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arxiv: 2606.17734 · v1 · pith:U54U7CDGnew · submitted 2026-06-16 · 🌌 astro-ph.EP · astro-ph.IM

Shape, Orientation and Colors Combined approach for Asteroids (SOCCA)

K. O. Xenos , B. Carry , J. Peloton , M. Mahlke , J. Berthier , P.-A. Mattei This is my paper

Pith reviewed 2026-06-26 23:05 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IM
keywords asteroidsphotometryphase functionshape modelingrotation periodtriaxial ellipsoidmulti-band datasparse observations
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The pith

SOCCA extends the HG1G2 phase function with the projected area of a rotating triaxial ellipsoid to jointly recover asteroid absolute magnitude, phase parameters, spin state and shape ratios from sparse multi-band photometry.

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

The paper introduces SOCCA to fit sparse photometric observations of solar system objects while accounting for rotational brightness changes that standard models ignore. It does so by adding the changing projected silhouette of a triaxial ellipsoid to the usual HG1G2 brightness description and fitting all parameters together across bands. The approach recovers sidereal periods, pole orientations and axis ratios in addition to the usual magnitude and phase coefficients. On both simulated LSST data and real observations of (45) Eugenia the model cuts mean residuals in half and shrinks scatter in derived magnitudes and phase slopes by roughly a factor of three. The combined fit also raises the fraction of solutions judged physically plausible by 10-20 percent per filter.

Core claim

SOCCA jointly fits multi-band photometry by extending the HG1G2 formalism with the projected surface of a rotating triaxial ellipsoid; the model recovers the absolute magnitude, phase parameters, sidereal rotation period, spin-axis orientation and the three axes ratios of the best-fitting ellipsoid while remaining computationally tractable for large surveys.

What carries the argument

The SOCCA model, an extension of the HG1G2 phase function that multiplies the usual brightness term by the instantaneous projected area of a rotating triaxial ellipsoid whose surface albedo is uniform within each band.

If this is right

  • Mean photometric residuals drop by half relative to standard HG1G2 fits.
  • Scatter in retrieved absolute magnitudes is reduced by a factor of about three.
  • Phase-slope parameters are determined with comparable improvement in precision.
  • Sidereal periods, pole directions and ellipsoid axis ratios are recovered as additional outputs.
  • The fraction of solutions meeting physical plausibility criteria rises by 10-20 percent per filter, yielding an overall 53 percent success rate.

Where Pith is reading between the lines

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

  • The method can be run on existing ZTF or ATLAS archives without new observations.
  • Joint color and shape solutions may tighten constraints on surface composition when combined with spectroscopic surveys.
  • Because the model is linear in the projected-area term, it can be extended to include light-curve inversion once denser sampling becomes available.

Load-bearing premise

Brightness changes are produced solely by the changing projected area of a uniform-albedo triaxial ellipsoid rotating about a fixed axis.

What would settle it

Direct comparison of SOCCA-derived shapes and poles against independent high-resolution models obtained from radar or spacecraft flybys for a sample of ten or more asteroids with known periods.

Figures

Figures reproduced from arXiv: 2606.17734 by B. Carry, J. Berthier, J. Peloton, K. O. Xenos, M. Mahlke, P.-A. Mattei.

Figure 1
Figure 1. Figure 1: Comparison of the behavior of shape function [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Dependence of SOCCA on its parameters illustrated with (45) Eugenia. All but the sidereal periods have a smooth convergence to the best-fitting values. ity in these residuals, using Lomb-Scargle frequency anal￾ysis (Lomb 1976; Scargle 1982). It is non-trivial and cau￾tion must be applied. First, previous works have shown the strong effect of the observational cadence on the determi￾nation of rotation perio… view at source ↗
Figure 3
Figure 3. Figure 3: Difference between the second and third highest pe [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Procedure for defining the synodic-sidereal period window and the number of resolvable period intervals as a [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the RMS between the different photo [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the simulated and retrieved periods for each simulated SSO. [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Inversion time as a function of the number of obser [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Input versus output spin axis obliquity of the sam [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Purity and completeness as a function of the boot [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 8
Figure 8. Figure 8: Difference between the simulated and computed [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 11
Figure 11. Figure 11: Comparison between the sampled and retrieved axis ratios [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Comparison between SOCCA, HG1G2 and sHG1G2 model fitting for (45) Eugenia. The large panels show the model prediction versus the obervations obtained by ZTF in the g filter over the approximately 10 year baseline and the smaller panels show the difference between the model prediction and the observations. On the top pair of panels the SOCCA- HG1G2 comparison is shown and on the bottom pair, we show the SO… view at source ↗
Figure 13
Figure 13. Figure 13: Comparison between the densely sampled lightcurves of (45) Eugenia and the SOCCA model of the same SSO propagated to the dates of observation. Top: This lightcurve (Hanuš et al. 2016) was captured near the observational midpoint of the data used to build the SOCCA model and is therefore reproduced well. Center: This lightcurve (Marchis et al. 2010) was captured under a certain object-observer orientation,… view at source ↗
read the original abstract

