Fraction of Contact Binary Trojan Asteroids

Mann, Rita K.; Jewitt, David; Lacerda, Pedro

doi:10.1086/520328

Cited by 42 publications

(38 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In fact, the observed albedos from 0.04 to 0.12 could only be explained with an average Δm of about 0.6 mag. So unless the small Trojans have substantially higher typical axial ratios than were measured by Mann et al (2007), the spread of small Trojan albedos really is intrinsically wider than that of the large Trojans. We searched for correlations between albedo and other properties of the small Trojans.…”

Section: Notesmentioning

confidence: 91%

“…Table 4 and Figure 3 indicate that the range of albedos among small Trojans is wider than the range for the large Trojans, but we must be careful since the width of the distribution is at least partly artificial due to the lack of simultaneity in our data sets as described in Section 3. We can estimate how much of this spread is real based on a study of Trojan light curves by Mann et al (2007). They observed 114 Trojans with sparse sampling and derived a distribution of photometric ranges.…”

Section: Ensemble Properties and Correlationsmentioning

confidence: 99%

See 1 more Smart Citation

Albedos of Small Jovian Trojans

Fernández

Jewitt

Ziffer

2009

The Astronomical Journal

Self Cite

View full text Add to dashboard Cite

We present thermal observations of 44 Jovian Trojan asteroids with diameters D ranging from 5 to 24 km. All objects were observed at a wavelength of 24 μm with the Spitzer Space Telescope. Measurements of the thermal emission and of scattered optical light, mostly from the University of Hawaii 2.2 m Telescope, together allow us to constrain the diameter and geometric albedo of each body. We find that the median R-band albedo of these small Jovian Trojans is about 0.12, much higher than that of "large" Trojans with D > 57 km (0.04). Also the range of albedos among the small Trojans is wider. The small Trojans' higher albedos are also glaringly different from those of cometary nuclei, which match our sample Trojans in diameter, however, they roughly match the spread of albedos among (much larger) Centaurs and trans-Neptunian objects. We attribute the Trojan albedos to an evolutionary effect: the small Trojans are more likely to be collisional fragments and so their surfaces would be younger. A younger surface means less cumulative exposure to the space environment, which suggests that their surfaces would not be as dark as those of the large, primordial Trojans. In support of this hypothesis is a statistically significant correlation of higher albedo with smaller diameter in our sample alone and in a sample that includes the larger Trojans. This correlation of albedo and radius implies that the true size distribution of small Trojans is shallower than the visible magnitude distribution alone would suggest, and that there are approximately half the Trojans with D > 1 km than previously estimated.

show abstract

Section: Notesmentioning

confidence: 91%

Section: Ensemble Properties and Correlationsmentioning

confidence: 99%

Albedos of Small Jovian Trojans

Fernández

Jewitt

Ziffer

2009

The Astronomical Journal

Self Cite

View full text Add to dashboard Cite

show abstract

“…The lightcurve of 2007 TS 24 consists of the central, quasisinusoidal part, bracketed by two V-type minima. Such minima are typical for binary asteroids (Mann et al 2007), and judging from the lightcurve alone, 2007 TS 24 could be an asynchronous binary with two elongated components, producing their own light variations, and eclipsing each other. In this case the orbital period P orb would be twice as long as the time span between the minima, which is Δt = 0.52 h.…”

Section: Ts 24mentioning

confidence: 97%

Photometric survey of the very small near-Earth asteroids with the SALT telescope

Kwiatkowski¹,

Polińska²,

Loaring

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. Very small asteroids (VSAs) are thought to be the building blocks of larger asteroids and, as such, are interesting to study. Many of these monolithic or deeply fractured objects display rapid rotations with periods as short as several minutes. Observations of such asteroids can reveal their spin limits, which can be related to the tensile strength of their interiors. The evolution of the spins of these objects is primarily shaped by the YORP effect, the theory of which needs comparison with observations. Methods. With the 10 m SALT telescope, we observed VSAs belonging to near-Earth asteroids. The obtained lightcurves were used to derive synodical periods of rotation, amplitudes, and elongations of these bodies. Results. Results for 14 rapidly rotating asteroids were reported in the first paper in this series. Here we show lightcurves of 2 fast rotators, 9 objects with periods ≥1 h, and a possible non-principal axis rotator. We also list negative detections that most probably indicate asteroids with long periods and/or low amplitudes. Combining our results with the data from the literature, we obtain a set of 79 near-Earth VSAs with a median period of 0.25 h (15 min). By adjusting the spin limits predicted by theory to those observations, we find tentative evidence that the tensile strengths of VSAs, after scaling them to the same size, are of the same order as the minimum tensile strengths of stony meteoroids that undergo fragmentation under the atmospheric load.

show abstract

“…2 The dynamical classification is based on the Deep Ecliptic Survey Object Classifications: http://www.boulder.swri. edu/~buie/kbo/astrom/04TT357.html to the trans-Neptunian belt (Benner et al 2015;Mann et al 2007;Sheppard & Jewitt 2004). The expected fraction of contact binaries is high in all of the small body populations, with estimates up to 20%.…”

Section: Fraction Of Contact Binariesmentioning

confidence: 99%

2004 TT₃₅₇: A Potential Contact Binary in the Trans-Neptunian Belt

Thirouin

Sheppard

Noll

2017

ApJ

View full text Add to dashboard Cite

We report photometric observations of the trans-Neptunian object 2004 TT 357 obtained in 2015 and 2017 using the 4.3 m Lowell's Discovery Channel Telescope. We derive a rotational period of 7.79±0.01 h and a peak-to-peak lightcurve amplitude of 0.76±0.03 mag. 2004 TT 357 displays a large variability that can be explained by a very elongated single object or can be due to a contact/close binary. The most likely scenario is that 2004 TT 357 is a contact binary. If it is in hydrostatic equilibrium, we find that the lightcurve can be explained by a system with a mass ratio q min =0.45±0.05, and a density of ρ min =2 g cm −3 , or less likely a system with q max =0.8±0.05, and ρ max =5 g cm −3 . Considering a single triaxial ellipsoid in hydrostatic equilibrium, we derive a lower limit to the density of 0.78 g cm

show abstract

Fraction of Contact Binary Trojan Asteroids

Cited by 42 publications

References 39 publications

Albedos of Small Jovian Trojans

Albedos of Small Jovian Trojans

Photometric survey of the very small near-Earth asteroids with the SALT telescope

2004 TT₃₅₇: A Potential Contact Binary in the Trans-Neptunian Belt

Contact Info

Product

Resources

About

Fraction of Contact Binary Trojan Asteroids

Cited by 42 publications

References 39 publications

Albedos of Small Jovian Trojans

Albedos of Small Jovian Trojans

Photometric survey of the very small near-Earth asteroids with the SALT telescope

2004 TT357: A Potential Contact Binary in the Trans-Neptunian Belt

Contact Info

Product

Resources

About

2004 TT₃₅₇: A Potential Contact Binary in the Trans-Neptunian Belt