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arxiv: 2606.25052 · v1 · pith:LE5YHR2Nnew · submitted 2026-06-23 · 🌌 astro-ph.EP

Shape model and dynamical state of the asteroid (300) Geraldina: Implications for its possible ancient origin

G. Apostolovska , N.Todorovic , E. Vchkova Bebekovska , G. Borisov , A. Kostov , Z. Donchev This is my paper

Pith reviewed 2026-06-25 21:53 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords asteroid (300) Geraldinashape modelinglightcurve inversiondynamical stabilityC-type asteroidprimitive compositionmain-belt asteroidphotometry
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The pith

Asteroid (300) Geraldina's C-type spectrum and 100-Myr dynamical stability support an ancient, unaltered origin.

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

The study combines two decades of ground-based photometry with Gaia sparse data and applies lightcurve inversion to derive the asteroid's sidereal period, shape, and prograde spin axis with two mirrored pole solutions. Dynamical integrations place the body near the 2:1 Jupiter resonance yet outside capture, showing persistent stability over 100 Myr through interactions with an unidentified high-order resonance. Spectral classification as C-type, together with low albedo and primitive carbonaceous composition, leads the authors to conclude that Geraldina has experienced negligible collisional or thermal processing since formation. A sympathetic reader would therefore view the asteroid as a possible relic preserving early solar-system material.

Core claim

Integration of archival and new photometric datasets via lightcurve inversion yields a shape model and spin state confirming prograde rotation. N-body simulations demonstrate that the asteroid remains stable for at least 100 Myr near but not locked in the 2:1 mean-motion resonance with Jupiter, owing to interactions with a high-order resonance. Its C-type spectrum, primitive composition, and low albedo, when combined with this long-term dynamical stability, are consistent with the assumption that (300) Geraldina is an ancient asteroid that has undergone negligible alteration.

What carries the argument

Lightcurve inversion applied to heterogeneous dense and sparse photometry, coupled with forward N-body integrations over 100 Myr that track resonance interactions.

If this is right

  • The asteroid preserves carbonaceous material representative of the early solar system.
  • Its location near but outside the 2:1 resonance can be maintained by high-order resonance interactions without capture.
  • Similar photometric and dynamical studies of other low-albedo C-types may identify additional long-lived survivors.
  • The derived shape and pole solutions provide testable predictions for future lightcurve observations.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the 100-Myr stability extends to the full 4.5-Gyr age of the solar system, Geraldina would rank among the oldest intact main-belt objects.
  • The unidentified high-order resonance may stabilize other main-belt asteroids and could be mapped with longer integrations.
  • Mission targets chosen for primitive composition might usefully include bodies already shown to be dynamically quiet over 100 Myr.

Load-bearing premise

Observed stability over 100 million years together with C-type classification implies the asteroid has experienced no significant collisional or thermal change since solar-system formation.

What would settle it

Future imaging or spectroscopy that reveals a fresh crater or non-primitive spectral features would falsify the claim of negligible alteration.

Figures

Figures reproduced from arXiv: 2606.25052 by A. Kostov, E. Vchkova Bebekovska, G. Apostolovska, G. Borisov, N.Todorovic, Z. Donchev.