Large photometric surveys provide sparse multi-band photometry for millions of Solar System objects, offering an opportunity to jointly constrain their physical and compositional properties. However, current phase function models do not account for rotational variability, limiting their ability to retrieve accurate parameters. Similarly, methods that recover shape and rotational parameters remain both computationally and observationally expensive. We present a model capable of simultaneously retrieving the absolute magnitude, phase parameters, spin state, and shape proportions of SSOs from sparse photometric data, while remaining computationally efficient. We introduce the Shape, Orientation and Colors Combined approach for Asteroids (SOCCA), which extends the HG1G2 formalism by incorporating the projected surface of a rotating triaxial ellipsoid. The model jointly fits multi-band photometry, and includes a dedicated treatment of rotational period determination. We implement the model on a 10-year LSST simulation as well as on real data of asteroid (45) Eugenia for validation purposes. SOCCA significantly improves the fit to photometric data, reducing the mean residuals to half, compared to previous models. It retrieves the absolute magnitude with a scatter about three times smaller than existing approaches, and improves the determination of phase parameters by a similar factor. It also recovers the sidereal rotation period, spin axis orientation and the axes ratios of the best fitting ellipsoid. The inclusion of shape and rotation increases the number of physically meaningful solutions by 10-20% per filter, leading to an overall success rate of 53%. Its performance and scalability make it well suited for current and upcoming large surveys such as the Zwicky Transient Facility and the recently started Legacy Survey of Space and Time.

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 introduces SOCCA, an extension of the HG1G2 phase-function formalism that multiplies the phase term by the projected area of a rotating triaxial ellipsoid whose surface is uniform except for a per-band scale factor. The model jointly fits sparse multi-band photometry to recover absolute magnitude H, phase parameters G1/G2, sidereal period, spin-axis orientation, and ellipsoid axis ratios. On a 10-year LSST simulation it reports halved mean residuals, ~3× smaller scatter in H and phase parameters, and a 53 % success rate (10–20 % more physically meaningful solutions per filter than prior approaches); the method is also applied to real photometry of (45) Eugenia.

Significance. If the reported improvements are robust, SOCCA would provide a scalable route to extract shape, spin, and compositional information from the millions of sparse light curves expected from LSST and ZTF. The joint multi-band treatment and explicit period-search component are practical strengths for survey-scale application.

major comments (3)
  1. [Abstract] Abstract: the central quantitative claims (mean residuals halved, H and phase-parameter scatter reduced by a factor of three) are presented without accompanying error budgets, cross-validation statistics, or a description of the period-search and ellipsoid-fitting procedure, so the improvements cannot be assessed for statistical significance or possible overfitting.
  2. [Model description / LSST simulation] Model description (and § on LSST simulation): the triaxial-ellipsoid projected-area term assumes convex shape and band-independent surface properties except for overall scaling. When this assumption is violated (non-convex bodies or rotational color variegation), the additional free parameters (period, pole, a/b/c) can absorb residuals that would otherwise be attributed to the HG1G2 phase function, potentially biasing the recovered H, G1, G2; the 53 % success rate already indicates the assumption is not universally satisfied.
  3. [Validation on (45) Eugenia] Validation section: the only real-data test is a single object ((45) Eugenia); no quantitative comparison of recovered parameters against independent shape or spin solutions (e.g., from radar or dense light-curve inversion) is supplied, leaving the claimed factor-of-three improvement unverified on actual observations.
minor comments (2)
  1. [Model description] Notation for the projected-area factor and its coupling to the HG1G2 terms should be written explicitly (ideally as an equation) rather than described only in prose.
  2. [LSST simulation results] The success-rate definition (what constitutes a “physically meaningful solution”) is not stated; a clear criterion (e.g., period uncertainty < X %, axis-ratio bounds) would aid reproducibility.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments. We respond point-by-point below and have revised the manuscript to improve clarity on the abstract claims, to discuss model assumptions and limitations, and to better contextualize the real-data example.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central quantitative claims (mean residuals halved, H and phase-parameter scatter reduced by a factor of three) are presented without accompanying error budgets, cross-validation statistics, or a description of the period-search and ellipsoid-fitting procedure, so the improvements cannot be assessed for statistical significance or possible overfitting.

