Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries

Pravec, Petr; Scheirich, P.; Vokrouhlický, David; Harris, Alan W.; Kušnirák, P.; Hornoch, K.; Pray, Donald P.; Higgins, David; Galád, A.; Világi, Jozef; Gajdoš, Š.; Kornoš, Leonard; Oey, Julian; Husárik, M.; Cooney, W. R.; Gross, John E.; Terrell, Dirk; Durkee, Russell I.; Pollock, J.; Reichart, D.; Ivarsen, K.; Haislip, J.; Lacluyzé, A.; Krugly, Yu. N.; Gaftonyuk, N.; Stephens, Robert D.; Dyvig, R.; Reddy, V.; Chiorny, V. G.; Văduvescu, O.; Longa-Peña, Penélope; Tudorica, A.; Warner, Brian D.; Masi, G.; Brinsfield, James W.; Gonçalves, R.; Brown, Peter; Krzeminski, Z.; Gerashchenko, O.; Shevchenko, V. G.; Молотов, И. Е.; Marchis, Franck

doi:10.1016/j.icarus.2011.11.026

Cited by 43 publications

(58 citation statements)

References 35 publications

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“…They propose that this is a result of YORP reorientation, before, during, or after formation, and estimate a reorientation rate for a D = 4 km object equivalent to τ obl ≈ 140 Myr. The results of Section 2 actually suggest a shorter time; scaling the curve for c/a = 0.7 in Figure 1c to the average parameters in Table 1 of Pravec et al (2012) and adopting their assumed ρ = 2500 kg m −3 , I find that τ obl can be as low as 30 Myr if Γ ≈ 300 J m −1 s −1/2 K −1 , which is a reasonable thermal inertia for a surface composed of broken rocks. None of the arguments presented here excludes YORP from playing significant roles in asteroid reshaping or binary formation.…”

Section: Discussionmentioning

confidence: 80%

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Obliquities of “top-shaped” asteroids may not imply reshaping by YORP spin-up

Statler

2015

Icarus

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The timescales over which the YORP effect alters the rotation period and the obliquity of a small asteroid can be very different, because the corresponding torques couple to different aspects of the object's shape. For nearly axisymmetric, "top-shaped" near-Earth asteroids such as 101955 Bennu, spin timescales are an order of magnitude or more longer than obliquity timescales, which are ∼ 10 5 to 10 6 yr. The observed low obliquities (near 0• or 180 • ) of top-shaped asteroids do not constitute evidence that they acquired their present shapes and spins through YORP spin-up, because low obliquities are expected regardless of the spin-up or reshaping mechanism.

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Section: Discussionmentioning

confidence: 80%

“…For inner main belt binaries, a preference for such alignments has been observed by Pravec et al (2012). They propose that this is a result of YORP reorientation, before, during, or after formation, and estimate a reorientation rate for a D = 4 km object equivalent to τ obl ≈ 140 Myr.…”

Section: Discussionmentioning

confidence: 87%

Obliquities of “top-shaped” asteroids may not imply reshaping by YORP spin-up

Statler

2015

Icarus

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“…We then receive the reflected signal, most of which has been polarized in the opposite direction (OC) upon reflection, though some of the signal, due to secondary reflections, is received with the same polarization (SC). The CW spectra are plotted in Hicks et al (1998), Hicks (1996) 2008-01-13.3 TMO 0.6-m Hicks Hicks et al (1998), Hicks (1996) 2008-01-16.0 Simeiz 1-m Gaftonyuk, Krugly Krugly et al (2002), Pravec et al (2012aPravec et al ( ) 2008 Simeiz 1-m Gaftonyuk, Krugly Krugly et al (2002), Pravec et al (2012aPravec et al ( ) 2008 Simeiz 1-m Gaftonyuk, Krugly Krugly et al (2002), Pravec et al (2012aPravec et al ( ) 2008 Simeiz 1-m Gaftonyuk, Krugly Krugly et al (2002), Pravec et al (2012aPravec et al ( ) 2008 OAVdA 0.81-m Carbognani Carbognani (2011Carbognani ( ) 2008 OAVdA 0.81-m Carbognani Carbognani (2011Carbognani ( ) 2008 Modra 0.6-m Világi, Gajdoš Galád et al (2007) Df is the Doppler frequency resolution. The thin bright peaks are due to the smaller satellites rotating much more slowly than the larger primary, constraining their entire signal to a smaller range in Doppler frequency.…”

Section: Continuous Wave Spectramentioning

confidence: 99%

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Becker

Howell

Nolan

et al. 2015

Icarus

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a b s t r a c tWe report radar observations (2380-MHz, 13-cm) by the Arecibo Observatory and optical light curves observed from eight different observatories and collected at the Ondřejov Observatory of the triple near-Earth asteroid system (153591) 2001 SN 263 . The radar observations were obtained over the course of ten nights spanning February 12-26, 2008 and the light curve observations were made throughout January 12 -March 31, 2008. Both data sets include observations during the object's close approach of 0.06558 AU on February 20th, 2008. The delay-Doppler images revealed the asteroid to be comprised of three components, making it the first known triple near-Earth asteroid. Only one other object, (136617) 1994 CC is a confirmed triple near-Earth asteroid.We present physical models of the three components of the asteroid system. We constrain the primary's pole direction to an ecliptic longitude and latitude of ð309 ; À80 Þ AE 15 . We find that the primary rotates with a period 3:4256 AE 0:0002 h and that the larger satellite has a rotation period of 13:43 AE 0:01 h, considerably shorter than its orbital period of approximately 6 days. We find that the rotation period of the smaller satellite is consistent with a tidally locked state and therefore rotates with a period of 0:686 AE 0:002 days (Fang et al. [2011]. Astron. J. 141, 154-168). The primary, the larger satellite, and the smaller satellite have equivalent diameters of 2:5 AE 0:3 km, 0:77 AE 0:12 km, 0:43 AE 0:14 km and densities of 1:1 AE 0:2 g=cm 3 ; 1:0 AE 0:4 g=cm 3 ; 2:3 AE 1:3 g=cm 3 , respectively.

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“…Among 477 mainbelt asteroids, Pravec et al (2012) found 45 binaries (i.e. the fraction of the binaries is 0.094).…”

Section: Formation Of Trans-neptunian Objects and Their Satellitesmentioning

confidence: 99%

Angular Momenta of Collided Rarefied Preplanetesimals

Ипатов¹

2012

Proc. IAU

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Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries

Cited by 43 publications

References 35 publications

Obliquities of “top-shaped” asteroids may not imply reshaping by YORP spin-up

Obliquities of “top-shaped” asteroids may not imply reshaping by YORP spin-up

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Angular Momenta of Collided Rarefied Preplanetesimals

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