Apollo Asteroids 1566 Icarus and 2007 MK
                    <sub>6</sub>
                    : Icarus Family Members?

Ohtsuka, K.; Arakida, Hideyoshi; Itô, Takashi; Kasuga, Toshihiro; Watanabe, J.; Kinoshita, Daisuke; Sekiguchi, T.; Asher, D. J.; Nakano, S.

doi:10.1086/522589

Cited by 30 publications

(15 citation statements)

References 22 publications

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“…In Figure 13, in the left panel, we plot the evolution of 1566 Icarus in the eccentricity-ω plane; one point is plotted every 1000 years. We see that the argument of perihelion circulates with a period of about 50 kyr, consistent with a previous study of 1566 Icarus (Ohtsuka et al 2007). During the circulation of ω, it spends more time around ω = 0 and ω = π.…”

Section: Argument Of Perihelionsupporting

confidence: 91%

On the non-uniform distribution of the angular elements of near-Earth objects

JeongAhn

Malhotra

2014

Icarus

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We examine the angular distributions of near-Earth objects (NEOs) which are often regarded as uniform. The apparent distribution of the longitude of ascending node, Ω, is strongly affected by well-known seasonal effects in the discovery rate of NEOs. The deviation from the expected π-periodicity in the apparent distribution of Ω indicates that its intrinsic distribution is slightly enhanced along a mean direction,Ω = 111 • ; approximately 53% of NEOs have Ω values within ±90 • ofΩ. We also find that each subgroup of NEOs (Amors, Apollos and Atens) has different observational selection effects which cause different non-uniformities in the apparent distributions of their arguments of perihelion ω, and longitudes of perihelion ̟. For their intrinsic distributions, our analysis reveals that the Apollo asteroids have non-uniform ω due to secular dynamics associated with inclination-eccentricity-ω coupling, and the Amors' ̟ distribution is peaked towards the secularly forced eccentricity vector. The Apollos' ω distribution is axial, favoring values near 0 and 180 • ; the two quadrants centered at 0 and 180 • account for 55% of the Apollos' ω values. The Amors' ̟ distribution peaks near̟ = 4 • ; sixtyone percent of Amors have ̟ within ±90 • of this peak. We show that these modest but statistically significant deviations from uniform random distributions of angular elements are owed to planetary perturbations, primarily Jupiter's. It is remarkable that this strongly chaotic population of minor planets reveals the presence of Jupiter in its angular distributions.

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Section: Argument Of Perihelionsupporting

confidence: 91%

On the non-uniform distribution of the angular elements of near-Earth objects

JeongAhn

Malhotra

2014

Icarus

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“…Intriguingly, Ohtsuka et al (2007) noted that 2007 MK 6 has a strong dynamical connection to Icarus, suggesting that these two asteroids share a common origin. Such groupings of asteroids are also recognized for Phaethon and (155140) 2005 UD (Ohtsuka et al 2006).…”

Section: Consideration Of Mass Ejection Around Perihelionmentioning

confidence: 99%

Polarimetric Study of Near-Earth Asteroid (1566) Icarus

Ishiguro

Kuroda

Watanabe

et al. 2017

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We conducted a polarimetric observation of the fast-rotating near-Earth asteroid (1566) Icarus at large phase (Sun-asteroid-observer's) angles α= 57 • -141 • around the 2015 summer solstice. We found that the maximum values of the linear polarization degree are P max =7.32±0.25 % at phase angles of α max =124 • ±8 • in the V -band and P max =7.04±0.21 % at α max =124 • ±6 • in the R C -band. Applying the polarimetric slope-albedo empirical law, we derived a geometric albedo of p V =0.25±0.02, which is in agreement with that of Q-type taxonomic asteroids. α max is unambiguously larger than that of Mercury, the Moon, and another near-Earth S-type asteroid (4179) Toutatis but consistent with laboratory samples with hundreds of microns in size. The combination of the maximum polarization degree and the geometric albedo is in accordance with terrestrial rocks with a diameter of several hundreds of micrometers. The photometric function indicates a large macroscopic roughness. We hypothesize that the unique environment (i.e., the small perihelion distance q=0.187 au and a short rotational period of T rot =2.27 hours) may be attributed to the paucity of small grains on the surface, as indicated on (3200) Phaethon.

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“…A second pair of dynamically associated asteroids in near-Earth space are the objects 1566 Icarus and 2007 MK6 (Ohtsuka et al, 2007). These objects have been associated with the Taurid-Perseid meteor complex.…”

Section: Introductionmentioning

confidence: 99%

A common origin for dynamically associated near-Earth asteroid pairs

Moskovitz

Fatka

Farnocchia

et al. 2019

Icarus

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identified and studied for over a decade, very few pair systems have been identified in the near-Earth asteroid population. We present data and analysis that supports the existence of two genetically related pairs in near-Earth space. The members of the individual systems, 2015 EE7 -2015 FP124 and 2017 SN16 -2018 RY7, are found to be of the same spectral taxonomic class, and both pairs are interpreted to have volatile-poor compositions. In conjunction with dynamical arguments, this suggests that these two systems formed via YORP spin-up and/or dissociation of a binary precursor. Backwards orbital integrations suggest a separation age of < 10 kyr for the pair 2017 SN16 -2018 RY7, making these objects amongst the youngest multiple asteroid systems known to date. A unique separation age was not realized for 2015 EE7 -2015 FP124 due to large uncertainties associated with these objects' orbits. Determining the ages of such young pairs is of great value for testing models of space weathering and asteroid spin-state evolution. As the NEO catalog continues to grow with current and future discovery surveys, it is expected that more NEO pairs will be found, thus providing an ideal laboratory for studying time dependent evolutionary processes that are relevant to asteroids throughout the Solar System.

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Apollo Asteroids 1566 Icarus and 2007 MK ₆ : Icarus Family Members?

Cited by 30 publications

References 22 publications

On the non-uniform distribution of the angular elements of near-Earth objects

On the non-uniform distribution of the angular elements of near-Earth objects

Polarimetric Study of Near-Earth Asteroid (1566) Icarus

A common origin for dynamically associated near-Earth asteroid pairs

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Apollo Asteroids 1566 Icarus and 2007 MK 6 : Icarus Family Members?

Cited by 30 publications

References 22 publications

On the non-uniform distribution of the angular elements of near-Earth objects

On the non-uniform distribution of the angular elements of near-Earth objects

Polarimetric Study of Near-Earth Asteroid (1566) Icarus

A common origin for dynamically associated near-Earth asteroid pairs

Contact Info

Product

Resources

About

Apollo Asteroids 1566 Icarus and 2007 MK ₆ : Icarus Family Members?