Search

We determine the absolute magnitude (H) distribution (or size-frequency distribution, SFD; N ( H )∝10 αH where α is the slope of the distribution) for near-Earth objects (NEO) with 13 < H < 30 and Asteroid Retrieval Mission (ARM) targets with 27 < H < 31 that were detected by the 1 st telescope of the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS1; e.g. Kaiser et al., 2002; Kaiser, 2004; Hodapp et al., 2004). The NEO and ARM target detection efficiencies were calculated using the Greenstreet et al. (2012) NEO orbit distribution. The debiased Pan-STARRS1 NEO absolute magnitude distribution is more complex than a single slope power law - it shows two transitions - at H ∼ 16 from steep to shallow slope, and in the 21 < H < 23 interval from a shallow to steep slope, which is consistent with other recent works ( e.g. Mainzer et al., 2011c; Brown et al., 2013; Harris and D’Abramo, 2015). We fit α = 0.48 ± 0.02 for NEOs with 13 < H < 16, α = 0.33 ± 0.01 for NEOs with 16 < H < 22, and α = 0.62 ± 0.03 for the smaller objects with H > 22. There is also another change in slope from steep to shallow around H = 27. The three ARM target candidates detected by Pan-STARRS1 in one year of surveying have a corrected SFD with slope α = 0 . 40 − 0.45 + 0.33 . We also show that the window for follow up observations of small (H≳ 22) NEOs with the NASA IRTF telescope and Arecibo and Goldstone radars are extremely short - on order of days, and procedures for fast response must be implemented in order to measure physical characteristics of small Earth-approaching objects. CFHT’s MegaCam and Pan-STARRS1 have longer observing windows and are capable of following-up more NEOs due to their deeper limiting magnitudes and wider fields of view. [ABSTRACT FROM AUTHOR]

The apparent magnitude of elongated small bodies is time-dependent over their rotation phase. Therefore, previously undiscovered aspherical minor planets may experience a shape-driven selection effect in systematic surveys versus their spherical counterparts. In this study, we conduct injection-recovery exercises of synthetic asteroid lightcurves using a simple model to quantify the effect of varying axial ratio on detection efficiencies. We find that high-amplitude lightcurves are confronted with adverse selection effects for survey cadences and discovery thresholds for constructing tracklets that are representative of modern and proposed future near-Earth object searches. Furthermore, we illustrate the possible hazards of drawing population-level inferences on an underlying reservoir of elongated small bodies. If physical size and characteristic axial ratios are correlated, then size-frequency distributions may require revision at small diameters. In particular, this effect could alter the estimated populations of near-Earth objects. We conclude by discussing the applicability of our results to various other classes of solar system minor planets and interstellar interlopers, as well as discussing future work that may further interrogate this detection bias. • We perform injection-recovery simulations of asteroids with shape-driven lightcurves. • Aspherical near-Earth objects are less likely to be discovered by modern surveys. • This bias complicates determinations of underlying size-frequency distribution. [ABSTRACT FROM AUTHOR]

We present a fast method to calculate an asteroid survey’s ‘bias’ – essentially a correction factor from the observed number of objects to the actual number in the population. The method builds upon the work of Jedicke and Metcalfe (Jedicke, R., Metcalfe, T.S. [1998]. Icaurs 131, 245–260) and Granvik et al. (Granvik, M., Vaubaillon, J., Jedicke, R. [2012]. Icarus 218, 262–277) and essentially efficiently maps out the phase space of orbit elements that can appear in a field-of-view. It does so by ‘integrating’ outwards in geocentric distance along a field’s boresite from the topocentric location of the survey and calculating the allowable angular elements for each desired combination of semi-major axis, eccentricity and inclination. We then use a contour algorithm to map out the orbit elements that place an object at the edge of the field-of-view. We illustrate the method’s application to calculate the bias correction for near Earth Objects detected with the Catalina Sky Survey (Christensen, E. et al. [2012]. AAS/Division for Planetary Sciences Meeting Abstracts, vol. 44, p. 210.13; Larson, S. et al. [1998]. Bulletin of the American Astronomical Society, vol. 30, p. 1037). [ABSTRACT FROM AUTHOR]

