Disaggregation of small, cohesive rubble pile asteroids due to YORP

Scheeres, Daniel J.

doi:10.1016/j.icarus.2017.05.029

Cited by 26 publications

(19 citation statements)

References 51 publications

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“…Section 6.2 will discuss A-type and X-complex for which a relative increase compare to other taxonomic type/complex is observed as a function of size. The last section is about the size/density dependent disaggregation of asteroids (Scheeres 2018). This only mechanism can possibly explain the overall observed variation of the taxonomy distribution as a function of size.…”

Section: Discussionmentioning

confidence: 97%

“…Several processes leading to full or partial disaggregation of asteroids have been suggested. First, Scheeres (2018) proposed a mechanism leading to the full disruption of small asteroids when reaching a spin rate threshold. The size limit at which such full dissagregation would occur is dependent on density (R 0 ∝ 1/ρ).…”

Section: Catastrophic Disaggregation Of Asteroidsmentioning

confidence: 99%

See 1 more Smart Citation

Visible Spectroscopy from the Mission Accessible Near-Earth Object Survey (MANOS): Taxonomic Dependence on Asteroid Size

Devogèle

Moskovitz

Thirouin

et al. 2019

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The Mission Accessible Near-Earth Object Survey (MANOS) aims to observe and characterize small (mean absolute magnitude H ∼ 25 mag) Near-Earth Objects (NEOs) that are accessible by spacecraft (mean ∆v ∼ 5.7 km/s) and that make close approaches with the Earth (mean Minimum Orbital Intersection Distance MOID ∼ 0.03 AU). We present here the first results of the MANOS visible spectroscopic survey. The spectra were obtained from August 2013 to March 2018 at Lowell Observatory's Discovery Channel 4.3 meter telescope, and both Gemini North and South facilities. In total, 210 NEOs have been observed and taxonomically classified. Our taxonomic distribution shows significant variations with respect to surveys of larger objects. We suspect these to be due to a dependence of Main Belt source regions on object size. Compared to previous surveys of larger objects (Binzel et al. 2019Perna et al. 2018), we report a lower fraction of S+Q-complex asteroids of 43.8 ± 4.6%. We associate this decrease with a lack of Phocaea family members at very small size. We also report higher fractions of X-complex and A-type asteroids of 23.8 ± 3.3% and 3.8 ± 1.3% respectively due to an increase of Hungaria family objects at small size. We find a strong correlation between the Q/S ratio and perihelion distance. We suggest this correlation is due to planetary close encounters with Venus playing a major role in turning asteroids from S to Q-type. This hypothesis is supported by a similar correlation between the Q/S ratio and Venus MOID.

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Section: Discussionmentioning

confidence: 97%

Section: Catastrophic Disaggregation Of Asteroidsmentioning

confidence: 99%

Visible Spectroscopy from the Mission Accessible Near-Earth Object Survey (MANOS): Taxonomic Dependence on Asteroid Size

Devogèle

Moskovitz

Thirouin

et al. 2019

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“…At higher spin rates failure will occur in landslide at higher latitudes. Note that at this spin rate, any regolith that is separated from the surface at the equator will immediately have escape speed, and thus this cohesive limit also demarcates when an asteroid would enter its disaggregation phase Scheeres (2018). However, the failed regolith at higher latitudes will still be initially bound to the asteroid and most likely return and impact later.…”

Section: Failure Spin Rates and Latitudesmentioning

confidence: 99%

Cohesive regolith on fast rotating asteroids

Sánchez

Scheeres

2020

Icarus

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The migration of cohesive regolith on the surface of an otherwise monolithic or strong asteroid is studied using theoretical and simulation models. The theory and simulations show that under an increasing spin rate (such as due to the YORP effect), the regolith covering is preferentially lost across certain regions of the body. For regolith with little or no cohesive strength, failure occurs by landsliding from the mid latitudes of the body at high enough spin rates.As the cohesive strength of the regolith increases, failure occurs by fission of grains (or coherent chunks of grains) across a greater extent of latitudes and eventually will first occur at the equator. As the spin rate is further increased, failure regions migrate from the first failure point to higher and lower latitudes. Eventually failure will encompass the equatorial region, however there always remains a region of high latitudes (around the poles) that will not undergo failure for arbitrarily high spin rates (unless disturbed by some other phenomenon). With these results a scaling law is derived that can be used to determine whether observed asteroids could retain surface regolith grains of a given size. The implications of this for the interpretation of spectral observations of small asteroids and boulder migration on large asteroids are discussed.

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“…Now we extend their study to higher stellar masses. The spin of a minor planet evolves according to Scheeres (2007Scheeres ( , 2018…”

Section: Minor Planet Survivalmentioning

confidence: 99%

Constraining planet formation around 6–8 M⊙ stars

Veras

Tremblay

Hermes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about 3M ⊙ . However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of planetary debris crossing our line-of-sight. These signatures offer the potential to explore the efficiency of planet formation for host stars with masses up to the corecollapse boundary at ≈ 8M ⊙ , a mass regime rarely investigated in planet formation theory. Here, we establish limits on where both major and minor planets must reside around ≈ 6M ⊙ − 8M ⊙ stars in order to survive into the white dwarf phase. For this mass range, we find that intact terrestrial or giant planets need to leave the main sequence beyond approximate minimum star-planet separations of respectively about 3 and 6 au. In these systems, rubble pile minor planets of radii 10, 1.0, and 0.1 km would have been shorn apart by giant branch radiative YORP spin-up if they formed and remained within, respectively, tens, hundreds and thousands of au. These boundary values would help distinguish the nature of the progenitor of metal-pollution in white dwarf atmospheres. We find that planet formation around the highest mass white dwarf progenitors may be feasible, and hence encourage both dedicated planet formation investigations for these systems and spectroscopic analyses of the highest mass white dwarfs.

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Disaggregation of small, cohesive rubble pile asteroids due to YORP

Cited by 26 publications

References 51 publications

Visible Spectroscopy from the Mission Accessible Near-Earth Object Survey (MANOS): Taxonomic Dependence on Asteroid Size

Visible Spectroscopy from the Mission Accessible Near-Earth Object Survey (MANOS): Taxonomic Dependence on Asteroid Size

Cohesive regolith on fast rotating asteroids

Constraining planet formation around 6–8 M⊙ stars

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