestimated because the phase function is unknown.
  • domain assumption The only non-gravitational force needed to fit the orbit is solar radiation pressure acting through a constant area-to-mass ratio.
    Adopted in the Find_Orb least-squares fit (§3.1); any unmodeled nongravitational effect would change the fitted AMR and the density derived from it.
  • domain assumption The albedo of 2024 PT5 is represented by the S-complex value 0.21 (or lunar 0.14) from literature albedo distributions.
    Used in §4 to convert H into diameter D=5.4±1.2 m and then density; no thermal or polarimetric albedo measurement is available.
  • domain assumption The single-epoch g,r,i,Z colors are representative of the surface reflectance without significant phase-reddening or rotational color variation.
    The spectral classification in §3.2 and Fig. 5 relies on this; the observations were interspersed to mitigate rotation, but a single epoch at 84 deg phase cannot fully exclude phase reddening.
  • domain assumption The lightcurve amplitude maps to an axial ratio via b/a=10^(0.4A) with a≈c (prolate triaxial ellipsoid).
    Used in §3.3 to estimate a b/a~1.3 shape; the authors note the ratio may be exaggerated at high phase angle.
  • domain assumption The NEOMOD3 model's source probabilities apply to this single object, and the NEO albedo model (Morbidelli et al. 2020) can be weighted by those probabilities.
    Used in §4 to infer pv≈0.21 and an 88.4% ν6 source probability; this extrapolates a population-level model to an individual.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The discovery and characterization of minimoon 2024 PT$_5$." pith.science (2026). https://pith.science/paper/NZMVOTOF

@misc{pith2026241108029,
  author       = {Pith},
  title        = {Pith review of: The discovery and characterization of minimoon 2024 PT$_5$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NZMVOTOF}},
  note         = {Machine review of arXiv:2411.08029}
}
abstract

Minimoons are asteroids that become temporarily captured by the Earth-Moon system. We present the discovery of 2024 PT$_5$, a minimoon discovered by the Asteroid Terrestrial-impact Last Alert System (ATLAS) Sutherland telescope on 2024 August 7. The minimoon with heliocentric semi-major axis, $a$$\sim$1.01 au, and perihelion, $q$$\sim$0.99 au, became captured by the Earth-Moon system on 2024 September 29 and left on 2024 November 25 UTC. Visible g, r, i, and Z spectrophotometry was obtained using Gemini North/Gemini Multi-Object Spectrograph (GMOS) on 2024 September 27. The color indices are g-r = 0.58$\pm$0.04, r-i = 0.29$\pm$0.04, i-Z = -0.27$\pm$0.06, and the spectrum best matches lunar rock samples followed by S-complex asteroids. Assuming an albedo of 0.21 and using our measured absolute magnitude of 28.64$\pm$0.04, 2024 PT$_5$ has a diameter of 5.4$\pm$1.2 m. We also detect variations in the lightcurve of 2024 PT$_5$ with a 0.28$\pm$0.07 magnitude amplitude and a double-peaked period of $\sim$2600$\pm$500 s. We improve the orbital solution of 2024 PT$_5$ with our astrometry and estimate the effect of radiation pressure on its deriving an area-to-mass ratio of 7.02$\pm$2.05$\times$10$^{-5}$ m$^2$/kg, implying a density of $\sim$3.9$\pm$2.1 g/cm$^3$, compatible with having a rocky composition. If we assume 2024 PT$_5$ is from the NEO population, its most likely sources are resonances in the inner Main Belt by comparing its orbit with the NEO population model, though this does not exclude a lunar origin.

Figures

Figures reproduced from arXiv: 2411.08029 by the authors.