We present the results of a Monte Carlo technique to calculate the absolute magnitudes ( H ) and slope parameters ( G ) of ∼240,000 asteroids observed by the Pan-STARRS1 telescope during the first 15 months of its 3-year all-sky survey mission. The system’s exquisite photometry with photometric errors ≲ 0.04 mag , and well-defined filter and photometric system, allowed us to derive accurate H and G even with a limited number of observations and restricted range in phase angles. Our Monte Carlo method simulates each asteroid’s rotation period, amplitude and color to derive the most-likely H and G , but its major advantage is in estimating realistic statistical + systematic uncertainties and errors on each parameter. The method was tested by comparison with the well-established and accurate results for about 500 asteroids provided by Pravec et al. (Pravec, P. et al. [2012]. Icarus 221, 365–387) and then applied to determining H and G for the Pan-STARRS1 asteroids using both the Muinonen et al. (Muinonen, K. et al. [2010]. Icarus 209, 542–555) and Bowell et al. (Bowell, E. et al. [1989]. Asteroids III, Chapter Application of Photometric Models to Asteroids. University of Arizona Press, pp. 524–555) phase functions. Our results confirm the bias in MPC photometry discovered by Jurić et al. (Jurić, M. et al. [2002]. Astrophys. J. 124, 1776–1787). [ABSTRACT FROM AUTHOR]

We present a study on the discoverability of temporarily captured orbiters (TCOs) by present day or near-term anticipated ground-based and space-based facilities. TCOs (Granvik, M., Vaubaillon, J., Jedicke, R. [2012]. Icarus 218, 262–277) are potential targets for spacecraft rendezvous or human exploration (Chyba, M., Patterson, G., Picot, G., Granvik, M., Jedicke, R., Vaubaillon, J. [2014]. J. Indust. Manage. Optim. 10, 477–501) and provide an opportunity to study the population of the smallest asteroids in the Solar System. We find that present day ground-based optical surveys such as Pan-STARRS and ATLAS can discover the largest TCOs over years of operation. A targeted survey conducted with the Subaru telescope can discover TCOs in the 0.5–1.0 m diameter size range in about 5 nights of observing. Furthermore, we discuss the application of space-based infrared surveys, such as NEOWISE, and ground-based meteor detection systems such as CAMS, CAMO and ASGARD in discovering TCOs. These systems can detect TCOs but at a uninteresting rate. Finally, we discuss the application of bi-static radar at Arecibo and Green Bank to discover TCOs. Our radar simulations are strongly dependent on the rotation rate distribution of the smallest asteroids but with an optimistic distribution we find that these systems have >80% chance of detecting a >10 cm diameter TCO in about 40 h of operation. [ABSTRACT FROM AUTHOR]

We have calculated the coherence and detectable lifetimes of synthetic near-Earth object (NEO) families created by catastrophic disruption of a progenitor as it suffers a very close Earth approach. The closest or slowest approaches yield the most violent 's-class' disruption events where the largest remaining fragment after disruption and reaccumulation retains less than 50% of the parent's mass. The resulting fragments have a 'string of pearls' configuration after their reaccummulation into gravitationally bound components (Richardson, D.C., Bottke, W.F., Love, S.G. [1998]. Icarus 134, 47-76). We found that the average absolute magnitude (H ) difference between the parent body and the largest fragment is ΔH∼1.0. The average slope of the absolute magnitude (H ) distribution, N(H) ∞ 10 (0.55±0.04) H, for the fragments in the s-class families is steeper than the slope of the NEO population (Mainzer, A., et al. [2011]. Astrophys. J. 743, 156) in the same size range. The es remain coherent as statistically significant clusters of orbits within the NEO population for an average of ̄Τc = (14.7±0.6) × 103 yr after disruption. The detectable lifetimes of tidally disrupted families are extremely short compared to the multi-Myr and -Gyr lifetimes of main belt families due to the chaotic dynamical environment in NEO space-they are detectable with the techniques developed by Fu et al. and Schunová et al. (Fu, H., Jedicke, R., Durda, D.D., Fevig, R., Binzel, R.P. [2005]. Icarus 178(2), 434-449 and Schunová, E., Granvik, M., Jedicke, R., Gronchi, G., Wainscoat, R., Abe, S. [2012]. Icarus 220, 1050-1063) for an average duration (̄Τcdet) ranging from about 2000 to about 12,000 years for progenitors in the absolute magnitude (Hp) range from 20 to 13 corresponding to diameters in the range from about 0.5 to 10 km respectively. The maximum absolute magnitude of a progenitor capable of producing an observable NEO family (i.e. detectable by our family finding technique) is Hp,max=20 (about 350 m). The short detectability lifetime explains why zero NEO families have been discovered to-date. Nonetheless, every tidal disruption event of a progenitor with diameter greater than 0.5km is capable of producing several million fragments in the 1-10 m diameter range that can contribute to temporary local density enhancements of small NEOs in Earth's vicinity. We expect that there are about 1200 objects in the steady state NEO population in this size range due to tidal disruption assuming that one 1 km diameter NEO tidally disrupts at Earth every 2500 years. These objects may be suitable targets for asteroid retrieval missions due to their Earth-like orbits with corresponding low v∞ which permits low-cost missions. The fragments from the tidal disruptions evolve into orbits that bring them into collision with terrestrial planets or the Sun or they may be ejected from the Solar System on hyperbolic orbits due to deep planetary encounters. The end-state for the fragments from a tidal disruption at Earth have ∼5× the collision probability with Earth compared to the background NEO population. [ABSTRACT FROM AUTHOR]

