The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Krugly, Yu. N.; Belskaya, I. N.; Shevchenko, V. G.; Chiorny, V. G.; Velichko, F. P.; Mottola, S.; Erikson, A.; Hahn, Gerhard; Nathues, A.; Neukum, G.; Gaftonyuk, N. M.; Dotto, E.

doi:10.1006/icar.2002.6884

Cited by 59 publications

(46 citation statements)

References 22 publications

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“…Our spin solution does not match the one of Krugly et al (2002), mainly because they reported a value of ∼-10 • for the ecliptic latitude. Nevertheless, their rather preliminary pole solutions based on an ellipsoidal shape model assumption are relatively close to both our pole solutions and to the one of Ansdell et al (2014; Table 1).…”

Section: Shape Model and Rotation Statecontrasting

confidence: 73%

“…The recent work of Ansdell et al (2014) based on additional photometric data reported a single pole solution compatible with one of the pole solutions of Krugly et al (2002). This provides a convex shape.…”

Section: Introductionmentioning

confidence: 65%

“…Whether this spectral slope difference is due to the extreme solar heating on the former compared to the latter or to different grain sizes of the regolith of these bodies is still unclear (de León et al 2010). If the spin state had an obliquity of ∼90 • (Krugly et al 2002;Ansdell et al 2014), one of the hemispheres of Phaethon would receive substantially more solar heating during the perihelion passage because it is always facing the Sun. But Ohtsuka et al (2009) reported no significant spectral variability across the body, which might indicate that, contrary to expectations (Hiroi et al 1996), the sun-driven heating does not affect the spectral properties.…”

Section: Introductionmentioning

confidence: 99%

“…The spin state of Phaethon was first constrained by Krugly et al (2002): they derived two pole solutions with low ecliptic latitude (about −10 deg). The recent work of Ansdell et al (2014) based on additional photometric data reported a single pole solution compatible with one of the pole solutions of Krugly et al (2002).…”

Section: Introductionmentioning

confidence: 99%

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Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

100

110

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Context. The near-Earth asteroid (3200) Phaethon is an intriguing object: its perihelion is at only 0.14 au and is associated with the Geminid meteor stream. Aims. We aim to use all available disk-integrated optical data to derive a reliable convex shape model of Phaethon. By interpreting the available space-and ground-based thermal infrared data and Spitzer spectra using a thermophysical model, we also aim to further constrain its size, thermal inertia, and visible geometric albedo. Methods. We applied the convex inversion method to the new optical data obtained by six instruments and to previous observations. The convex shape model was then used as input for the thermophysical modeling. We also studied the long-term stability of Phaethon's orbit and spin axis with a numerical orbital and rotation-state integrator.Results. We present a new convex shape model and rotational state of Phaethon: a sidereal rotation period of 3.603958(2) h and ecliptic coordinates of the preferred pole orientation of (319 • , −39 • ) with a 5 • uncertainty. Moreover, we derive its size (D = 5.1 ± 0.2 km), thermal inertia (Γ = 600 ± 200 J m −2 s −1/2 K −1 ), geometric visible albedo (p V = 0.122 ± 0.008), and estimate the macroscopic surface roughness. We also find that the Sun illumination at the perihelion passage during the past several thousand years is not connected to a specific area on the surface, which implies non-preferential heating.

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Section: Shape Model and Rotation Statecontrasting

confidence: 73%

Section: Introductionmentioning

confidence: 65%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

100

110

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“…Most of the data have been obtained by a few dedicated programs (see, e.g., Pravec et al 1998, Mottola et al 1995a, Krugly et al 2002 that placed a high priority within their observational strategies on suppressing selection effects against slow rotators as well as low amplitude objects, and on resolving complex lightcurves of tumblers and binaries among NEAs. Radar observations contributed to the rotation data 2 P. Pravec, A.W.…”

Section: Introductionmentioning

confidence: 99%

NEA rotations and binaries

2006

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Abstract. Of the nearly 3900 near-Earth asteroids (NEAs) known as of June 2006, 325 have estimated rotation periods, with most of those determined by lightcurve analysis led by a few dedicated programs. NEAs with diameters down to 10 meters have been sampled. Observed spin distribution shows a major changing point around diameter of 200 meters. Larger NEAs show a barrier against spins faster than 11 d −1 (period about 2.2 h) that shifts to slower rates (longer periods) with increasing lightcurve amplitude (i.e., with increasing equatorial elongation). The spin barrier is interpreted as a critical spin rate for bodies in a gravity regime; NEAs larger than 200 meters are predominantly bodies with tensile strength too low to withstand a centrifugal acceleration for rotation faster than the critical spin rate. The cohesionless spin barrier disappears at sizes less than 200 meters where most objects rotate too fast to be held together by self-gravitation only, so a cohesion is implied in the smaller NEAs.The distribution of NEA spin rates in the cohesionless size range (D > 0.2 km) is highly nonMaxwellian, suggesting that mechanisms other than just collisions have been at work. There is a pile up just in front of the barrier, at periods 2-3 h. It may be related to a spin up mechanism crowding asteroids to the barrier. An excess of slow rotators is observed at periods longer than 30 hours. A spin-down mechanism has no obvious lower limit on spin rate; periods as long as tens of days have been observed.Most NEAs appear to be in their basic spin states with rotation around principal axis with maximum moment of inertia. Tumbling objects (i.e., bodies in excited, non-principal axis rotation) are present and actually predominate among slow rotators with estimated damping timescales longer than the age of the solar system. A few tumblers observed among fast rotating coherent objects appear to be either more rigid or younger than the larger (cohesionless) tumblers.An abundant population of binary systems has been found among NEAs. The fraction of binaries among NEAs larger than 0.3 km has been estimated to be 15 ± 4%. Primaries of binary systems concentrate at fast spin rates (periods 2-3 h) and low amplitudes, i.e., they lie just below the cohesionless spin barrier. The total angular momentum content in binary systems suggests that they formed from parent bodies spinning at the critical rate. The fact that a very similar population of binaries has been found among small main belt asteroids suggests a binary formation mechanism that may not be related to close encounters with the terrestrial planets.

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International ISON project & databases on space debris and asteroids

Molotov,

Zhao,

et al. 2024

Astrophys Space Sci

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The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Cited by 59 publications

References 22 publications

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

NEA rotations and binaries

International ISON project & databases on space debris and asteroids

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