scholarly journals Non-principal axis rotation in binary asteroid systems and how it weakens the BYORP effect

Icarus ◽  
2022 ◽  
Vol 374 ◽  
pp. 114826
Author(s):  
Alice C. Quillen ◽  
Anthony LaBarca ◽  
YuanYuan Chen
Keyword(s):  
Principal Axis ◽  
Binary Asteroid ◽  
Axis Rotation

scholarly journals NEA rotations and binaries

2006 ◽  
Vol 2 (S236) ◽  
pp. 167-176 ◽  
Author(s):  
Petr Pravec ◽  
A. W. Harris ◽  
B. D. Warner
Keyword(s):  
Binary Systems ◽  
Principal Axis ◽  
Spin Distribution ◽  
Rotation Periods ◽  
System A ◽  
Binary Formation ◽  
Basic Spin ◽  
Axis Rotation ◽  
Near Earth Asteroids ◽  
Abundant Population

AbstractOf the nearly 3900 near-Earth asteroids (NEAs) known as of June 2006, 325 have estimated rotation periods, with most of those determined by lightcurve analysis led by a few dedicated programs. NEAs with diameters down to 10 meters have been sampled. Observed spin distribution shows a major changing point around diameter of 200 meters. Larger NEAs show a barrier against spins faster than 11 d−1 (period about 2.2 h) that shifts to slower rates (longer periods) with increasing lightcurve amplitude (i.e., with increasing equatorial elongation). The spin barrier is interpreted as a critical spin rate for bodies in a gravity regime; NEAs larger than 200 meters are predominantly bodies with tensile strength too low to withstand a centrifugal acceleration for rotation faster than the critical spin rate. The cohesionless spin barrier disappears at sizes less than 200 meters where most objects rotate too fast to be held together by self-gravitation only, so a cohesion is implied in the smaller NEAs.The distribution of NEA spin rates in the cohesionless size range (D0.2 km) is highly non-Maxwellian, suggesting that mechanisms other than just collisions have been at work. There is a pile up just in front of the barrier, at periods 2–3 h. It may be related to a spin up mechanism crowding asteroids to the barrier. An excess of slow rotators is observed at periods longer than 30 hours. A spin-down mechanism has no obvious lower limit on spin rate; periods as long as tens of days have been observed.Most NEAs appear to be in their basic spin states with rotation around principal axis with maximum moment of inertia. Tumbling objects (i.e., bodies in excited, non-principal axis rotation) are present and actually predominate among slow rotators with estimated damping timescales longer than the age of the solar system. A few tumblers observed among fast rotating coherent objects appear to be either more rigid or younger than the larger (cohesionless) tumblers.An abundant population of binary systems has been found among NEAs. The fraction of binaries among NEAs larger than 0.3 km has been estimated to be 15 ± 4%. Primaries of binary systems concentrate at fast spin rates (periods 2–3 h) and low amplitudes, i.e., they lie just below the cohesionless spin barrier. The total angular momentum content in binary systems suggests that they formed from parent bodies spinning at the critical rate. The fact that a very similar population of binaries has been found among small main belt asteroids suggests a binary formation mechanism that may not be related to close encounters with the terrestrial planets.

Periodic motion near non-principal-axis rotation asteroids

2017 ◽  
Vol 471 (3) ◽  
pp. 3234-3244 ◽  
Author(s):  
Haibin Shang ◽  
Xiaoyu Wu ◽  
Xiao Qin ◽  
Dong Qiao
Keyword(s):  
Periodic Motion ◽  
Principal Axis ◽  
Axis Rotation

Principal axis rotation of magnetoresistance in α-EDT-TTF[Ni(dmit)2] salt

1993 ◽  
Vol 86 (1) ◽  
pp. 7-10 ◽  
Author(s):  
H. Tajima ◽  
S. Ikeda ◽  
A. Kobayashi ◽  
H. Kuroda ◽  
R. Kato ◽  
...  
Keyword(s):  
Principal Axis ◽  
Axis Rotation

Principal axis rotation of magnetoresistance in α-EDT-TTF[Ni(dmit)2] salt

1993 ◽  
Vol 56 (1) ◽  
pp. 2323-2328 ◽  
Author(s):  
H. Tajima ◽  
S. Ikeda ◽  
A. Kobayashi ◽  
H. Kuroda ◽  
R. Kato ◽  
...  
Keyword(s):  
Principal Axis ◽  
Axis Rotation

scholarly journals Asteroid Spins: From the Very Fast to the Very Slow

1997 ◽  
Vol 165 ◽  
pp. 265-268
Author(s):  
A. W. Harris ◽  
W.Z. Wisniewski
Keyword(s):  
Solar System ◽  
Time Scale ◽  
Rotation Rate ◽  
Principal Axis ◽  
Ccd Photometry ◽  
Radar Observations ◽  
The Earth ◽  
Axis Rotation