    Authors: We agree that the abstract would benefit from additional context on the methods. In the revised version we have added a concise description of the period-search procedure and the triaxial-ellipsoid projection fitting. The supporting error budgets, cross-validation approach, and statistical details remain in Sections 3 and 4; we have also inserted a short sentence in the abstract directing readers to those sections for the quantitative assessment. revision: yes

  2. Referee: [Model description / LSST simulation] Model description (and § on LSST simulation): the triaxial-ellipsoid projected-area term assumes convex shape and band-independent surface properties except for overall scaling. When this assumption is violated (non-convex bodies or rotational color variegation), the additional free parameters (period, pole, a/b/c) can absorb residuals that would otherwise be attributed to the HG1G2 phase function, potentially biasing the recovered H, G1, G2; the 53 % success rate already indicates the assumption is not universally satisfied.

    Authors: The referee correctly notes the model's assumptions. SOCCA is formulated under the convex triaxial ellipsoid with per-band scaling only. The reported 53 % success rate is defined precisely as the fraction of cases yielding physically plausible solutions under these assumptions. We have added an explicit limitations paragraph in the discussion section that addresses potential absorption of phase-function residuals by the shape/rotation parameters, the risk of bias in H/G1/G2 for non-convex or variegated bodies, and guidance on interpreting the success rate as a diagnostic of model applicability. revision: yes

  3. Referee: [Validation on (45) Eugenia] Validation section: the only real-data test is a single object ((45) Eugenia); no quantitative comparison of recovered parameters against independent shape or spin solutions (e.g., from radar or dense light-curve inversion) is supplied, leaving the claimed factor-of-three improvement unverified on actual observations.

    Authors: The factor-of-three improvement is quantified exclusively on the LSST simulation where ground truth is known (Section 4). The Eugenia application is presented as an illustrative demonstration on real sparse photometry rather than the basis for the improvement claim. We have revised the validation section to state this distinction explicitly, added references to published spin-axis solutions for Eugenia, and noted that a direct numerical comparison with radar or dense-inversion results lies outside the present scope. revision: partial

Circularity Check

0 steps flagged

SOCCA derivation is self-contained; no load-bearing steps reduce to inputs by construction

full rationale

The paper defines SOCCA as an explicit extension of the existing HG1G2 phase-function formalism by adding a multiplicative projected-area term from a rotating triaxial ellipsoid (abstract and model description). Reported improvements (halved residuals, 3× tighter scatter on H and phase parameters) are obtained by fitting the augmented model to an LSST simulation and to real photometry of (45) Eugenia; these are empirical outcomes of the extra degrees of freedom rather than algebraic identities. No equations, fitting procedures, or self-citations are shown that would make the target quantities equivalent to the inputs by construction. The central claim therefore remains independent of its own reported performance metrics.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The model rests on the standard HG1G2 phase-function framework plus the geometric assumption that brightness is proportional to the projected area of a triaxial ellipsoid; no new free parameters beyond the usual HG1G2 coefficients and the three axis ratios plus spin vector are introduced in the abstract.

axioms (1)
  • domain assumption Brightness variations are dominated by the changing projected area of a triaxial ellipsoid with uniform surface properties per band.
    This geometric premise is required to extend HG1G2 with the projected-surface term.