Figure 1
Figure 1. Panel a: The first of four o-band ATLAS-Sutherland telescope discovery images of 2024 PT5 from 2024 August 7 21:11:57 UTC. The asteroid moved at a rate of 34.3 arcminutes per hour (13.7 degrees per day) in the northwest direction. The asteroid makes a ∼9 pixel trail in the 30 s ATLAS exposures, indicated by the red circle. Panel b: the same as panel a but shows the image after subtracting static sources. Despite the… view at source ↗
Figure 2
Figure 2. Top left panel: a median combination stack of 11 x 75 s g filter images of 2024 PT5. An arrow indicating the width of 10′′ is shown for scale, and the cardinal directions are indicated. Top right panel: a median combination stack of 5 x 50 s r filter images of 2024 PT5. Bottom left panel: a median combination stack of 2 x 60 s i filter images of 2024 PT5. Bottom right panel: a median combination stack of 2 x 60 s Z … view at source ↗
Figure 3
Figure 3. Top panel: side view of the Earth co-rotating frame orbital trajectory of 2024 PT5 as it enters and leaves the Earth-Moon system between 2024 June and 2025 April in Cartesian Earth-Moon barycentric x and z coordinates. The daily position of 2024 PT5 is represented as blue points except the portion of its trajectory when it had eg<1 plotted in red. The position of the Earth is plotted with a cyan circle. The circular… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: a ∗ vs. i-z(Z) colors of 2024 PT5 plotted with a∗ vs. i-z colors of C, S and V type asteroids from (Ivezi´c et al. 2001; Juri´c et al. 2002), active comets (Solontoi et al. 2012), Kuiper Belt Objects (Ofek 2012), and bulk lunar rock samples (Isaacson et al. 2011). The …
Figure 5
Figure 5. Figure 5: Reflectance photometric spectrum of 2024 PT5 consisting of g, r, i, and Z observations of 2024 PT5 on 2024 September 27 UTC. The λeff locations of the g, r, i, and Z filters have been plotted as vertical dashed lines. The data points for the normalized reflectivity of …
Figure 6
Figure 6. Figure 6: Top panel: g filter lightcurve from 2024 September 27 GMOS observations of 2024 PT5. The error bars on the data points are equal to their 1 σ photometric uncertainties. A model lightcurve is plotted in black with a double-peaked period of ∼2600 s and amplitude of 0.28 …
Figure 7
Figure 7. Figure 7: Top panel: Lomb-Scargle periodogram of lightcurve period vs. spectral power (Lomb 1976) for the g filter data from the 2024 September 27 UTC Gemini N/GMOS observations. A peak in the power is located at single-peaked lightcurve period of 1320 s. Bottom panel: Phase dis…

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. On The Lunar Origin of Near-Earth Asteroid 2024 PT5

    astro-ph.EP 2024-12 accept novelty 6.0 of 10

    2024 PT5 is likely the second near-Earth object of lunar origin, identified by its Moon-like reflectance spectrum and natural, debris-free orbit.

Reference graph

Works this paper leans on

70 extracted references · 22 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ""...

  3. [3]

    - [1] #1 = = ^ ^ ^ .\!\!^ d .\!\!^ h .\!\!^ m .\!\!^ s .\!\!^ @mss

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    2017

  4. [4]

    P., Farinella , P., Zappal\`a , V., & Cellino , A

    Binzel , R. P., Farinella , P., Zappal\`a , V., & Cellino , A. 1989, in Asteroids II, ed. R. P. Binzel , T. Gehrels , & M. S. Matthews , 416--441

    work page 1989

  5. [5]

    P., Rivkin , A

    Binzel , R. P., Rivkin , A. S., Stuart , J. S., et al. 2004, , 170, 259, 10.1016/j.icarus.2004.04.004

    doi:10.1016/j.icarus.2004.04.004 2004

  6. [6]

    T., Ghosal , M., & Jedicke , R

    Bolin , B. T., Ghosal , M., & Jedicke , R. 2024, , 527, 1633, 10.1093/mnras/stad3227

    doi:10.1093/mnras/stad3227 2024

  7. [7]

    T., Noll , K

    Bolin , B. T., Noll , K. S., Caiazzo , I., Fremling , C., & Binzel , R. P. 2023, , 400, 115562, 10.1016/j.icarus.2023.115562

    arXiv 2023

  8. [8]

    T., Weaver , H

    Bolin , B. T., Weaver , H. A., Fernandez , Y. R., et al. 2018, , 852, L2, 10.3847/2041-8213/aaa0c9

    doi:10.3847/2041-8213/aaa0c9 2018

Show all 70 references
  1. [9]

    T., Fremling , C., Holt , T

    Bolin , B. T., Fremling , C., Holt , T. R., et al. 2020, , 900, L45, 10.3847/2041-8213/abae69

    2020 doi

  2. [10]

    T., Fernandez , Y

    Bolin , B. T., Fernandez , Y. R., Lisse , C. M., et al. 2021, , 161, 116, 10.3847/1538-3881/abd94b

