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Accurate modelling of the low-order secondary resonances in the spin-orbit problem

Ioannis Gkolias, Christos Efthymiopoulos, Alessandra Celletti, Giuseppe Pucacco
2019 Communications in nonlinear science & numerical simulation  
We provide an analytical approximation to the dynamics in each of the three most important low order secondary resonances (1:1, 2:1, and 3:1) bifurcating from the synchronous primary resonance in the gravitational  ...  spin-orbit problem.  ...  6th order normal form in Poincaré variables for the 1:1 secondary resonance of the 1:1 primary spin-orbit resonance.  ... 
doi:10.1016/j.cnsns.2019.04.015 fatcat:cboavobrjna3xfidtlegpamjoq


Shantanu P. Naidu, Jean-Luc Margot
2015 Astronomical Journal  
We develop a fourth-order numerical integrator to simulate the coupled spin and orbital motions of two rigid bodies having arbitrary mass distributions under the influence of their mutual gravitational  ...  The variations in spin rate due to large librations also affect the analysis and interpretation of lightcurve and radar observations.  ...  This material is based upon work supported by the National Science Foundation under Grant No. AST-1211581.  ... 
doi:10.1088/0004-6256/149/2/80 fatcat:alhlki2twbadtnvscgeoszvuou

The theory of secondary resonances in the spin–orbit problem

Ioannis Gkolias, Alessandra Celletti, Christos Efthymiopoulos, Giuseppe Pucacco
2016 Monthly notices of the Royal Astronomical Society  
We study the resonant dynamics in a simple one degree of freedom, time dependent Hamiltonian model describing spin-orbit interactions.  ...  the bifurcation thresholds of the secondary resonances.  ...  The model for the study of spin-orbit resonances is introduced in Section 2; an analytical theory for the 2:1 secondary resonance of the synchronous state is given in Section 3 followed by a series of  ... 
doi:10.1093/mnras/stw752 fatcat:i6vunayzvjb25dbj6uru55nqla

The Excited Spin State of Dimorphos Resulting from the DART Impact [article]

Harrison F. Agrusa
2021 arXiv   pre-print
We also show that a fully coupled treatment of the spin and orbital evolution of both bodies is crucial to accurately model the long-term evolution of the secondary's spin state and libration amplitude  ...  Using two independent numerical codes, we recover many of the resonances predicted by the analytic model and indeed show attitude instability.  ...  The Excited Spin State of Dimorphos Resulting from the DART Impact The Excited Spin State of Dimorphos Resulting from the DART Impact and = 1 2 ∕( 1 + 2 ).  ... 
arXiv:2107.07996v2 fatcat:z2veya7lbfaxhk6ydsnu7mfnti

Effects of thermal radiation on the dynamics of binary NEAs

2005 Icarus (New York, N.Y. 1962)  
Here we explore a related effect, the "binary YORP" (BYORP), that can modify the orbit of a synchronously rotating secondary in a binary system.  ...  To estimate BYORP's strength, we subjected 100 random Gaussian spheroids to the thermal radiation model of Rubincam (2000, Radiative spin-up and spin-down of small asteroids, Icarus, 148, 2-11).  ...  Acknowledgments The authors thank Petr Pravec for allowing use of his statistical data on NEA binaries (Table 1) , David Rubincam for permitting us to reproduce Fig. 1 from his paper, and Jean-Luc Margot  ... 
doi:10.1016/j.icarus.2005.02.001 fatcat:lkjgyizcwfbefisurx5d75g3bu

Excitation of Tumbling in Phobos and Deimos [article]

Alice C. Quillen and Mckenzie Lane and Miki Nakajima and Esteban Wright
2019 arXiv   pre-print
We propose that the low orbital eccentricities of Phobos and Deimos could in part be due to spin excitation by impacts rather than tidal evolution following orbital resonance excitation.  ...  From an initially tidally locked state, we find crossing of a spin-orbit resonance with Mars or a mean motion resonance with each other does not excite tumbling in Phobos or Deimos.  ...  We acknowledge support from the NASA Summer Undergraduate Program for Planetary Research (SUPPR) internship program.  ... 
arXiv:1908.05720v1 fatcat:fw2n6gpx65db7m7s4nawogs5ua

Commission 7: Celestial Mechanics (Mécanique Céleste)

Victor A. Brumberg, Sylvio Ferraz-Mello, Andrea Milani, Martin J. Duncan, Harold F. Levison, Jacques Henrard, Haruo Yoshida
1994 Transactions of the International Astronomical Union  
In what concerns the other planets the results are the following (Laskar et al., Nature 361, 608): The present spin of Mercury is very low and apparently trapped in a 2 : 3 spin-orbit resonance; however  ...  Such models involve the second-order effects in light propagation.  ... 
doi:10.1017/s0251107x00007677 fatcat:mverzgh36bdzfpqxhauspu6h3a

Creep Tide Model for the 3-Body Problem. The rotational evolution of a circumbinary planet [article]

F. A. Zoppetti, H. Folonier, A. M. Leiva, C. Beaugé
2021 arXiv   pre-print
We find that, in this low planetary eccentricity case, the most likely final stationary rotation state is the 1:1 spin-orbit resonance, considering an arbitrary planetary viscosity inside the estimated  ...  We derive analytical expressions for the mean rotational stationary state, based on high-order power series of the semimajor axes ratio a1 /a2 and low-order expansions of the eccentricities.  ...  The authors also wish to thank the anonymous referee for helpful suggestions that greatly improved this work)  ... 
arXiv:2105.02336v1 fatcat:cwaj62ct6vbxzo32vflsi5s5um