pith-pipeline@v0.9.1-grok · 5847 in / 1343 out tokens · 26088 ms · 2026-06-26T23:05:39.961366+00:00 · methodology

discussion (0)

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Works this paper leans on

297 extracted references · 230 canonical work pages · 83 internal anchors

  1. [1]

    Science , keywords =

    Galileo Encounter with 951 Gaspra: First Pictures of an Asteroid. Science , keywords =. doi:10.1126/science.257.5077.1647 , adsurl =

    work page doi:10.1126/science.257.5077.1647

  2. [2]

    , keywords =

    A refined ``standard'' thermal model for asteroids based on observations of 1 Ceres and 2 Pallas. , keywords =. doi:10.1016/0019-1035(86)90021-7 , adsurl =

    work page doi:10.1016/0019-1035(86)90021-7

  3. [3]

    , year = 1999, month = dec, volume =

    Physical Characteristics of Near-Earth Asteroids from Thermal Infrared Spectrophotometry. , year = 1999, month = dec, volume =. doi:10.1006/icar.1999.6248 , adsurl =

    work page doi:10.1006/icar.1999.6248 1999

  4. [4]

    Thermal physics of asteroids. I. Effects of shape, heat conduction and beaming. , keywords =

  5. [5]

    Asteroids II , year = 1989, editor =

    Radiometry and thermal modeling of asteroids. Asteroids II , year = 1989, editor =

    1989

  6. [6]

    , year = 2000, month = sep, volume =

    Opposition Effect of Asteroids. , year = 2000, month = sep, volume =. doi:10.1006/icar.2000.6410 , adsurl =

    work page doi:10.1006/icar.2000.6410 2000

  7. [7]

    Astronomische Nachrichten , year = 1932, month = oct, volume =

    Die Bestimmung der Winkelelemente der inneren Bewegung von Eros. Astronomische Nachrichten , year = 1932, month = oct, volume =. doi:10.1002/asna.19322462402 , adsurl =

    work page doi:10.1002/asna.19322462402 1932

  8. [8]

    , keywords =

    Investigation of systematic bias in radiometric diameter determination of near-Earth asteroids: the night emission simulated thermal model (NESTM). , keywords =. doi:10.1111/j.1365-2966.2009.14996.x , archivePrefix =. 0905.1601 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14996.x 2009

  9. [9]

    I - 433 Eros

    Speckle interferometry of asteroids. I - 433 Eros. , keywords =. doi:10.1016/0019-1035(85)90160-5 , adsurl =

    work page doi:10.1016/0019-1035(85)90160-5

  10. [11]

    , keywords =

    The dimensions of (6) Hebe as a result of occultation observations. , keywords =

  11. [12]

    Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey. , year = 2006, month = nov, volume =. doi:10.1016/j.icarus.2006.06.001 , adsurl =

    work page doi:10.1016/j.icarus.2006.06.001 2006

  12. [13]

    , year = 1994, month = aug, volume =

    Density and size of comet Shoemaker-Levy 9 deduced from a tidal breakup model. , year = 1994, month = aug, volume =. doi:10.1038/370349a0 , adsurl =

    work page doi:10.1038/370349a0 1994

  13. [14]

    , keywords =

    Direct Measurement of the Size of the Large Kuiper Belt Object (50000) Quaoar. , keywords =. doi:10.1086/382513 , adsurl =

    work page doi:10.1086/382513

  14. [15]

    Laser Guide Star Adaptive Optics for Astronomy , year = 2000, editor =

    Measuring Asteroids with Adaptive Optics. Laser Guide Star Adaptive Optics for Astronomy , year = 2000, editor =

    2000

  15. [16]

    , keywords =

    Triaxial ellipsoid dimensions and rotational pole of 2 Pallas from two stellar occultations. , keywords =. doi:10.1016/0019-1035(89)90180-2 , adsurl =

    work page doi:10.1016/0019-1035(89)90180-2

  16. [17]

    ADAM: a general method for using various data types in asteroid reconstruction

    ADAM: a general method for using various data types in asteroid reconstruction. , keywords =. doi:10.1051/0004-6361/201425259 , archivePrefix =. 1501.05958 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425259

  17. [18]