The application of CCD photometry to monitoring the light variations of very small asteroids has led to an explosion of data available, and perhaps as importantly, has made it possible to probe fainter, and hence smaller asteroids. In this paper, we review several new results from the analysis of such lightcurve data, much of it taken by the late W. Z. Wisniewski, a native of Poland who studied at Poznan University (Wisniewski et al., 1997).At the time of the last close pass of the asteroid 4179 Toutatis by the Earth in 1992, it became apparent from radar observations that the asteroid was in a bizarre rotation state, and that the rotation rate was extremely slow. Harris (1994), re-evaluating the work by Burns and Safronov (1973) found that very small and slowly rotating asteroids can have a time scale of damping into a principal-axis rotation state which is long compared to their expected collisional lifetime, or for that matter, the age of the solar system:

scholarly journals Interplay between tilted and principal axis rotation

2014 ◽  
Author(s):  
Pradip Datta ◽  
Santosh Roy ◽  
S. Chattopadhyay
Keyword(s):  
Principal Axis ◽  
Axis Rotation

scholarly journals Shape model and spin state of non-principal axis rotator (5247) Krylov

2020 ◽  
Vol 635 ◽  
pp. A137
Author(s):  
H.-J. Lee ◽  
J. Ďurech ◽  
M.-J. Kim ◽  
H.-K. Moon ◽  
C.-H. Kim ◽  
...  
Keyword(s):  
Physical Model ◽  
Spin State ◽  
Principal Axis ◽  
Light Curves ◽  
Infrared Light ◽  
Inversion Method ◽  
Wide Field ◽  
Angular Momentum Vector ◽  
Axis Rotation ◽  
Vector Orientation

Context. The study of non-principal axis (NPA) rotators can provide important clues to the evolution of the spin state of asteroids. However, very few studies to date have focused on NPA-rotating main belt asteroids (MBAs). One MBA known to be in an excited rotation state is asteroid (5247) Krylov. Aims. By using disk-integrated photometric data, we construct a physical model of (5247) Krylov including shape and spin state. Methods. We applied the light curve convex inversion method employing optical light curves obtained by using ground-based telescopes in three apparitions during 2006, 2016, and 2017, along with infrared light curves obtained by the Wide-field Infrared Survey Explorer satellite in 2010. Results. Asteroid (5247) Krylov is spinning in a short axis mode characterized by rotation and precession periods of 368.7 and 67.27 h, respectively. The angular momentum vector orientation of Krylov is found to be λL = 298° and βL = −58°. The ratio of the rotational kinetic energy to the basic spin-state energy E∕E0 ≃ 1.02 shows that the (5247) Krylov is about 2% excited state compared to the principal axis rotation state. The shape of (5247) Krylov can be approximated by an elongated prolate ellipsoid with a ratio of moments of inertia of Ia : Ib : Ic = 0.36 : 0.96 : 1. This is the first physical model of an NPA rotator among MBAs. The physical processes that led to the current NPA rotation cannot be unambiguously reconstructed.

scholarly journals GEOMETRIC INTERPRETATION INERTIA MOMENT CORRELATION AT CENTROIDAL PRINCIPAL AXIS ROTATION

2018 ◽  
pp. 111-118
Author(s):  
P. S. Ivanov ◽  
A. S. Plyaskin
Keyword(s):  
Internal Structure ◽  
Principal Axis ◽  
Geometric Interpretation ◽  
Theoretical Studies ◽  
Trigonometric Functions ◽  
Inertia Moment ◽  
New Approaches ◽  
The Creation ◽  
Axis Rotation ◽  
Practical Implications

One of the directions of further building development and improvement is the creation of structures with a complex internal structure, i. e. combined sections made of various materials operating in a single construction. It is necessary to search for new engineering methods that take into account the behavior of such structures. Trigonometric functions of in ertia moments not only increase the efficiency of computations, especially for complex resistance, but also provide new approaches to the development of engineering methods of building calculation with a complex internal structure.Objective: The aim of this work is to increase the calculation range for formulas of determining the ratios of inertia moments based on the transformation of trigonometric functions.Results: A new application of inertia ratios is proposed for the use of trigonometric functions.Practical implications: The results of theoretical studies can be used in the development of engineering methods for building calculations with a complex internal structure.

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