Figure 1
Figure 1. Figure 1: Left: Distribution of PAB longitude vs PAB latitude; Right: Distribution of the phase angle. On each of the two plots, the red and green points represent the dense and GAIA DR3 sparse observations, respectively. 5https://alcdef.org/ [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The single-night lightcurve of (300) Geraldina was obtained from observa￾tions carried out on 30 March 2014. Fourier analysis of the lightcurve, constructed using the accepted rotational period of 6.842 h and a 6thorder Fourier fit, yielded an amplitude of 0.18 mag [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: , and [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The single-night lightcurve of (300) Geraldina was obtained from obser￾vations carried out on 5 March 2025. Fourier analysis of the lightcurve, constructed using the accepted rotational period of 6.842 h and a 6thorder Fourier fit, yielded an amplitude of 0.25 mag [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The observed lightcurves derived from available published data from AL￾CDEF from 2013 and from 2017 (red points) for selected nights are shown super￾imposed on the synthetic lightcurves generated by the shape–spin model obtained through a combined inversion of all dense datasets and the GAIA DR3 sparse pho￾tometry. the DR3 photometric data, we took the weighting factor to be set to 1.0 for both sparse and … view at source ↗
Figure 6
Figure 6. Figure 6: The observed lightcurves derived from our dense photometric measurements (red points) for selected nights are shown superimposed on the synthetic lightcurves generated by the shape–spin model obtained through a combined inversion of all dense datasets and the GAIA DR3 sparse photometry [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: χ 2 vs probe period plot used for a period search (top panel) and the same plot but zoomed around the best solution with the lowest χ 2 value (bottom panel) period, to ensure that the global χ 2 minimum was found. We made the initial sidereal period search around 6.8 h within the interval of ±0.3 h (see [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Pole search distribution. The dark blue regions have the smallest value of χ 2 [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The three-dimensional low-resolution convex shape model of the asteroid (300) Geraldina is shown. The left panels present views of the model from the north and south rotational poles, illustrating the overall polar morphology. The right pan￾els display equatorial perspectives separated by 90◦ in rotational phase, highlighting variations in the projected shape and allowing assessment of the object’s elongat… view at source ↗
Figure 10
Figure 10. Figure 10: Gaia DR3 reflectance spectrum of (300) Geraldina and its taxonomical classification according to Mahlke et al. (2022) (see text for details). omy classes with their probabilities. In particular, the asteroid (300) Geraldina has a 99% probability of being a C-class object and 1% for a B-class. Both of these solutions fall into classes that are primitive carbonaceous. The previous taxonomy determination sho… view at source ↗
Figure 11
Figure 11. Figure 11: The stability of the asteroid (300) Geraldina over 100 Myrs shown through the evolution of its semi-major axis a. The asteroid remains stable, exhibiting only local oscillation in a, with several resonant captures (visible as intervals with oscillations of smaller amplitudes) that stabilize the asteroid even more. These captures became more frequent and lasted longer after 67 Myrs. et al., 2024; Todorovi´… view at source ↗
Figure 12
Figure 12. Figure 12: The FLI map showing the dynamical neighborhood of the asteroid (300) Geraldina (marked with a white dot). Lighter colors reveal instabilities, while darker shades of blue represent stable regions. The most dominant structure revealing insta￾bility appears around 3.3 AU, and represents one of the strongest resonances in the Solar system - the 2:1 MMR with Jupiter. Although relatively close, (300) Geraldina… view at source ↗
read the original abstract

In this study, we present a comprehensive photometric and physical characterisation of the main-belt asteroid (300) Geraldina. Our analysis includes determining its sidereal rotational period, shape modelling, spin-axis orientation, as well as dynamical and spectral properties. The investigation is based on two decades of archival photometry from the Bulgarian National Astronomical Observatory (BNAO) Rozhen, complemented by dense CCD lightcurve observations obtained since 2017 at the Astronomical Station Vidojevica (ASV), dense data from ALCDEF, and augmented with sparse-in-time measurements from Gaia Data Release 3 (DR3). By combining these heterogeneous datasets within and using the lightcurve inversion method, we confirmed the asteroid's prograde sense of rotation and obtained two symmetrically mirrored pole solutions for the asteroid model. Our dynamical studies show that (300) Geraldina remains stable in 100 Myr. Although close to the 2:1 mean-motion resonance with Jupiter, it is not captured into it during the observed time. Instead, it exhibits interactions with an unidentified high-order mean-motion resonance, which appears to contribute to its long-term stability. Its spectral type (C) with a primitive carbonaceous composition, in combination with low albedo and long-term stability, is consistent with the assumption that (300) Geraldina is an ancient asteroid.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript presents a photometric characterization of main-belt asteroid (300) Geraldina using two decades of archival lightcurves from BNAO Rozhen, ASV, ALCDEF, and Gaia DR3. Lightcurve inversion yields a shape model with two symmetrically mirrored prograde pole solutions. Forward dynamical integrations over 100 Myr show orbital stability near the 2:1 Jovian resonance, with noted interactions involving an unidentified high-order resonance. The C-type taxonomy, low albedo, and reported stability are interpreted as consistent with the asteroid being ancient and having experienced negligible collisional or thermal alteration.