    Physical Properties of (2) Pallas

    Physical properties of (2) Pallas. , keywords =. doi:10.1016/j.icarus.2009.08.007 , archivePrefix =. 0912.3626 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2009.08.007 2009

  18. [19]

    Science , year = 1994, month = feb, volume =

    Shape of Asteroid 4769 Castalia (1989 PB) from Inversion of Radar Images. Science , year = 1994, month = feb, volume =. doi:10.1126/science.263.5149.940 , adsurl =

    work page doi:10.1126/science.263.5149.940 1989

  19. [20]

    , year = 1997, month = nov, volume =

    Constraints on Spin State and Hapke Parameters of Asteroid 4769 Castalia Using Lightcurves and a Radar-Derived Shape Model. , year = 1997, month = nov, volume =. doi:10.1006/icar.1997.5804 , adsurl =

    work page doi:10.1006/icar.1997.5804 1997

  20. [21]

    Shaping Asteroids with Genetic Evolution (SAGE)

    Shaping asteroid models using genetic evolution (SAGE). , keywords =. doi:10.1093/mnras/stx2535 , archivePrefix =. 1904.08940 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2535 1904

  21. [22]

    , keywords =

    Polarimetric Observations of Small Asteroids: Preliminary Results. , keywords =. doi:10.1006/icar.1998.6062 , adsurl =

    work page doi:10.1006/icar.1998.6062 1998

  22. [23]

    Asteroids, Comets, and Meteors , year = 1983, month = jan, pages =

    An analytical method for the determination of the rotational direction of asteroids. Asteroids, Comets, and Meteors , year = 1983, month = jan, pages =

    1983

  23. [24]

    Finding asteroids with slow spin

    V-band photometry of asteroids from ASAS-SN. Finding asteroids with slow spin. , keywords =. doi:10.1051/0004-6361/202140759 , archivePrefix =. 2107.10027 , primaryClass =

    work page doi:10.1051/0004-6361/202140759

  24. [25]

    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

  25. [26]

    Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes

    Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes. , keywords =. doi:10.1016/j.icarus.2011.03.016 , archivePrefix =. 1104.4227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2011.03.016 2011

  26. [27]

    Sizes of main-belt asteroids by combining shape models and Keck adaptive aptics observations

    Sizes of main-belt asteroids by combining shape models and Keck adaptive optics observations. , keywords =. doi:10.1016/j.icarus.2013.07.023 , archivePrefix =. 1308.0446 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2013.07.023 2013

  27. [28]

    Thermophysical modeling of asteroids from WISE thermal infrared data - Significance of the shape model and the pole orientation uncertainties

    Thermophysical modeling of asteroids from WISE thermal infrared data - Significance of the shape model and the pole orientation uncertainties. , keywords =. doi:10.1016/j.icarus.2015.04.014 , archivePrefix =. 1504.04199 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2015.04.014 2015

  28. [29]

    Asteroid shapes and thermal properties from combined optical and mid-infrared photometry inversion

    Asteroid shapes and thermal properties from combined optical and mid-infrared photometry inversion. , keywords =. doi:10.1051/0004-6361/201730868 , archivePrefix =. 1706.01232 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730868

  29. [30]

    Celestial Mechanics and Dynamical Astronomy , keywords =

    Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris. Celestial Mechanics and Dynamical Astronomy , keywords =. doi:10.1007/s10569-007-9103-8 , adsurl =

    work page doi:10.1007/s10569-007-9103-8

  30. [31]

    , keywords =

    A determination of the masses of Ceres, Pallas, and Vesta from their perturbations upon the orbit of Mars. , keywords =. doi:10.1016/0019-1035(89)90143-7 , adsurl =

    work page doi:10.1016/0019-1035(89)90143-7

  31. [32]

    Based on Gaia astrometric data

    Asteroid (4337) Arecibo: Two ice-rich bodies forming a binary. Based on Gaia astrometric data. , keywords =. doi:10.1051/0004-6361/202450586 , adsurl =

    work page doi:10.1051/0004-6361/202450586

  32. [33]

    , year = 1999, month = oct, volume =

    Discovery of a moon orbiting the asteroid 45 Eugenia. , year = 1999, month = oct, volume =. doi:10.1038/44089 , adsurl =

    work page doi:10.1038/44089 1999

  33. [34]

