Rotation lightcurves of small jovian Trojan asteroids

French, Linda M.; Stephens, Robert D.; Coley, Daniel R.; Wasserman, L. H.; Sieben, Jennifer

doi:10.1016/j.icarus.2015.03.026

Cited by 18 publications

(21 citation statements)

References 19 publications

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“…Applying the critical density calculation above for our sample, the highest density values we obtain are ∼0.5 g cm −3 (see Fig. 8), lower than that of Main Belt asteroids in the same size range, but the same as obtained by French et al (2015). Even in our unbiased sample, despite the fact that rotation periods longer than ∼1 h should have been identified, we were unable to find any Jovian Trojan asteroid with a high (∼2 h) spin rate.…”

Section: Period Distribution and The Spin Barrier Of Jovian Trojan Assupporting

confidence: 74%

“…5 we plot the amplitude-period diagram for Trojans from the literature (Molnar et al 2008;Mottola et al 2011;French et al 2015;Waszczak et al 2015) compared to our results. It is known that Main Belt families are characterized by specific brightness variation distributions (Szabó & Kiss 2008).…”

Section: Period and Amplitude Distributionsmentioning

confidence: 88%

“…Very long rotation periods may be an indication of binarity, as is the case, for example, for Jovian Trojan (617) Patroclus where the >100 h rotation period is explained by tidal breaking (Mueller et al 2010). Slow rotation of small (<30 km) and low density (<1 g cm −3 ) objects may have also been set by the YORP effect (French et al 2015). Among our slow rotators, there are objects that fall into this susceptible size range according to the sizes derived by Grav et al (2012) based on NEOWISE observations.…”

Section: Period Distribution and The Spin Barrier Of Jovian Trojan Asmentioning

confidence: 97%

“…Our period determinations are plotted against data from the literature (Molnar et al 2008;Mottola et al 2011;French et al 2015;Waszczak et al 2015) in Fig. 4.…”

Section: Period and Amplitude Distributionsmentioning

confidence: 99%

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The heart of the swarm: K2 photometry and rotational characteristics of 56 Jovian Trojan asteroids

Szabó

Pál

Kiss

et al. 2017

A&A

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We present fully covered phased light curves for 56 Jovian Trojan asteroids as observed by the K2 mission of the Kepler space telescope. This set of objects has been monitored during Campaign 6 and represents a nearly unbiased subsample of the population of small solar system bodies. We derived precise periods and amplitudes for all Trojans, and found their distributions to be compatible with the previous statistics. We point out, however, that ground-based rotation periods are often unreliable above 20 h, and we find an overabundance of rotation periods above 60 h compared with other minor planet populations. From amplitude analysis we derive a rate of binarity of 20 ± 5%. Our spin rate distribution confirms the previously obtained spin barrier of ∼5 h and the corresponding ∼0.5 g cm −3 cometary-like density limit, also suggesting a high internal porosity for Jovian Trojans. One of our targets, asteroid 65227 exhibits a double rotation period, which can either be due to binarity or the outcome of a recent collision.

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Section: Period Distribution and The Spin Barrier Of Jovian Trojan Assupporting

confidence: 74%

Section: Period and Amplitude Distributionsmentioning

confidence: 88%

Section: Period Distribution and The Spin Barrier Of Jovian Trojan Asmentioning

confidence: 97%

“…Our period determinations are plotted against data from the literature (Molnar et al 2008;Mottola et al 2011;French et al 2015;Waszczak et al 2015) in Fig. 4.…”

Section: Period and Amplitude Distributionsmentioning

confidence: 99%

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The heart of the swarm: K2 photometry and rotational characteristics of 56 Jovian Trojan asteroids

Szabó

Pál

Kiss

et al. 2017

A&A

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“…For smaller Trojans, the overabundance of slow rotators is even more pronounced. Figure 3, from French et al (2015), shows the distribution of rotation rates for Trojans less than 30 km in diameter, along with the best fit Maxwellian curve. The Maxwellian is the distribution that would be expected if the spin vectors were oriented isotropically, with each component of the angular velocity following a Gaussian distribution.…”

Section: Rotational States and Phase Curvesmentioning

confidence: 99%

The Complex History of Trojan Asteroids

Emery¹,

Marzari²,

Morbidelli³

et al. 2015

Asteroids IV

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The Trojan asteroids provide a unique perspective on the history of Solar System. As a large population of small bodies, they record important gravitational interactions and dynamical evolution of the Solar System. In the past decade, significant advances have been made in understanding physical properties, and there has been a revolution in thinking about the origin of Trojans. The ice and organics generally presumed to be a significant part of Trojan compositions have yet to be detected directly, though low density of the binary system Patroclus (and possibly low density of the binary/moonlet system Hektor) is consistent with an interior ice component. By contrast, fine-grained silicates that appear to be similar to cometary silicates in composition have been detected, and a color bimodality may indicate distinct compositional groups among the Trojans. Whereas Trojans had traditionally been thought to have formed near 5 AU, a new paradigm has developed in which the Trojans formed in the proto-Kuiper Belt, and they were scattered inward and captured in the Trojan swarms as a result of resonant interactions of the giant planets. Whereas the orbital and population distributions of current Trojans are consistent with this origin scenario, there are significant differences between current physical properties of Trojans and those of Kuiper Belt objects. These differences may be indicative of surface modification due to the inward migration of objects that became the Trojans, but understanding of appropriate modification mechanisms is poor and would benefit from additional laboratory studies. Many open questions remain, and the future promises significant strides in our understanding of Trojans. The time is ripe for a spacecraft mission to the Trojans, to turn these objects into geologic worlds that can be studied in detail to unravel their complex history.Comment: Chapter for Asteroids IV book (UA Press), accepted for publication, 33 pages, 10 figure

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Trojan Asteroid Satellites, Rings, and Activity

Noll,

Brown,

Buie

et al. 2023

Space Sci Rev

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The Lucy mission will encounter five Jupiter Trojans during its mission with three of the five already known to be multiple systems. These include a near-equal-mass binary, a small and widely separated satellite, and one intermediate-size satellite system. This chapter reviews the current state of knowledge of Trojan asteroid satellites in the context of similar satellite systems in other small body populations. The prospects for the detection of additional satellites as well as other near-body phenomena are considered. The scientific utility of satellites makes their observation with Lucy an important scientific priority for the mission.

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Rotation lightcurves of small jovian Trojan asteroids

Cited by 18 publications

References 19 publications

The heart of the swarm: K2 photometry and rotational characteristics of 56 Jovian Trojan asteroids

The heart of the swarm: K2 photometry and rotational characteristics of 56 Jovian Trojan asteroids

The Complex History of Trojan Asteroids

Trojan Asteroid Satellites, Rings, and Activity

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