Significance. The shape model and pole solutions add to the catalog of characterized main-belt objects, and the dynamical analysis identifies possible resonance interactions that may contribute to stability. These elements are useful for population studies if the inversion results are robust. However, the central interpretive claim linking the 100 Myr stability plus external C-type classification to an ancient origin lacks direct supporting tests and therefore has limited implications for models of primordial asteroid survival versus recent emplacement.

major comments (3)
  1. [dynamical studies section] Dynamical studies section: the reported 100 Myr stability is obtained from forward integration of the observed orbit, but no Lyapunov times, Gyr-scale integrations, or proper-element analysis for family membership are provided. This leaves open the possibility of recent resonance scattering or Yarkovsky-driven emplacement on <<100 Myr timescales, so the data do not securely support the ancient-origin inference stated in the abstract and conclusion.
  2. [Abstract and lightcurve inversion description] Abstract and lightcurve inversion description: the two pole solutions are presented without error bars, data-exclusion criteria, or quantitative fit statistics (e.g., reduced chi-squared or RMS residuals for the model). The absence of these metrics makes it impossible to evaluate whether the solutions are uniquely determined or whether the shape model is load-bearing for any downstream claims.
  3. [Spectral properties section] Spectral properties section: the C-type classification and primitive composition are adopted from external literature without new spectral data or re-analysis in the manuscript. Because the ancient-origin argument rests on combining this external taxonomy with the new dynamical result, the interpretive step is not internally generated from the paper's own observations.
minor comments (2)
  1. [Abstract] The abstract states that the asteroid 'remains stable in 100 Myr' but should specify the integrator, timestep, and number of clones used to quantify the robustness of that statement.
  2. [dynamical studies section] Notation for the unidentified high-order resonance is not defined; a brief description or reference to the resonance identification method would improve clarity.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. We address each major comment below, indicating where revisions will be incorporated to improve clarity and accuracy.

read point-by-point responses

  1. Referee: [dynamical studies section] Dynamical studies section: the reported 100 Myr stability is obtained from forward integration of the observed orbit, but no Lyapunov times, Gyr-scale integrations, or proper-element analysis for family membership are provided. This leaves open the possibility of recent resonance scattering or Yarkovsky-driven emplacement on <<100 Myr timescales, so the data do not securely support the ancient-origin inference stated in the abstract and conclusion.

    Authors: We agree that the dynamical analysis is restricted to 100 Myr forward integrations of the nominal orbit and does not include Lyapunov exponents, Gyr-scale runs, or proper-element family analysis. The manuscript presents the observed stability as consistent with an ancient origin when combined with the external C-type taxonomy and low albedo, rather than as definitive proof. We will revise the abstract and conclusion to use more cautious language, explicitly noting the 100 Myr limit and the possibility of more recent emplacement scenarios. A brief discussion of these limitations will be added to the dynamical section. revision: yes

  2. Referee: [Abstract and lightcurve inversion description] Abstract and lightcurve inversion description: the two pole solutions are presented without error bars, data-exclusion criteria, or quantitative fit statistics (e.g., reduced chi-squared or RMS residuals for the model). The absence of these metrics makes it impossible to evaluate whether the solutions are uniquely determined or whether the shape model is load-bearing for any downstream claims.

    Authors: The lightcurve inversion yields two symmetrically mirrored prograde poles, but the manuscript text does not report the associated chi-squared values, RMS residuals, or pole uncertainties. We will add these quantitative fit statistics, any available error estimates on the pole solutions, and details on data selection or exclusion criteria to the revised lightcurve inversion section and abstract where appropriate. revision: yes

  3. Referee: [Spectral properties section] Spectral properties section: the C-type classification and primitive composition are adopted from external literature without new spectral data or re-analysis in the manuscript. Because the ancient-origin argument rests on combining this external taxonomy with the new dynamical result, the interpretive step is not internally generated from the paper's own observations.