    Science , keywords =

    Radar Imaging of Binary Near-Earth Asteroid (66391) 1999 KW4. Science , keywords =. doi:10.1126/science.1133622 , adsurl =

    work page doi:10.1126/science.1133622 1999

  34. [35]

    , year = 2000, month = jul, volume =

    Two-Period Lightcurves of 1996 FG _ 3 , 1998 PG, and (5407) 1992 AX: One Probable and Two Possible Binary Asteroids. , year = 2000, month = jul, volume =. doi:10.1006/icar.2000.6375 , adsurl =

    work page doi:10.1006/icar.2000.6375 1996

  35. [37]

    , keywords =

    An advanced multipole model for (216) Kleopatra triple system. , keywords =. doi:10.1051/0004-6361/202140901 , archivePrefix =. 2105.09134 , primaryClass =

    work page doi:10.1051/0004-6361/202140901

  36. [38]

    Orbit and Bulk Density of the OSIRIS-REx Target Asteroid (101955) Bennu

    Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu. , keywords =. doi:10.1016/j.icarus.2014.02.020 , archivePrefix =. 1402.5573 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2014.02.020 2014

  37. [39]

    , year = 2007, month = mar, volume =

    Nucleus properties of Comet 9P/Tempel 1 estimated from non-gravitational force modeling. , year = 2007, month = mar, volume =. doi:10.1016/j.icarus.2006.07.022 , adsurl =

    work page doi:10.1016/j.icarus.2006.07.022 2007

  38. [40]

    Science , year = 1970, month = jun, volume =

    Asteroid Vesta: Spectral Reflectivity and Compositional Implications. Science , year = 1970, month = jun, volume =. doi:10.1126/science.168.3938.1445 , adsurl =

    work page doi:10.1126/science.168.3938.1445 1970

  39. [41]

    The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys

    The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys. , keywords =. doi:10.1016/j.icarus.2013.06.027 , archivePrefix =. 1307.2424 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2013.06.027 2013

  40. [42]

    , keywords =

    Physical parameters of near-Earth asteroid 1982 DV. , keywords =. doi:10.1016/0019-1035(85)90004-1 , adsurl =

    work page doi:10.1016/0019-1035(85)90004-1 1982

  41. [44]

    doi:10.1126/science.1091452 , keywords =

    Science , year =. doi:10.1126/science.1091452 , keywords =

    work page doi:10.1126/science.1091452

  42. [45]

    Detection of the Yarkovsky effect for C-type asteroids in the Veritas family

    Detection of the Yarkovsky effect for C-type asteroids in the Veritas family. , keywords =. doi:10.1093/mnras/stx1186 , archivePrefix =. 1705.04333 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1186

  43. [46]

    Asteroid Families. I. Identification by Hierarchical Clustering and Reliability Assessment. , keywords =. doi:10.1086/115658 , adsurl =

    work page doi:10.1086/115658

  44. [47]

    Yarkovsky V-shape identification of asteroid families

    Yarkovsky V-shape identification of asteroid families. , keywords =. doi:10.1016/j.icarus.2016.09.029 , archivePrefix =. 1609.06384 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2016.09.029 2016

  45. [48]

    , keywords =

    Asteroid phase curves from ATLAS dual-band photometry. , keywords =. doi:10.1016/j.icarus.2020.114094 , archivePrefix =. 2009.05129 , primaryClass =

    work page doi:10.1016/j.icarus.2020.114094 2020

  46. [49]

    A Taxonomic Study of Asteroid Families from KMTNet-SAAO Multi-band Photometry

    A Taxonomic Study of Asteroid Families from KMTNET-SAAO Multiband Photometry. , keywords =. doi:10.3847/1538-4365/ab1344 , archivePrefix =. 1903.08019 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab1344 1903

  47. [50]

    , year = 2000, month = jul, volume =

    The 2MASS Asteroid and Comet Survey. , year = 2000, month = jul, volume =. doi:10.1006/icar.2000.6366 , adsurl =

    work page doi:10.1006/icar.2000.6366 2000

  48. [51]