Abstract: We have performed a simulation of a next generation sky survey’s (Pan-STARRS 1) efficiency for detecting Earth-impacting asteroids. The steady-state sky-plane distribution of the impactors long before impact is concentrated towards small solar elongations (Chesley, S.R., Spahr T.B., 2004. In: Belton, M.J.S., Morgan, T.H., Samarashinha, N.H., Yeomans, D.K. (Eds.), Mitigation of Hazardous Comets and Asteroids. Cambridge University Press, Cambridge, pp. 22–37) but we find that there is interesting and potentially exploitable behavior in the sky-plane distribution in the months leading up to impact. The next generation surveys will find most of the dangerous impactors (>140m diameter) during their decade-long survey missions though there is the potential to miss difficult objects with long synodic periods appearing in the direction of the Sun, as well as objects with long orbital periods that spend much of their time far from the Sun and Earth. A space-based platform that can observe close to the Sun may be needed to identify many of the potential impactors that spend much of their time interior to the Earth’s orbit. The next generation surveys have a good chance of imaging a bolide like 2008 TC3 before it enters the atmosphere but the difficulty will lie in obtaining enough images in advance of impact to allow an accurate pre-impact orbit to be computed. [Copyright &y& Elsevier]

We present the results and implications of our optimized round-trip trajectories to thousands of synthetic but realistic ultra-low Δ v (≲ 8 ​km ​s−1) asteroids for the purpose of in-space resource utilization (ISRU) of water extracted from the targets. We show that our carpe diem mission scenario works — ISRU missions utilizing 'hibernating' spacecraft on loosely-bound orbits in cis-lunar space can begin soon after targets are discovered if the asteroids are rapidly characterized with accurate and precise orbits. Our algorithm identified ultra-low Δ v round-trip mission trajectories for 100% of the ISRU targets that approach to within 0.05 au of Earth. The median minimum distance between the targets and Earth during the rendezvous/mining phase is ∼ 0.23 au (∼ 115 light-seconds) while the maximum one-way communication time is ​≲ ​4 ​min. The return-trip missions have a median Δ v ∼ 2.9 ​km ​s−1 so that the typical mission returns about 50% of the extracted H 2 O to cis-lunar space. We estimate a steady-state rate of about 2 water-mining missions per year returning about 100 tonne yr−1 to the Earth-Moon system. Converting the water to LOX/LH 2 is ∼ 93% efficient, suggesting that asteroid H 2 O mining could provide ∼ 93 tonne of bipropellant to cis-lunar space on an annual basis. We applied our mission optimization algorithm to 168 known near-Earth objects (NEO) with orbital elements similar to our synthetic ultra-low Δ v population and estimate that almost 95% of the population of ultra-low Δ v NEOs remain to be discovered. •We have developed an algorithm to rapidly optimize continuous-thrust round-trip trajectories to thousands of ultra-low delta-v asteroids •We applied the technique to a realistic synthetic population of ultralow delta-v asteroids •The median return-trip mission has a delta-v of ∼2.9 ​km ​s−1 •Assuming that water is extracted from the target asteroids the typical mission could return about 50% of the mined material to cis-lunar space •Our mining mission concept could return 100 tonnes of water to cislunar space per year if coupled to an efficient asteroid survey system [ABSTRACT FROM AUTHOR]