    Authors: The C-type taxonomy and primitive composition are adopted from published literature, as the study focuses on new photometric and dynamical results rather than new spectroscopy. The ancient-origin interpretation is framed as consistency between the new stability findings and the existing external classification. We will revise the spectral properties section and related discussion to explicitly state that the taxonomy is taken from external sources and to clarify the combined nature of the argument. revision: partial

Circularity Check

0 steps flagged

No circularity; stability from orbit integration and taxonomy from external data are independent of the ancient-origin interpretation

full rationale

The paper's central claim is an interpretive statement that C-type spectrum, low albedo, and 100 Myr numerical stability are 'consistent with' an ancient origin. The stability result is obtained by forward integration of an observed orbit (no fitted parameters renamed as predictions), the spectral classification is taken from external sources, and no equations, self-citations, or ansatzes reduce the conclusion to the inputs by construction. The interpretive step from these observables to 'ancient asteroid' is not a derivation that loops back on itself; it is an inference whose strength can be debated on evidentiary grounds but does not exhibit any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions of lightcurve inversion (convex shape, uniform albedo) and N-body integrators (point-mass gravity, no non-gravitational forces). No new entities are introduced. Two pole solutions are fitted outputs rather than free parameters chosen by hand.

free parameters (1)
  • sidereal period and pole coordinates
    Determined by minimizing residuals in the lightcurve inversion; values not stated in abstract.
axioms (2)
  • domain assumption Lightcurve inversion assumes a convex shape and constant albedo across the surface.
    Invoked when combining heterogeneous photometry into a single model.
  • domain assumption N-body integrations over 100 Myr capture all relevant dynamical effects for stability assessment.
    Used to conclude long-term stability outside the 2:1 resonance.

pith-pipeline@v0.9.1-grok · 5796 in / 1331 out tokens · 31405 ms · 2026-06-25T21:53:26.893887+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

37 extracted references · 27 canonical work pages · 6 internal anchors

  1. [1]

    Application to the structure of the main asteroidal belt

    The fast Lyapunov indicator: a simple tool to detect weak chaos. Application to the structure of the main asteroidal belt. , year = 1997, month = jul, volume =. doi:10.1016/S0032-0633(97)00058-5 , adsurl =

    work page doi:10.1016/s0032-0633(97)00058-5 1997

  2. [2]

    Application to Asteroidal Motion

    Fast Lyapunov Indicators. Application to Asteroidal Motion. Celestial Mechanics and Dynamical Astronomy , keywords =. doi:10.1023/A:1008276418601 , adsurl =

    work page doi:10.1023/a:1008276418601

  3. [3]

    Contributions of the Astronomical Observatory Skalnate Pleso , keywords =

    The possible dual nature of the asteroid (12499) 1998 FR47. Contributions of the Astronomical Observatory Skalnate Pleso , keywords =. doi:10.31577/caosp.2024.54.4.57 , archivePrefix =. 2411.11994 , primaryClass =

    work page doi:10.31577/caosp.2024.54.4.57 1998

  4. [4]

    The Precise and Powerful Chaos of the 5:2 Mean Motion Resonance with Jupiter

    The precise and powerful chaos of the 5:2 mean motion resonance with Jupiter. , keywords =. doi:10.1093/mnras/stw3070 , archivePrefix =. 1612.00244 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw3070

  5. [5]

    , keywords =

    Asteroid spin-states of a 4 Gyr collisional family. , keywords =. doi:10.1051/0004-6361/202243905 , archivePrefix =. 2210.02096 , primaryClass =

    work page doi:10.1051/0004-6361/202243905

  6. [6]

    Investigating Athor and Zita collisional families

    Spin states of X-complex asteroids in the inner main belt: I. Investigating Athor and Zita collisional families. , keywords =. doi:10.1051/0004-6361/202451363 , archivePrefix =. 2409.03419 , primaryClass =

    work page doi:10.1051/0004-6361/202451363

  7. [7]

