TY - JOUR
T1 - “Fast Rotating Near Earth Asteroids Observed with the Arecibo Planetary Radar System”
AU - Zambrano-Marin, Luisa Fernanda
AU - Howell, Ellen S.
AU - Vendittia, Flaviane Cristine Faria
AU - Marshall, Sean E.
N1 - Publisher Copyright:
© 2022 by the International Astronautical Federation (IAF). All rights reserved.
PY - 2022
Y1 - 2022
N2 - Selection of mitigation response techniques for the case of a potential asteroid impact depends primarily on the duration of time between discovery and the impact event, and secondarily on the asteroid composition and structure. Using planetary radar systems is an unsurpassed ground-based technique for obtaining some of the basic physical and dynamical properties of these objects. The Arecibo Observatory planetary radar system (S-band, 2380 MHz, 12.6 cm) observed over 800 near-Earth Asteroids through five decades of operations. Its transmitter power reached up to 1 MW (50% efficiency), during its peak performance time. Of interest to this work are the Fast Rotating Asteroids (FRAs) observed at Arecibo; FRAs are considered to be small bodies having a rotation period (P) faster than the spin barrier (~2 hours), starting at diameters (D) of less than 300 m. We selected the fastest 20 Arecibo radar-observed targets with P < 0.13 hr (~8 min). Some key measurements and calculations obtained from radar observations include: the rotation period, the circular polarization ratio, the radar albedo, astrometry corrections, and (with enough signal-to-noise) delay-Doppler imaging of the object. Taking advantage of the radar-derived rotation periods and diameters available, we compared these rotation periods with values from the Light Curve DataBase, finding a few cases where these two differ by several orders of magnitude. In such instances we take the radar-derived period as the preferred value; the apparent rotation period indicated by the bandwidth can appear slower than the object's true rotation, but not faster, providing an upper limit to the true rotation period. Asteroid cohesion required to prevent rotational disruption depends on rotation rate, composition and structure; we performed calculations for the cohesion (k) via the Drucker-Prager (D-P) cohesion criterion. Preliminary results place most of these objects needing a few to a few-hundred Pascals for k; however three cases stand out: 2014 TV, 2015 RF36 and 2017 EK, needing a k of 4.2, 4.4 and 10.2 kPa respectively. In comparison, Earth mineral aggregates are 1-100 kPa for fractured rocks and up to a few MPa for crystalline rocks. A few are seen to be much larger than those calculated for some other near-Earth objects, but close to those measured on some areas of the lunar surface (~5 kPa). The loss of Arecibo, in a time where we have a continuously growing amount of discovered objects to categorize, puts the planetary defense community at a great disadvantage in successfully mitigating a collision event.
AB - Selection of mitigation response techniques for the case of a potential asteroid impact depends primarily on the duration of time between discovery and the impact event, and secondarily on the asteroid composition and structure. Using planetary radar systems is an unsurpassed ground-based technique for obtaining some of the basic physical and dynamical properties of these objects. The Arecibo Observatory planetary radar system (S-band, 2380 MHz, 12.6 cm) observed over 800 near-Earth Asteroids through five decades of operations. Its transmitter power reached up to 1 MW (50% efficiency), during its peak performance time. Of interest to this work are the Fast Rotating Asteroids (FRAs) observed at Arecibo; FRAs are considered to be small bodies having a rotation period (P) faster than the spin barrier (~2 hours), starting at diameters (D) of less than 300 m. We selected the fastest 20 Arecibo radar-observed targets with P < 0.13 hr (~8 min). Some key measurements and calculations obtained from radar observations include: the rotation period, the circular polarization ratio, the radar albedo, astrometry corrections, and (with enough signal-to-noise) delay-Doppler imaging of the object. Taking advantage of the radar-derived rotation periods and diameters available, we compared these rotation periods with values from the Light Curve DataBase, finding a few cases where these two differ by several orders of magnitude. In such instances we take the radar-derived period as the preferred value; the apparent rotation period indicated by the bandwidth can appear slower than the object's true rotation, but not faster, providing an upper limit to the true rotation period. Asteroid cohesion required to prevent rotational disruption depends on rotation rate, composition and structure; we performed calculations for the cohesion (k) via the Drucker-Prager (D-P) cohesion criterion. Preliminary results place most of these objects needing a few to a few-hundred Pascals for k; however three cases stand out: 2014 TV, 2015 RF36 and 2017 EK, needing a k of 4.2, 4.4 and 10.2 kPa respectively. In comparison, Earth mineral aggregates are 1-100 kPa for fractured rocks and up to a few MPa for crystalline rocks. A few are seen to be much larger than those calculated for some other near-Earth objects, but close to those measured on some areas of the lunar surface (~5 kPa). The loss of Arecibo, in a time where we have a continuously growing amount of discovered objects to categorize, puts the planetary defense community at a great disadvantage in successfully mitigating a collision event.
KW - Arecibo Observatory
KW - Fast Rotators
KW - Near-Earth Asteroids
KW - Planetary Defence
KW - Planetary Radar
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M3 - Conference article
AN - SCOPUS:85167602397
SN - 0074-1795
VL - 2022-September
JO - Proceedings of the International Astronautical Congress, IAC
JF - Proceedings of the International Astronautical Congress, IAC
T2 - 73rd International Astronautical Congress, IAC 2022
Y2 - 18 September 2022 through 22 September 2022
ER -