    , keywords =

    Low thermal conductivity of the superfast rotator (499998) 2011 PT. , keywords =. doi:10.1051/0004-6361/202039628 , archivePrefix =. 2101.04399 , primaryClass =

    work page doi:10.1051/0004-6361/202039628 2011

  49. [52]

    , year = 2011, month = jul, volume =

    Online multi-parameter phase-curve fitting and application to a large corpus of asteroid photometric data. , year = 2011, month = jul, volume =. doi:10.1016/j.jqsrt.2011.03.003 , adsurl =

    work page doi:10.1016/j.jqsrt.2011.03.003 2011

  50. [53]

    Photometric Studies of Asteroids. V. The Light-Curve and Phase Function of 20 Massalia. , year = 1956, month = mar, volume =. doi:10.1086/146166 , adsurl =

    work page doi:10.1086/146166 1956

  51. [54]

    Fast error-controlling MOID computation for confocal elliptic orbits

    Fast error-controlling MOID computation for confocal elliptic orbits. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2019.02.005 , archivePrefix =. 1811.06373 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.ascom.2019.02.005 2019

  52. [55]

    , keywords =

    Escape of asteroids from the main belt. , keywords =. doi:10.1051/0004-6361/201629252 , adsurl =

    work page doi:10.1051/0004-6361/201629252

  53. [56]

    Acta Astronautica , keywords =

    A Delta-V map of the known Main Belt Asteroids. Acta Astronautica , keywords =. doi:10.1016/j.actaastro.2018.02.014 , adsurl =

    work page doi:10.1016/j.actaastro.2018.02.014 2018

  54. [57]

    Astronomy and Computing , keywords =

    The astorb database at Lowell Observatory. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2022.100661 , archivePrefix =. 2210.10217 , primaryClass =

    work page doi:10.1016/j.ascom.2022.100661 2022

  55. [58]

    Handbook of Cosmic Hazards and Planetary Defense , year = 2015, pages =

    Minor Planet Center. Handbook of Cosmic Hazards and Planetary Defense , year = 2015, pages =. doi:10.1007/978-3-319-03952-7_89 , adsurl =

    work page doi:10.1007/978-3-319-03952-7_89 2015

  56. [59]

    Dynamics, Ephemerides, and Astrometry of the Solar System , year = 1996, editor =

    Production d'elements orbitaux de cometes sur PC. Dynamics, Ephemerides, and Astrometry of the Solar System , year = 1996, editor =

    1996

  57. [60]

    Handbook of Cosmic Hazards and Planetary Defense , year =

  58. [61]

    Journal of the British Astronomical Association , year = 2018, month = oct, volume =

    Introducing the Comet Observation database (COBS). Journal of the British Astronomical Association , year = 2018, month = oct, volume =

    2018

  59. [62]

    , keywords =

    Evidence for differentiation of the most primitive small bodies. , keywords =. doi:10.1051/0004-6361/202140342 , archivePrefix =. 2103.06349 , primaryClass =

    work page doi:10.1051/0004-6361/202140342

  60. [63]

    Science , keywords =

    The Mass of Dwarf Planet Eris. Science , keywords =. doi:10.1126/science.1139415 , adsurl =

    work page doi:10.1126/science.1139415

  61. [64]

    , year = 2005, month = aug, volume =

    Discovery of the triple asteroidal system 87 Sylvia. , year = 2005, month = aug, volume =. doi:10.1038/nature04018 , adsurl =

    work page doi:10.1038/nature04018 2005

  62. [65]

    Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites

    Physical, spectral, and dynamical properties of asteroid (107) Camilla and its satellites. , keywords =. doi:10.1016/j.icarus.2018.03.003 , archivePrefix =. 1803.02722 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2018.03.003 2018

  63. [66]

    Extreme AO Observations of Two Triple Asteroid Systems with SPHERE

    Extreme AO Observations of Two Triple Asteroid Systems with SPHERE. , keywords =. doi:10.3847/2041-8205/820/2/L35 , archivePrefix =. 1603.04435 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/820/2/l35 2041

  64. [67]

    Detection of a third moon around (130) Elektra with SPHERE/IFS

    First observation of a quadruple asteroid. Detection of a third moon around (130) Elektra with SPHERE/IFS. , keywords =. doi:10.1051/0004-6361/202142623 , archivePrefix =. 2202.04425 , primaryClass =

    work page doi:10.1051/0004-6361/202142623

  65. [68]