    2021 doi

  3. [11]

    T., Ahumada , T., van Dokkum , P., et al

    Bolin , B. T., Ahumada , T., van Dokkum , P., et al. 2022, , 517, L49, 10.1093/mnrasl/slac089

    2022 doi

  4. [12]

    1988, Asteroids II, 399

    Bowell , E., Hapke , B., Domingue , D., et al. 1988, Asteroids II, 399

    1988

  5. [13]

    A., Connors , M., et al

    Brasser , R., Innanen , K. A., Connors , M., et al. 2004, , 171, 102, 10.1016/j.icarus.2004.04.019

    2004 doi

  6. [14]

    J., & Binzel , R

    Bus , S. J., & Binzel , R. P. 2002, Icarus, 158, 146, 10.1006/icar.2002.6856

    2002

  7. [15]

    2007, , 467, 777, 10.1051/0004-6361:20066514

    Casali , M., Adamson , A., Alves de Oliveira , C., et al. 2007, , 467, 777, 10.1051/0004-6361:20066514

    2007 doi

  8. [16]

    C., Magnier , E

    Chambers , K. C., Magnier , E. A., Metcalfe , N., et al. 2016, ArXiv e-prints. 1612.05560

    2016 arXiv

  9. [17]

    W., Binzel , R

    Delbo , M., Harris , A. W., Binzel , R. P., Pravec , P., & Davies , J. K. 2003, , 166, 116, 10.1016/j.icarus.2003.07.002

    2003 doi

  10. [18]

    E., Binzel , R

    DeMeo , F. E., Binzel , R. P., Slivan , S. M., & Bus , S. J. 2009, , 202, 160, 10.1016/j.icarus.2009.02.005

    2009 doi

  11. [19]

    E., & Carry , B

    DeMeo , F. E., & Carry , B. 2014, , 505, 629, 10.1038/nature12908

    2014 doi

  12. [20]

    2024, Minor Planet Electronic Circulars, 2024-P170

    Denneau , L., Siverd , R., Tonry , J., et al. 2024, Minor Planet Electronic Circulars, 2024-P170

    2024

  13. [21]

    M., et al

    Farnocchia , D., Reddy , V., Bauer , J. M., et al. 2022, , 3, 156, 10.3847/PSJ/ac7224

    2022 doi

  14. [22]

    2017, , 285, 83, 10.1016/j.icarus.2016.12.022

    Fedorets , G., Granvik , M., & Jedicke , R. 2017, , 285, 83, 10.1016/j.icarus.2016.12.022

    2017 doi

  15. [23]

    2020, , 160, 277, 10.3847/1538-3881/abc3bc

    Fedorets , G., Micheli , M., Jedicke , R., et al. 2020, , 160, 277, 10.3847/1538-3881/abc3bc

    2020 doi

  16. [24]

    E., et al

    Fukugita , M., Ichikawa , T., Gunn , J. E., et al. 1996, , 111, 1748, 10.1086/117915

    1996 doi

  17. [25]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  18. [26]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2018, , 616, A1, 10.1051/0004-6361/201833051

    2018 doi

  19. [27]

    J., Burns , J

    Gladman , B. J., Burns , J. A., Duncan , M. J., & Levison , H. F. 1995, , 118, 302, 10.1006/icar.1995.1193

    1995

  20. [28]

    2013, Earth's Temporarily-Captured Natural Satellites - The First Step towards Utilization of Asteroid Resources , ed

    Granvik , M., Jedicke , R., Bolin , B., Chyba , M., & Patterson , G. 2013, Earth's Temporarily-Captured Natural Satellites - The First Step towards Utilization of Asteroid Resources , ed. V. Badescu , 151--167

    2013

  21. [29]

    2017, , 598, A52, 10.1051/0004-6361/201629252

    Granvik , M., Morbidelli , A., Vokrouhlick \'y , D., et al. 2017, , 598, A52, 10.1051/0004-6361/201629252

    2017 doi

  22. [30]

    2012, , 218, 262, 10.1016/j.icarus.2011.12.003

    Granvik , M., Vaubaillon , J., & Jedicke , R. 2012, , 218, 262, 10.1016/j.icarus.2011.12.003

    2012 doi

  23. [31]