Abstract: We present the first observational measurement of the orbit and size distribution of small Solar System objects whose orbits are wholly interior to the Earth''s (Inner Earth Objects, IEOs, with aphelion <0.983 AU). We show that we are able to model the detections of near-Earth objects (NEO) by the Catalina Sky Survey (CSS) using a detailed parameterization of the CSS survey cadence and detection efficiencies as implemented within the Jedicke et al. [Jedicke, R., Morbidelli, A., Spahr, T., Petit, J.M., Bottke, W.F., 2003. Icarus 161, 17–33] survey simulator and utilizing the Bottke et al. [Bottke, W.F., Morbidelli, A., Jedicke, R., Petit, J.-M., Levison, H.F., Michel, P., Metcalfe, T.S., 2002. Icarus 156, 399–433] model of the NEO population''s size and orbit distribution. We then show that the CSS detections of 4 IEOs are consistent with the Bottke et al. [Bottke, W.F., Morbidelli, A., Jedicke, R., Petit, J.-M., Levison, H.F., Michel, P., Metcalfe, T.S., 2002. Icarus 156, 399–433] IEO model. Observational selection effects for the IEOs discovered by the CSS were then determined using the survey simulator in order to calculate the corrected number and H distribution of the IEOs. The actual number of IEOs with (21) is () and the slope of the H magnitude distribution () for the IEOs is . The slope is consistent with previous measurements for the NEO population of [Bottke, W.F., Morbidelli, A., Jedicke, R., Petit, J.-M., Levison, H.F., Michel, P., Metcalfe, T.S., 2002. Icarus 156, 399–433] and [Stuart, J.S., Binzel, R.P., 2004. Icarus 170, 295–311]. Based on the agreement between the predicted and observed IEO orbit and absolute magnitude distributions there is no indication of any non-gravitational effects (e.g. Yarkovsky, tidal disruption) affecting the known IEO population. [Copyright &y& Elsevier]

The debiased absolute-magnitude and orbit distributions as well as source regions for near-Earth objects (NEOs) provide a fundamental frame of reference for studies of individual NEOs and more complex population-level questions. We present a new four-dimensional model of the NEO population that describes debiased steady-state distributions of semimajor axis, eccentricity, inclination, and absolute magnitude H in the range 17 <  H  < 25. The modeling approach improves upon the methodology originally developed by Bottke et al. (2000, Science 288, 2190–2194) in that it is, for example, based on more realistic orbit distributions and uses source-specific absolute-magnitude distributions that allow for a power-law slope that varies with H . We divide the main asteroid belt into six different entrance routes or regions (ER) to the NEO region: the ν 6 , 3:1J, 5:2J and 2:1J resonance complexes as well as Hungarias and Phocaeas. In addition we include the Jupiter-family comets as the primary cometary source of NEOs. We calibrate the model against NEO detections by Catalina Sky Surveys’ stations 703 and G96 during 2005–2012, and utilize the complementary nature of these two systems to quantify the systematic uncertainties associated to the resulting model. We find that the (fitted) H distributions have significant differences, although most of them show a minimum power-law slope at H  ∼ 20. As a consequence of the differences between the ER-specific H distributions we find significant variations in, for example, the NEO orbit distribution, average lifetime, and the relative contribution of different ERs as a function of H . The most important ERs are the ν 6 and 3:1J resonance complexes with JFCs contributing a few percent of NEOs on average. A significant contribution from the Hungaria group leads to notable changes compared to the predictions by Bottke et al. in, for example, the orbit distribution and average lifetime of NEOs. We predict that there are 962 − 56 + 52 ( 802 − 42 + 48 × 10 3 ) NEOs with H  < 17.75 ( H  < 25) and these numbers are in agreement with the most recent estimates found in the literature (the uncertainty estimates only account for the random component). Based on our model we find that relative shares between different NEO groups (Amor, Apollo, Aten, Atira, Vatira) are (39.4,54.4,3.5,1.2,0.3)%, respectively, for the considered H range and that these ratios have a negligible dependence on H . Finally, we find an agreement between our estimate for the rate of Earth impacts by NEOs and recent estimates in the literature, but there remains a potentially significant discrepancy in the frequency of Tunguska-sized and Chelyabinsk-sized impacts. [ABSTRACT FROM AUTHOR]

