The Maria asteroid family

Aljbaae, S.; Carruba, V.; Masiero, J.; Domingos, R. C.; Huaman, M.

doi:10.1093/mnras/stx1921

Cited by 6 publications

(3 citation statements)

References 33 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…23, with C Y E = 6.5 × 10 −5 au calculated from Eq. 20 where C = 1.1 × 10 −4 au in agreement with the results of (Aljbaae et al 2017a) for the age of the Maria family. The value of µ α = 0.87 and C EV = 4.6 × 10 −5 au calculated using Eq.…”

Section: A34 Mariasupporting

confidence: 86%

Size-dependent modification of asteroid family Yarkovsky V-shapes

Bolin

Morbidelli

Walsh

2018

A&A

View full text Add to dashboard Cite

Context. The thermal properties of the surfaces of asteroids determine the magnitude of the drift rate cause by the Yarkovsky force. In the general case of Main Belt asteroids, the Yarkovsky force is indirectly proportional to the thermal inertia, Γ. Aims. Following the proposed relationship between Γ and asteroid diameter D, we find that asteroids' Yarkovsky drift rates might have a more complex size dependence than previous thought, leading to a curved family V-shape boundary in semi-major axis, a, vs. 1/D space. This implies that asteroids are drifting faster at larger sizes than previously considered decreasing on average the known ages of asteroid families. Methods. The V-Shape curvature is determined for >25 families located throughout the Main Belt to quantify the Yarkovsky sizedependent drift rate. Results. We find that there is no correlation between family age and V-shape curvature. In addition, the V-shape curvature decreases for asteroid families with larger heliocentric distances suggesting that the relationship between Γ and D is weaker in the outer MB possibly due to homogenous surface roughness among family members. B. T. Bolin et al.: Size-dependent modification of asteroid family Yarkovsky V-shapesThe Yarkovsky force has diurnal and seasonal components, but the seasonal component has a much smaller effect on a than the diurnal component, so we assume the following form for the orbit-averaged da dt from (Rubincam 1995;Farinella et al. 1998;Vokrouhlický 1999).

show abstract

Section: A34 Mariasupporting

confidence: 86%

Size-dependent modification of asteroid family Yarkovsky V-shapes

Bolin

Morbidelli

Walsh

2018

A&A

View full text Add to dashboard Cite

show abstract

“…As reported above, the odds of asteroids from the J3:1 reaching an Eros-like orbit are ~20%, less likely than the inner main belt but not unreasonably low. Several published dynamical ages for the Maria family have suggested that it is ~2 Ga (e.g., Spoto et al, 2015;Aljbaae et al, 2017) or possibly 3 ± 1 Ga (Brož et al, 2013). The collision probability of main belt asteroids with (170) Maria is Pi = 2.923 × 10 -18 km -2 yr -1 , about 1.1 times the value used for the above age calculation.…”

Section: Interpretation Of Eros's Crater Recordmentioning

confidence: 77%

Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-explored Asteroids

Bottke

Vokrouhlický

Ballouz

et al. 2020

View full text Add to dashboard Cite

Asteroid crater retention ages have unknown accuracy because projectile-crater scaling laws are difficult to verify. At the same time, our knowledge of asteroid and crater size-frequency distributions has increased substantially over the past few decades. These advances make it possible to empirically derive asteroid crater scaling laws by fitting model asteroid size distributions to crater size distributions from asteroids observed by spacecraft. For D > 10 km diameter asteroids like Ceres, Vesta, Lutetia, Mathilde, Ida, Eros, and Gaspra, the best matches occur when the ratio of crater to projectile sizes is f ~ 10. The same scaling law applied to 0.3 < D < 2.5 km near-Earth asteroids such as Bennu, Ryugu, Itokawa, and Toutatis yield intriguing yet perplexing results. When applied to the largest craters on these asteroids, we obtain crater retention ages of ~1 billion years for Bennu, Ryugu, and Itokawa and ~2.5 billion years for Toutatis. These ages agree with the estimated formation ages of their source families, and could suggest that the near-Earth asteroid population is dominated by bodies that avoided disruption during their traverse across the main asteroid belt. An alternative interpretation is that f >> 10, which would make their crater retention ages much younger. If true, crater scaling laws need to change in a substantial way between D > 10 km asteroids, where f ~ 10, and 0.3 < D < 2.5 km asteroids, where f >> 10.

show abstract

“…Currently, there should be about ten family members larger than 1 km in diameter, and many more smaller objects, orbiting in near-Earth space. finally, Aljbaae et al (2017) found that the Maria family could contribute some objects to the NEOs population, though the contribution of bodies larger than 3 km in size should be practically zero at present.…”

Section: Families Delivering Fragments On Earthmentioning

confidence: 93%

Asteroid families: properties, recent advances, and future opportunities

Novaković

Vokrouhlický

Spoto

et al. 2022

Celest Mech Dyn Astron

View full text Add to dashboard Cite

Collisions are one of the key processes shaping planetary systems. Asteroid families are outcomes of such collision still identifiable across our solar system. The families provide a unique view of catastrophic disruption phenomena and have been in the focus of planetary scientists for more than a century. Most of them are located in the main belt, a ring of asteroids between Mars and Jupiter. Here we review the basic properties of the families, discuss some recent advances, and anticipate future challenges. This review pays more attention to dynamic aspects such as family identification, age determination, and long-term evolution. The text, however, goes beyond that. Especially, we cover the details of young families that see the major advances in the last years, and we anticipate it will develop even faster in the future. We also discuss the relevance of asteroid families for water-ice content in the asteroid belt and our current knowledge on links between families and main-belt comets. query Please check the edit made in the article title.

show abstract

The Maria asteroid family

Cited by 6 publications

References 33 publications

Size-dependent modification of asteroid family Yarkovsky V-shapes

Size-dependent modification of asteroid family Yarkovsky V-shapes

Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-explored Asteroids

Asteroid families: properties, recent advances, and future opportunities

Contact Info

Product

Resources

About