    2018, , 312, 181, 10.1016/j.icarus.2018.04.018

    Granvik , M., Morbidelli , A., Jedicke , R., et al. 2018, , 312, 181, 10.1016/j.icarus.2018.04.018

    2018 doi

  24. [32]

    2018, , 299, 84, 10.1016/j.icarus.2017.07.007

    Hanu s , J., Delbo , M., Al \' -Lagoa , V., et al. 2018, , 299, 84, 10.1016/j.icarus.2017.07.007

    2018 doi

  25. [33]

    2016, , 592, A34, 10.1051/0004-6361/201628666

    Hanu s , J., Delbo , M., Vokrouhlick \'y , D., et al. 2016, , 592, A34, 10.1051/0004-6361/201628666

    2016 doi

  26. [34]

    C., Warren , S

    Hewett , P. C., Warren , S. J., Leggett , S. K., & Hodgkin , S. T. 2006, , 367, 454, 10.1111/j.1365-2966.2005.09969.x

    2006

  27. [35]

    T., Irwin , M

    Hodgkin , S. T., Irwin , M. J., Hewett , P. C., & Warren , S. J. 2009, , 394, 675, 10.1111/j.1365-2966.2008.14387.x

    2009

  28. [36]

    M., J rgensen , I., Allington-Smith , J

    Hook , I. M., J rgensen , I., Allington-Smith , J. R., et al. 2004, , 116, 425, 10.1086/383624

    2004 doi

  29. [37]

    J., Pieters , C

    Isaacson , P. J., Pieters , C. M., Besse , S., et al. 2011, Journal of Geophysical Research (Planets), 116, E00G11, 10.1029/2010JE003731

    2011 doi

  30. [38]

    2001, , 122, 2749, 10.1086/323452

    Ivezi \'c , Z ., Tabachnik , S., Rafikov , R., et al. 2001, , 122, 2749, 10.1086/323452

    2001 doi

  31. [39]

    H., Juri \'c , M., et al

    Ivezi \'c , Z ., Lupton , R. H., Juri \'c , M., et al. 2002, , 124, 2943, 10.1086/344077

    2002 doi

  32. [40]

    T., Bottke , W

    Jedicke , R., Bolin , B. T., Bottke , W. F., et al. 2018, Frontiers in Astronomy and Space Sciences, 5, 13, 10.3389/fspas.2018.00013

    2018

  33. [41]

    2024, arXiv e-prints, arXiv:2411.10923, 10.48550/arXiv.2411.10923

    Jewitt , D. 2024, arXiv e-prints, arXiv:2411.10923, 10.48550/arXiv.2411.10923

    2024 doi arXiv

  34. [42]

    2024, Nature Astronomy, 8, 819, 10.1038/s41550-024-02258-z

    Jiao , Y., Cheng , B., Huang , Y., et al. 2024, Nature Astronomy, 8, 819, 10.1038/s41550-024-02258-z

    2024 doi

  35. [43]

    H., et al

    Juri \'c , M., Ivezi \'c , Z ., Lupton , R. H., et al. 2002, , 124, 1776, 10.1086/341950

    2002 doi

  36. [44]

    S., Macke , R

    Kiefer , W. S., Macke , R. J., Britt , D. T., Irving , A. J., & Consolmagno , G. J. 2012, , 39, L07201, 10.1029/2012GL051319

    2012 doi

  37. [45]

    2008, LPI Contributions, 1405, 8297

    Kwiatkowski , T., Kryszczynska , A., Polinska , M., et al. 2008, LPI Contributions, 1405, 8297

    2008

  38. [46]

    2023, Research Notes of the American Astronomical Society, 7, 214, 10.3847/2515-5172/ad0044

    Labrie , K., Simpson , C., Cardenes , R., et al. 2023, Research Notes of the American Astronomical Society, 7, 214, 10.3847/2515-5172/ad0044

    2023 doi

  39. [47]

    Lomb , N. R. 1976, , 39, 447, 10.1007/BF00648343

    1976 doi

  40. [48]

    J., Britt , D

    Macke , R. J., Britt , D. T., & Consolmagno , G. J. 2011, , 46, 311, 10.1111/j.1945-5100.2010.01155.x

    2011

  41. [49]