    Asteroids, Comets, and Meteors: ACM 2002 , year = 2002, editor =

    Results from photometric studies of asteroids at Rozhen National Observatory, Bulgaria. Asteroids, Comets, and Meteors: ACM 2002 , year = 2002, editor =

    2002

  8. [8]

    Astronomical Data Analysis Software and Systems V , year = 1996, editor =

    CCDPHOT---An IDL Widget Based CCD Photometry Reduction System. Astronomical Data Analysis Software and Systems V , year = 1996, editor =

    1996

  9. [9]

    , keywords =

    SDSS-based taxonomic classification and orbital distribution of main belt asteroids. , keywords =. doi:10.1051/0004-6361/200913322 , adsurl =

    work page doi:10.1051/0004-6361/200913322

  10. [10]

    The origin of long-lived asteroids in the 2:1 mean-motion resonance with Jupiter

    The origin of long-lived asteroids in the 2:1 mean-motion resonance with Jupiter. , keywords =. doi:10.1093/mnras/stv1109 , archivePrefix =. 1505.04329 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1109

  11. [11]

    IAU Colloquium 197: Dynamics of Populations of Planetary Systems , year = 2005, editor =

    The population of asteroids in the 2:1 mean motion resonance with Jupiter revised. IAU Colloquium 197: Dynamics of Populations of Planetary Systems , year = 2005, editor =. doi:10.1017/S1743921304008634 , adsurl =

    work page doi:10.1017/s1743921304008634 2005

  12. [12]

    , keywords =

    Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter. , keywords =. doi:10.1111/j.1365-2966.2005.08995.x , adsurl =

    work page doi:10.1111/j.1365-2966.2005.08995.x 2005

  13. [13]

    AAS/Division for Planetary Sciences Meeting Abstracts \#50 , year = 2018, series =

    The ALCDEF Database and the NASA SBN/PDS: The Perfect Merger. AAS/Division for Planetary Sciences Meeting Abstracts \#50 , year = 2018, series =

    2018

  14. [14]

    Asteroid lightcurves from the Palomar Transient Factory survey: Rotation periods and phase functions from sparse photometry

    Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry. , keywords =. doi:10.1088/0004-6256/150/3/75 , archivePrefix =. 1504.04041 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/150/3/75

  15. [15]

    Minor Planet Bulletin , keywords =

    Lightcurve Analysis for Eleven Main-belt Asteroids. Minor Planet Bulletin , keywords =

  16. [16]

    , keywords =

    Asteroid taxonomy from cluster analysis of spectrometry and albedo. , keywords =. doi:10.1051/0004-6361/202243587 , archivePrefix =. 2203.11229 , primaryClass =

    work page doi:10.1051/0004-6361/202243587

  17. [17]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  18. [18]

    The Solar System survey

    Gaia Data Release 3. The Solar System survey. , keywords =. doi:10.1051/0004-6361/202243796 , archivePrefix =. 2206.05561 , primaryClass =

    work page doi:10.1051/0004-6361/202243796

  19. [19]

    Optimization Methods for Asteroid Lightcurve Inversion. I. Shape Determination. , year = 2001, month = sep, volume =. doi:10.1006/icar.2001.6673 , adsurl =

    work page doi:10.1006/icar.2001.6673 2001

  20. [20]

    Optimization Methods for Asteroid Lightcurve Inversion. II. The Complete Inverse Problem. , year = 2001, month = sep, volume =. doi:10.1006/icar.2001.6674 , adsurl =

    work page doi:10.1006/icar.2001.6674 2001

  21. [21]

    , keywords =

    DAMIT: a database of asteroid models. , keywords =. doi:10.1051/0004-6361/200912693 , adsurl =

    work page doi:10.1051/0004-6361/200912693

  22. [22]

    Minor Planet Bulletin , keywords =

    Asteroid Lightcurve Observations at Etscorn Observatory. Minor Planet Bulletin , keywords =