This work is dedicated to debias the Near-Earth Object (NEO) population based on observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS) telescopes. We have applied similar methods used to develop the recently released NEO model generator (NEOMOD), once debiasing the NEO population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is composed of four different telescopes. We first analyzed observational data from each of all four telescopes separately and later combined them. Our results highlight main differences between CSS and ATLAS, e.g., sky coverage and survey power at debiasing the NEO population. ATLAS has a much larger sky coverage than CSS, allowing it to find bright NEOs that would be constantly "hiding" from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H ≲ 19. With its intrinsically greater sensitivity and emphasis on observing near opposition, CSS excels in the debiasing of smaller objects. ATLAS, as an all sky survey designed to find imminent hazardous objects, necessarily spends a significant fraction of time looking at places on the sky where objects do not appear, reducing its power for debiasing the population of small objects. We estimate a NEO population completeness of ≈ 88 % − 2 % + 3 % for H < 17.75 and ≈ 36 % − 1 % + 1 % for H < 22.25. Those numbers are similar to previous estimates (within error bars for H < 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the ν 6 secular resonance is the main source of small and faint NEOs at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for larger and brighter NEOs at H = 15. • We debiased the NEO population based on the all-sky ATLAS observations. • All four ATLAS telescopes (North and South) were individually considered in the study. • We combined all four ATLAS telescopes for our new NEO population estimate. • Results were compared with NEOMOD2. • We estimate a population completeness of 88 % − 2 % + 3 % for N(H < 17.75) and 36 % − 1 % + 1 % for N(H < 22.25). [ABSTRACT FROM AUTHOR]

Our previous model (NEOMOD2) for the orbital and absolute magnitude distribution of Near Earth Objects (NEOs) was calibrated on the Catalina Sky Survey observations between 2013 and 2022. Here we extend NEOMOD2 to include visible albedo information from the Wide-Field Infrared Survey Explorer. The debiased albedo distribution of NEOs can be approximated by the sum of two Rayleigh distributions with the scale parameters p V,dark ≃ 0. 03 and p V,bright ≃ 0. 17. We find evidence for smaller NEOs having (on average) higher albedos than larger NEOs; this is likely a consequence of the size-dependent sampling of different main belt sources. These inferences and the absolute magnitude distribution from NEOMOD2 are used to construct the debiased size distribution of NEOs. We estimate 830 ± 60 NEOs with diameters D > 1 km and 20 , 000 ± 2 , 000 NEOs with D > 140 m. The new model, NEOMOD3, is available via the NEOMOD Simulator — an easy-to-operate code that can be used to generate user-defined samples (orbits, sizes and albedos) from the model. • The albedo distribution of NEOs is size and orbit dependent. • There are 830 NEOs larger than 1 km and 20,000 NEOs larger than 140 m. • The average interval between impacts of > 140 m km NEOs is 20,000 yr. [ABSTRACT FROM AUTHOR]

Abstract: We report on our search for genetically related asteroids amongst the near-Earth object (NEO) population—families of NEOs akin to the well known main belt asteroid families. We used the technique proposed by Fu et al. (Fu, H., Jedicke, R., Durda, D.D., Fevig, R. Binzel, R.P. [2005]. Icarus 178(2), 434–449) supplemented with a detailed analysis of the statistical significance of the detected clusters. Their significance was assessed by comparison to identical searches performed on 1000 ‘fuzzy-real’ NEO orbit distribution models that we developed for this purpose. The family-free ‘fuzzy-real’ NEO models maintain both the micro and macro distribution of five orbital elements (ignoring the mean anomaly). Three clusters were identified that contain four or more NEOs but none of them are statistically significant at . The most statistically significant cluster at the level contains four objects with and all members have long observational arcs and concomitant good orbital elements. Despite the low statistical significance we performed several other tests on the cluster to determine if it is likely a genetic family. The tests included examining the cluster’s taxonomy, size–frequency distribution, consistency with a family-forming event during tidal disruption in a close approach to Mars, and whether it is detectable in a proper element cluster search. None of these tests exclude the possibility that the cluster is a family but neither do they confirm the hypothesis. We conclude that we have not identified any NEO families. [Copyright &y& Elsevier]