    2008, , 47, 4981, 10.1364/AO.47.004981

    Matthews , G. 2008, , 47, 4981, 10.1364/AO.47.004981

    2008 doi

  42. [50]

    J., & Elliott , G

    Micheli , M., Tholen , D. J., & Elliott , G. T. 2012, , 17, 446, 10.1016/j.newast.2011.11.008

    2012 doi

  43. [51]

    2013, , 226, 251, 10.1016/j.icarus.2013.05.032

    ---. 2013, , 226, 251, 10.1016/j.icarus.2013.05.032

    2013 doi

  44. [52]

    L., Farnocchia , D., et al

    Mommert , M., Hora , J. L., Farnocchia , D., et al. 2014, , 786, 148, 10.1088/0004-637X/786/2/148

    2014 doi

  45. [53]

    Morais , M. H. M., & Morbidelli , A. 2002, , 160, 1, 10.1006/icar.2002.6937

    2002

  46. [54]

    2020, , 340, 113631, 10.1016/j.icarus.2020.113631

    Morbidelli , A., Delbo , M., Granvik , M., et al. 2020, , 340, 113631, 10.1016/j.icarus.2020.113631

    2020

  47. [55]

    P., Micheli , M., Farnocchia , D., et al

    Naidu , S. P., Micheli , M., Farnocchia , D., et al. 2021, , 913, L6, 10.3847/2041-8213/abf836

    2021 doi

  48. [56]

    F., et al

    Nesvorn \'y , D., Deienno , R., Bottke , W. F., et al. 2023, , 166, 55, 10.3847/1538-3881/ace040

    2023 doi

  49. [57]

    2024, , 417, 116110, 10.1016/j.icarus.2024.116110

    Nesvorn \'y , D., Vokrouhlick \'y , D., Shelly , F., et al. 2024, , 417, 116110, 10.1016/j.icarus.2024.116110

    2024

  50. [58]

    Ofek, E. O. 2012, The Astrophysical Journal, 749, 10

    2012

  51. [59]

    2012, Astrometrica: Astrometric data reduction of CCD images

    Raab , H. 2012, Astrometrica: Astrometric data reduction of CCD images . 1203.012

    2012

  52. [60]

    Russell , H. N. 1916, , 43, 173, 10.1086/142244

    1916 doi

  53. [61]

    Sharkey , B. N. L., Reddy , V., Malhotra , R., et al. 2021, Communications Earth and Environment, 2, 231, 10.1038/s43247-021-00303-7

    2021 doi

  54. [62]

    2012, , 218, 571, 10.1016/j.icarus.2011.10.008

    Solontoi , M., Ivezi \'c , Z ., Juri \'c , M., et al. 2012, , 218, 571, 10.1016/j.icarus.2011.10.008

    2012 doi

  55. [63]

    Stellingwerf , R. F. 1978, , 224, 953, 10.1086/156444

    1978 doi

  56. [64]

    A., Trilling , D

    Thomas , C. A., Trilling , D. E., Emery , J. P., et al. 2011, , 142, 85, 10.1088/0004-6256/142/3/85

    2011 doi

  57. [65]

    L., Stubbs , C

    Tonry , J. L., Stubbs , C. W., Lykke , K. R., et al. 2012, , 750, 99, 10.1088/0004-637X/750/2/99

    2012 doi

  58. [66]

    L., Denneau , L., Heinze , A

    Tonry , J. L., Denneau , L., Heinze , A. N., et al. 2018, , 130, 064505, 10.1088/1538-3873/aabadf

    2018 doi

  59. [67]

    2015, , 261, 34, 10.1016/j.icarus.2015.08.007

    Vere s , P., Jedicke , R., Fitzsimmons , A., et al. 2015, , 261, 34, 10.1016/j.icarus.2015.08.007

    2015 doi

  60. [68]

    R., & Chamberlin , A

    Vere s , P., Farnocchia , D., Chesley , S. R., & Chamberlin , A. B. 2017, , 296, 139, 10.1016/j.icarus.2017.05.021

    2017 doi

  61. [69]

    Williams , G. V. 2024, Minor Planet Electronic Circulars, 2024-V67

    2024

  62. [70]

    M., Fulchignoni , M., & Lupishko , D

    Zappala , V., Cellino , A., Barucci , A. M., Fulchignoni , M., & Lupishko , D. F. 1990, , 231, 548

    1990

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.