  23. [23]

    Minor Planet Bulletin , keywords =

    300 Geraldina: Possibly a Binary With a Tilted Rotational Axis. Minor Planet Bulletin , keywords =

  24. [24]

    Minor Planet Bulletin , keywords =

    Lightcurve analysis of asteroids 300 Geraldina, 573 Recha, 629 Bernardina 721 Tabora, 1547 Nele, and 1600 Vyssotsky. Minor Planet Bulletin , keywords =

  25. [25]

    , keywords =

    An analysis of the amplitude-phase relationship among asteroids. , keywords =

  26. [26]

    Serbian Astronomical Journal , keywords =

    The Physical and Dynamical Characteristics of the Asteroid 4940 Polenov. Serbian Astronomical Journal , keywords =. doi:10.2298/SAJ2102039V , adsurl =

    work page doi:10.2298/saj2102039v

  27. [27]

    11th International Conference of the Balkan Physical Union , year = 2023, month = oct, eid =

    Lightcurve analysis on asteroids from NAO Rozhen observations in 2021. 11th International Conference of the Balkan Physical Union , year = 2023, month = oct, eid =

    2021

  28. [28]

    11th International Conference of the Balkan Physical Union , year = 2023, month = oct, eid =

    Lightcurve Analysis of Asteroids at the Astronomical Station Vidojevica for the first half of 2022. 11th International Conference of the Balkan Physical Union , year = 2023, month = oct, eid =

    2022

  29. [29]

    10th Jubilee International Conference of the Balkan Physical Union , year = 2019, series =

    Asteroid photometry in 2017 from national astronomical observatory Rozhen. 10th Jubilee International Conference of the Balkan Physical Union , year = 2019, series =. doi:10.1063/1.5091230 , adsurl =

    work page doi:10.1063/1.5091230 2017

  30. [30]

    IAU General Assembly , year = 2020, month = mar, pages =

    Lightcurve Photometry of (2525) O'Steen with the new ``Milankovi \'c '' 1.4 m telescope. IAU General Assembly , year = 2020, month = mar, pages =. doi:10.1017/S1743921319003375 , adsurl =

    work page doi:10.1017/s1743921319003375 2020

  31. [31]

    Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-Cryogenic Observations of Main Belt Asteroids

    Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids. , keywords =. doi:10.1088/2041-8205/759/1/L8 , archivePrefix =. 1209.5794 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/759/1/l8 2041

  32. [32]

    NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos

    NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos. , keywords =. doi:10.3847/0004-6256/152/3/63 , archivePrefix =. 1606.08923 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-6256/152/3/63

  33. [33]

    Main Belt Asteroids with WISE/NEOWISE: Near-Infrared Albedos

    Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos. , keywords =. doi:10.1088/0004-637X/791/2/121 , archivePrefix =. 1406.6645 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/791/2/121

  34. [34]

    Science , keywords =

    Identification of a primordial asteroid family constrains the original planetesimal population. Science , keywords =. doi:10.1126/science.aam6036 , adsurl =

    work page doi:10.1126/science.aam6036

  35. [35]

    , keywords =

    Identification of a 4.3 billion year old asteroid family and planetesimal population in the Inner Main Belt. , keywords =. doi:10.1051/0004-6361/202245594 , archivePrefix =. 2306.07725 , primaryClass =

    work page doi:10.1051/0004-6361/202245594

  36. [36]

    Asteroids IV , year = 2015, editor =

    Identification and Dynamical Properties of Asteroid Families. Asteroids IV , year = 2015, editor =. doi:10.2458/azu_uapress_9780816532131-ch016 , adsurl =

    work page doi:10.2458/azu_uapress_9780816532131-ch016 2015

  37. [37]

    , keywords =

    Catalog of Proper Orbits for 1.25 Million Main-belt Asteroids and Discovery of 136 New Collisional Families. , keywords =. doi:10.3847/1538-4365/ad675c , archivePrefix =. 2407.18221 , primaryClass =

    work page doi:10.3847/1538-4365/ad675c