ASTEROID FAMILY IDENTIFICATION USING THE HIERARCHICAL CLUSTERING METHOD AND<i>WISE</i>/NEOWISE PHYSICAL PROPERTIES

Masiero, J.; Mainzer, A.; Bauer, J. M.; Grav, T.; Nugent, C.; Stevenson, R.

doi:10.1088/0004-637x/770/1/7

Cited by 128 publications

(178 citation statements)

References 44 publications

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“…Milani et al 2014), estimated to be about 1.2 Gyr old (Milani et al 2016). The possible existence of other families inside this region has been discussed by several authors (Gil-Hutton 2006;Carruba 2009;Novaković et al 2011;Masiero et al 2013) who proposed several candidate groups which might be collisional families. Still, no family formed by a break-up of a dark carbonaceous parent body has been proposed to exist in the Phocaea region.…”

Section: Most Of the Phocaeasmentioning

confidence: 94%

A Dark Asteroid Family in the Phocaea Region

Novaković

Tsirvoulis

Granvik

et al. 2017

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We report the discovery of a new asteroid family among the dark asteroids residing in the Phocaea region the Tamara family. We make use of available physical data to separate asteroids in the region according to their surface reflectance properties, and establish the membership of the family. We determine the slope of the cumulative magnitude distribution of the family, and find it to be significantly steeper than the corresponding slope of all the asteroids in the Phocaea region. This implies that sub-kilometer dark Phocaeas are comparable in number to bright S-type objects, shedding light on an entirely new aspect of the composition of small Phocaea asteroids. We then use the Yarkovsky V-shape based method and estimate the age of the family to be 264 ± 43 Myr. Finally, we carry out numerical simulations of the dynamical evolution of the Tamara family. The results suggest that up to 50 Tamara members with absolute magnitude H < 19.4 may currently be found in the near-Earth region. Despite their relatively small number in the near-Earth space, the rate of Earth impacts by small, dark Phocaeas is non-negligible.

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Section: Most Of the Phocaeasmentioning

confidence: 94%

A Dark Asteroid Family in the Phocaea Region

Novaković

Tsirvoulis

Granvik

et al. 2017

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“…For comparison between our results and Masiero et al (2013), we fit gaussian profiles to the log distributions of the three families. The distributions in log space are shown in Figure 7.…”

Section: Albedo Variationsmentioning

confidence: 99%

Space weathering trends among carbonaceous asteroids

Kaluna

Masiero

Meech

2016

Icarus

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We present visible spectroscopic and albedo data of the 2.3 Gyr old Themis family and the <10 Myr old Beagle sub-family. The slope and albedo variations between these two families indicate C-complex asteroids become redder and darker in response to space weathering. Our observations of Themis family members confirm previously observed trends where phyllosilicate absorption features are less common among small diameter objects. Similar trends in the albedos of large (>15 km) and small (≤15 km) Themis members suggest these phyllosilicate feature and albedo trends result from regolith variations as a function of diameter. Observations of the Beagle asteroids show a small, but notable fraction of members with phyllosilicate features. The presence of phyllosilicates and the dynamical association of the main-belt comet 133P/Elst-Pizarro with the Beagle family imply the Beagle parent body was a heterogenous mixture of ice and aqueously altered minerals.Subject headings: main belt asteroids, carbonaceous asteroids, space weathering

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“…The spectroscopic signatures of the E-types match the characteristics of enstatite, a high-albedo iron-poor mineral that comprises much of the aubrite meteorites (Kelley & Gaffey 2002;Gaffey & Kelley 2004). The high albedos of the E-type asteroids (>40%) also make candidate source asteroids highly distinctive in both the Hungaria and main belt populations when we consider data from IR surveys like WISE (Masiero et al 2011(Masiero et al , 2013.…”

Section: Source Regionmentioning

confidence: 99%

PHYSICAL CHARACTERIZATION OF ∼2 m DIAMETER NEAR-EARTH ASTEROID 2015 TC25: A POSSIBLE BOULDER FROM E-TYPE ASTEROID (44) NYSA

Reddy¹,

Sanchez²,

Bottke³

et al. 2016

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Small near-Earth asteroids (NEAs) (<20 m) are interesting, because they are progenitors for meteorites in our terrestrial collection. The physical characteristics of these small NEAs are crucial to our understanding of the effectiveness of our atmosphere in filtering low-strength impactors. In the past, the characterization of small NEAs has been a challenge, because of the difficulty in detecting them prior to close Earth flyby. In this study, we physically characterized the 2 m diameter NEA 2015 TC25 using ground-based optical, near-infrared and radar assets during a close flyby of the Earth (distance 128,000 km) in 2015 October 12. Our observations suggest that its surface composition is similar to aubrites, a rare class of high-albedo differentiated meteorites. Aubrites make up only 0.14% of all known meteorites in our terrestrial meteorite collection. 2015 TC25 is also a very fast rotator with a period of 133±6 s. We combined the spectral and dynamical properties of 2015 TC25 and found the best candidate source body in the inner main belt to be the 70 km diameter E-type asteroid (44) Nysa. We attribute the difference in spectral slope between the two objects to the lack of regolith on the surface of 2015 TC25. Using the albedo of E-type asteroids (50%-60%) we refine the diameter of 2015 TC25 to 2 m, making it one of the smallest NEAs ever to be characterized.

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ASTEROID FAMILY IDENTIFICATION USING THE HIERARCHICAL CLUSTERING METHOD ANDWISE/NEOWISE PHYSICAL PROPERTIES

Cited by 128 publications

References 44 publications

A Dark Asteroid Family in the Phocaea Region

A Dark Asteroid Family in the Phocaea Region

Space weathering trends among carbonaceous asteroids

PHYSICAL CHARACTERIZATION OF ∼2 m DIAMETER NEAR-EARTH ASTEROID 2015 TC25: A POSSIBLE BOULDER FROM E-TYPE ASTEROID (44) NYSA

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