Bias-corrected population, size distribution, and impact hazard for the near-Earth objects

By J. S. Stuart, R. Binzel. 2004

243 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b37d2b758c4f625ef59e75e6bfa05b65c5edfd64

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Citations in the corpus

In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, methodology): “This task has already been performed in detail by Vokrouhlický et al. (2006a), so here we merely verify the performance of our code with the new parameters, namely dYORP 1⁄4 0:4; creorient 1⁄4 0:9, and cYORP 1⁄4 0:7. Even so, we found something interesting in the process of our modeling work. Using ”
The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys (2013, background): “Efforts to correct the observed asteroid distribution from observing biases have been undertaken for decades (Chapman et al. 1971, Kiang 1971, Gradie and Tedesco 1982, Gradie et al. 1989, Bus 1999, Stuart and Binzel 2004).”
Nonuniform cratering of the Moon and a revised crater chronology of the inner Solar System (2011, methodology): “Concerning the LINEAR survey, esti-6 mates of Harris, A. W. (2002) have been scaled at large sizes to the estimates7 of Stuart and Binzel (2004).”
Observed spectral properties of near-Earth objects: results for population distribution, source regions, and space weathering processes (2004, methodology): “These taxonomic results pro basic input to the debiased population model derived in companion paper(Stuart and Binzel, 2004).”
Debiased orbit and absolute-magnitude distributions for near-Earth objects (2018, unknown): “…calculation of the four-dimensional ( a, e, i, ) is non-trivial but was performed for the Spacewatch survey Bottke et al., 2002a ), for the Catalina Sky Survey G96 and 703 ites employed herein ( Jedicke et al., 2016 ), and most recently for combination of many NEO surveys ( Tricarico, 2016; 2017 ).”
THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE (2010, background): “Stuart & Binzel (2004) show a range in albedos from 0.023 to 0.63 for near Earth asteroids, leading to a 5:1 range in estimated diameters and a 125:1 range in volumes.”
Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect (2007, background): “…visual magnitude H distribution of a population of asteroids with the form 0( ) 10 HN H N β′ = , (9) where the exponential slope of the absolute magnitude distribution, β, can be converted into the power-law slope of the diameter distribution via α = 5β (see, e.g., Stuart and Binzel, 2004) .”
A NEW CHRONOLOGY FOR THE MOON AND MERCURY (2008, methodology): “The numerical multiplicative factor takes into account the correction from transient to final crater dimension (Stuart & Binzel 2004).”
PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE (2011, background): “Although considerable work has been done to debias visible surveys (e.g., Stuart & Binzel 2004; Jedicke & Metcalfe 1998; Harris 2008), IR surveys offer a complementary approach to determining the size and albedo distributions of small bodies in the Solar System.”
Nonuniform cratering of the terrestrial planets (2008, background): “While this is not completely correct (see Morbidelli et al., 2002; Stuart and Binzel, 2004) we will ignore this complication here.”
The faint young Sun problem (2012, background): “The bolometric solar luminosity is dominated by radiation in the visible spectral range originating from the Sun’s lower atmosphere which shows very little variation with solar activity [Fröhlich and Lean, 2004].”
Neptune’s Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simulations to Observations (2005, background): “The Near Earth Objects have a fairly shallow size distribution with Q = 1.95 (Stuart & Binzel 2004), while the asteroid families exhibit steeper size distributions.”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, background): “…the size-frequency distribution of kilometer-sized NEOs is shallower than one would expect from a population dominated by fresh ejecta (Morbidelli & Vokrouhlický 2003, Stuart & Binzel 2004, Bottke et al. 2005b, McEwen et al. 2005). www.annualreviews.org • The Yarkovsky and YORP Effects 159 A nn u.”
NEOWISE OBSERVATIONS OF NEAR-EARTH OBJECTS: PRELIMINARY RESULTS (2011, background): “…for NEOs derived from these visible light surveys remain uncertain (particularly for sub-kilometer objects) since these models rely upon the absolute magnitude (H) through an assumed albedo to derive size (Stuart & Binzel 2004; Morbidelli et al. 2002; Shoemaker et al. 1990; Luu & Jewitt 1998).”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, methodology): “To glean insights into plausible values, we compared the main belt population from B05 between D = 10 cm to 1 km to the known NEO population (and various constraints) over the same size range (Stokes et al., 2003; Stuart and Binzel, 2004; see Sections 5.2 and 5.4).”
INITIAL PERFORMANCE OF THE NEOWISE REACTIVATION MISSION (2014, unknown): “If taxonomic type can be ascertained, it can be used to restrict the range of probable albedos, although the correlation between taxonomic type and albedo is not foolproof (e.g. Stuart & Binzel 2004; Mainzer et al. 2011e, 2012b; Thomas et al. 2011).”