Abstract: We have for the first time calculated the population characteristics of the Earth’s irregular natural satellites (NESs) that are temporarily captured from the near-Earth-object (NEO) population. The steady-state NES size–frequency and residence-time distributions were determined under the dynamical influence of all the massive bodies in the Solar System (but mainly the Sun, Earth, and Moon) for NEOs of negligible mass. To this end, we compute the NES capture probability from the NEO population as a function of the latter’s heliocentric orbital elements and combine those results with the current best estimates for the NEO size–frequency and orbital distribution. At any given time there should be at least one NES of 1-m diameter orbiting the Earth. The average temporarily-captured orbiter (TCO; an object that makes at least one revolution around the Earth in a co-rotating coordinate system) completes (2.88±0.82) rev around the Earth during a capture event that lasts (286±18) d. We find a small preference for capture events starting in either January or July. Our results are consistent with the single known natural TCO, 2006 RH120, a few-meter diameter object that was captured for about a year starting in June 2006. We estimate that about 0.1% of all meteors impacting the Earth were TCOs. [Copyright &y& Elsevier]

Catalina Sky Survey (CSS) is a major survey of Near-Earth Objects (NEOs). In a recent work, we used CSS observations from 2005–2012 to develop a new population model of NEOs (NEOMOD). CSS's G96 telescope was upgraded in 2016 and detected over 10,000 unique NEOs since then. Here we characterize the NEO detection efficiency of G96 and use G96's NEO detections from 2013–2022 to update NEOMOD. This resolves previous model inconsistencies related to the population of large NEOs. We estimate there are 936 ± 29 NEOs with absolute magnitude H < 17. 75 (diameter D > 1 km for the reference albedo p V = 0. 14) and semimajor axis a < 4. 2 au. The slope of the NEO size distribution for H = 25 –28 is found to be relatively shallow (cumulative index ≃ 2. 6) and the number of H < 28 NEOs (D > 9 m for p V = 0. 14) is determined to be (1. 20 ± 0. 04) × 1 0 7 , about 3 times lower than in Harris & Chodas (2021). Small NEOs have a different orbital distribution and higher impact probabilities than large NEOs. We estimate 0. 034 ± 0. 002 impacts of H < 28 NEOs on the Earth per year, which is near the low end of the impact flux range inferred from atmospheric bolide observations. Relative to a model where all NEOs are delivered directly from the main belt, the population of small NEOs detected by G96 shows an excess of low-eccentricity orbits with a ≃ 1 –1.6 au that appears to increase with H (≃ 30 % excess for H = 28). We suggest that the population of very small NEOs is boosted by tidal disruption of large NEOs during close encounters to the terrestrial planets. When the effect of tidal disruption is (approximately) accounted for in the model, we estimate 0. 06 ± 0. 01 impacts of H < 28 NEOs on the Earth per year, which is more in line with the bolide data. The impact probability of a H < 22 (D > 140 m for p V = 0. 14) object on the Earth in this millennium is estimated to be ≃ 4. 5 %. • Catalina Sky Survey observations (2013–2022) are used to update our NEO model. • There are 936 ± 29 NEOs with absolute magnitude H ¡17.75. • The population of very small NEOs is boosted by tidal disruption of large NEOs. • We estimate 0. 06 ± 0. 01 impacts of H ¡28 NEOs on the Earth per year. • The impact probability of a H ¡22 NEO on the Earth in this millennium is 4.5%. [ABSTRACT FROM AUTHOR]

Earth's temporarily-captured orbiters (TCOs) are a sub-population of near-Earth objects (NEOs). TCOs can provide constraints for NEO population models in the 1–10-metre-diameter range, and they are outstanding targets for in situ exploration of asteroids due to a low requirement on Δ v. So far there has only been a single serendipitous discovery of a TCO. Here we assess in detail the possibility of their discovery with the upcoming Large Synoptic Survey Telescope (LSST), previously identified as the primary facility for such discoveries. We simulated observations of TCOs by combining a synthetic TCO population with an LSST survey simulation. We then assessed the detection rates, detection linking and orbit computation, and sources for confusion. Typical velocities of detectable TCOs will range from 1 ∘ /day to 50 ∘ /day, and typical apparent V magnitudes from 21 to 23. Potentially-hazardous asteroids have observational characteristics similar to TCOs, but the two populations can be distinguished based on their orbits with LSST data alone. We predict that a TCO can be discovered once every year with the baseline moving-object processing system (MOPS). The rate can be increased to one TCO discovery every two months if tools complementary to the baseline MOPS are developed for the specific purpose of discovering these objects. • The discoverability of Earth's temporary moons with LSST is assessed. • With a tailored approach, a temporary moon is detected with LSST every three months. • Rapid follow-up is needed to constrain the orbit for fast in situ missions. [ABSTRACT FROM AUTHOR]