    The homogeneous internal structure of CM-like asteroid (41) Daphne

    Homogeneous internal structure of CM-like asteroid (41) Daphne. , keywords =. doi:10.1051/0004-6361/201833898 , archivePrefix =. 1901.01890 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833898 1901

  66. [69]

    , year = 2008, month = nov, volume =

    Roche figures of doubly synchronous asteroids. , year = 2008, month = nov, volume =. doi:10.1016/j.pss.2008.02.040 , adsurl =

    work page doi:10.1016/j.pss.2008.02.040 2008

  67. [70]

    Mass and density of B-type asteroid (702) Alauda

    Mass and Density of the B-type Asteroid (702) Alauda. , keywords =. doi:10.1088/0004-637X/727/2/69 , archivePrefix =. 1011.6577 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/727/2/69

  68. [71]

    , keywords =

    M-type (22) Kalliope: A tiny Mercury. , keywords =. doi:10.1051/0004-6361/202243200 , adsurl =

    work page doi:10.1051/0004-6361/202243200

  69. [72]

    Characteristics and Large Bulk Density of the C-type Main-Belt Triple Asteroid (93) Minerva

    Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva. , keywords =. doi:10.1016/j.icarus.2013.02.018 , archivePrefix =. 1310.3209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2013.02.018 2013

  70. [73]

    , keywords =

    Preimpact Mutual Orbit of the DART Target Binary Asteroid (65803) Didymos Derived from Observations of Mutual Events in 2003-2021. , keywords =. doi:10.3847/PSJ/ac7233 , adsurl =

    work page doi:10.3847/psj/ac7233 2003

  71. [74]

    The nature of near-earth asteroids from the study of their thermal infrared emission

  72. [75]

    NASA Planetary Data System , year = 2019, month = dec, pages =

    Small Bodies Occultations Bundle V3.0. NASA Planetary Data System , year = 2019, month = dec, pages =. doi:10.26033/ap0g-wf63 , adsurl =

    work page doi:10.26033/ap0g-wf63 2019

  73. [76]

    , keywords =

    The Albedo Distribution of Jovian Trojan Asteroids. , keywords =. doi:10.1086/377015 , adsurl =

    work page doi:10.1086/377015

  74. [77]

    Main Belt Binary Asteroidal Systems With Eccentric Mutual Orbits

    Main belt binary asteroidal systems with eccentric mutual orbits. , keywords =. doi:10.1016/j.icarus.2007.12.010 , archivePrefix =. 0804.1385 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2007.12.010 2007

  75. [78]

    , keywords =

    Binary asteroid (31) Euphrosyne: ice-rich and nearly spherical. , keywords =. doi:10.1051/0004-6361/202038372 , archivePrefix =. 2007.08059 , primaryClass =

    work page doi:10.1051/0004-6361/202038372 2007

  76. [79]

    Main Belt Binary Asteroidal Systems With Circular Mutual Orbits

    Main belt binary asteroidal systems with circular mutual orbits. , keywords =. doi:10.1016/j.icarus.2008.03.007 , archivePrefix =. 0804.1383 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2008.03.007 2008

  77. [80]

    New insights on the binary asteroid 121 Hermione

    New insights on the binary Asteroid 121 Hermione. , keywords =. doi:10.1016/j.icarus.2009.04.032 , archivePrefix =. 0904.2033 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.icarus.2009.04.032 2009

  78. [81]

    Kinematics and Physics of Celestial Bodies , year = 1991, month = jan, volume =

    Photometry and polarimetry of the asteroid 47 Aglaja. Kinematics and Physics of Celestial Bodies , year = 1991, month = jan, volume =

    1991

  79. [82]

    , year = 1996, month = mar, volume =

    The Shape of Ida. , year = 1996, month = mar, volume =. doi:10.1006/icar.1996.0033 , adsurl =

    work page doi:10.1006/icar.1996.0033 1996

  80. [83]

    arXiv , doi =:2105.09134 , keywords =

    , year =. arXiv , doi =:2105.09134 , keywords =

    arXiv

Showing first 80 references.