20 Years Of Observing Campaigns Of Oj287: The Black Hole Binary Model As Witness Of The Validity Of The General Relativity

Stefano Ciprini
2016 Zenodo  
The data obtained during the last two observing multifrequency campaigns of 2004-2007 and 2015-2016, allowed to put some indirect tests of the General Relativity, under the assumption that the driving  ...  A peculiar and controversial phenomenology is the periodicity of AGN and blazars.  ...  Its timing is spin-sensitive accurate timing of the secondary BH impact flare allowed us to constrain the Kerr parameter (spinning BH) of the primary BH with a fraction of percent accuracy for the first  ... 
doi:10.5281/zenodo.163816 fatcat:2lxrhd5vinasnbsioi4awu5x2e

Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation

Davide Gerosa, Michael Kesden, Emanuele Berti, Richard O'Shaughnessy, Ulrich Sperhake
2013 Physical Review D  
This "resonant plane" is identified by the conditions ΔΦ=0 or ΔΦ=+/-180, where ΔΦ is the angle between the components of the black-hole spins in the plane orthogonal to the orbital angular momentum.  ...  If the angles ΔΦ can be accurately measured for a large sample of gravitational-wave detections, their distribution will constrain models of compact binary formation.  ...  This research was supported in part by  ... 
doi:10.1103/physrevd.87.104028 fatcat:6z6cp2eenncmziwgljgarvx2mi

Bodily tides near the 1:1 spin-orbit resonance: correction to Goldreich's dynamical model

James G. Williams, Michael Efroimsky
2012 Celestial mechanics & dynamical astronomy  
Spin-orbit coupling is often described in the "MacDonald torque" approach which has become the textbook standard.  ...  However, the stability of pseudosynchronous spin hinges upon the dissipation model.  ...  A portion of the research described in this paper was carried out at the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration  ... 
doi:10.1007/s10569-012-9446-7 fatcat:vom42y2fljcyfesmmu7zqpkqpm

Long-term capture orbits for low-energy space missions

Stefano Carletta, Mauro Pontani, Paolo Teofilatto
2018 Celestial mechanics & dynamical astronomy  
In the framework of the space debris problem, in order to mitigate the already critical situation in the Low Earth Orbit (LEO) region, and, more generally, to preserve the circumterrestrial environment  ...  Planets in mean-motion resonances (MMR) prompt the investigation of the dynamics in the framework of the three-body problem (TBP), where the families of stable periodic orbits constitute the backbone of  ...  The algorithm starts from a least squares orbit, for which an impact on Earth is possible at some epoch in the future, with a positive impact probability IP>0, as provided by the main impact monitoring  ... 
doi:10.1007/s10569-018-9843-7 fatcat:mie5p3lzircr7pxb3xj2monqqi

Tidal Dissipation in Rotating Solar‐Type Stars

G. I. Ogilvie, D. N. C. Lin
2007 Astrophysical Journal  
We calculate the excitation and dissipation of low-frequency tidal oscillations in uniformly rotating solar-type stars.  ...  However, the dependence of the results on the spin frequency, tidal frequency, and stellar model indicate that a more detailed evolutionary study including inertial and Hough waves is required.  ...  We are very grateful to Shulin Li and Christopher Tout for providing stellar interior models and assisting with their interpretation.  ... 
doi:10.1086/515435 fatcat:kcw2haamdbagvptgl72kdxst74

COMMISSION 7: Celestial Mechanics and Dynamical Astronomy

Andrea Milani, Joseph A. Burns, J. Hadjidemetriou, Z. Knežević, C. Beaugé, B. Erdi, T. Fukushima, D.C. Heggie, A. Lemaitre, A. Maciejewski, A. Morbidelli, M. Sidlichovský (+2 others)
2005 Proceedings of the International Astronomical Union  
In some cases, different orbital solutions provide similarly good fits, especially when two planets are near mean-motion resonances.  ...  The orbital fits of multi-planetary systems from radial velocity data has proved to be a complex task.  ...  In addition, the most advanced of the collisional models showed that the total mass of the Kuiper belt could be reduced to few 0.01M ⊕ , only if a very low specific disruption energy Q * is assumed; if  ... 
doi:10.1017/s1743921306004297 fatcat:grpf5keatbeqvf5tkmguuimbsa

Tidal Dissipation in Dual-Body, Highly Eccentric, and Non-synchronously Rotating Systems: Applications to Pluto-Charon and the Exoplanet TRAPPIST-1e [article]

Joe P. Renaud, Wade G. Henning, Prabal Saxena, Marc Neveu, Amirhossein Bagheri, Avi Mandell, Terry Hurford
2020 arXiv   pre-print
Order-of-magnitude differences begin to occur for e>0.6. Critically, higher-order eccentricity terms activate additional spin-orbit resonances.  ...  Finally, the assumption that short-period, solid-body exoplanets with e≳0.1 are tidally locked in their 1:1 spin-orbit resonance should be reconsidered.  ...  ACKNOWLEDGMENTS We would like to thank Michael Efroimsky for his guidance on implementing the dual-dissipation model for NSR tides.  ... 
arXiv:2010.11801v1 fatcat:6tpsvdeedneebb75smfwzhus7y
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