Detection of amino acids on thin-layer plates

Laskar, Subrata; Basak, Bidyut

doi:10.1016/s0021-9673(00)94594-1

Cited by 81 publications

(90 citation statements)

References 8 publications

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“…Over its range, this solution presents only small differences with the secular solutions of Laskar (1988Laskar ( , 1990) (see Laskar et al 1992). The orbital motion of the full Solar System was computed over 100 Myr by Sussman & Wisdom (1992) using a symplectic integrator with mixed variables (Wisdom & Holman 1991), confirming the chaotic behavior found by Laskar (1989Laskar ( , 1990.…”

Section: Introductionsupporting

confidence: 53%

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La2010: a new orbital solution for the long-term motion of the Earth

Laskar

Fienga

Gastineau

et al. 2011

A&A

734

763

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We present here a new solution for the astronomical computation of the orbital motion of the Earth spanning from 0 to −250 Myr. The main improvement with respect to our previous numerical solution La2004 is an improved adjustment of the parameters and initial conditions through a fit over 1 Myr to a special version of the highly accurate numerical ephemeris INPOP08 (Intégration Numérique Planétaire de l'Observatoire de Paris). The precession equations have also been entirely revised and are no longer averaged over the orbital motion of the Earth and Moon. This new orbital solution is now valid over more than 50 Myr in the past or into the future with proper phases of the eccentricity variations. Owing to the chaotic behavior, the precision of the solution decreases rapidly beyond this time span, and we discuss the behavior of various solutions beyond 50 Myr. For paleoclimate calibrations, we provide several different solutions that are all compatible with the most precise planetary ephemeris. We have thus reached the time where geological data are now required to discriminate between planetary orbital solutions beyond 50 Myr.

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Section: Introductionsupporting

confidence: 53%

“…For paleoclimate studies, the most widely used orbital solutions are nowadays either the averaged solution of Laskar (1988) and Laskar et al (1993b) or the numerical solution of Laskar et al (2004).…”

Section: Introductionmentioning

confidence: 99%

La2010: a new orbital solution for the long-term motion of the Earth

Laskar

Fienga

Gastineau

et al. 2011

A&A

734

763

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show abstract

“…This model uses a four-term quasi-periodic model for the orbital variations of Venus (Laskar 1988). The two-resonance model and the full simulation are in satisfactory agreement.…”

Section: Enusmentioning

confidence: 83%

“…Modeling the variation of EarthÏs orbit by the Ðrst four terms in the quasi-periodic series of Laskar (1988), we Ðnd the evolution of the core o †set angle shown in Figure 12. The total dissipated energy is 3.74 ] 1025 J.…”

Section: Simulation Resultsmentioning

confidence: 99%

Nonlinear Core-Mantle Coupling

Touma

Wisdom

2001

The Astronomical Journal

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We explore the nonlinear dynamics of a forced core-mantle system. We show that the free axisymmetric motion of a uniform-vorticity Ñuid core coupled to a rigid mantle (the model) is Poincare-Hough integrable. We derive an approximate Hamiltonian for the core tilt mode that includes the leading nonlinear contribution. We then include gravitational perturbations in the analysis. We identify the principal nonlinear prograde and retrograde resonances and the characteristic excitation associated with each. We compare the nonlinear excitation with the excitation expected in the corresponding linear model. The nonlinear model indicates that for each principal commensurability there are multiple overlapping resonances, and so varying degrees of chaotic behavior are predicted. Chaotic behavior at the principal coremantle commensurabilities is conÐrmed with surfaces of section. We then present the results of numerical evolutions done with a generalization of our (1994) Lie-Poisson integrator to allow for a Poincarecore, core-mantle friction, and tidal dissipation. We use our analytical and numerical models to Hough explore the evolution of Earth through the prograde core-mantle resonances and to explore the evolution of Venus through the retrograde resonances. Heating of the core-mantle boundary during resonance passage is much greater for Venus than for Earth. We raise the question whether heating during coremantle resonance passage could be responsible for the global resurfacing of Venus.

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“…The proper frequencies were computed with the frequency modified Fourier transform method of Laskar (1988Laskar ( , 1990Laskar ( , 1993, using an algorithm also described in Šidlichovský & Nesvorný (1997). A list of the first 39 most massive asteroids is given in Table A.1.…”

Section: The Indirect Effect Of Other Massive Asteroids: Choosing Thementioning

confidence: 99%

Chaotic diffusion caused by close encounters with several massive asteroids

Carruba

Huaman

Domingos

et al. 2013

A&A

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Context. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families.

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Detection of amino acids on thin-layer plates

Cited by 81 publications

References 8 publications

La2010: a new orbital solution for the long-term motion of the Earth

La2010: a new orbital solution for the long-term motion of the Earth

Nonlinear Core-Mantle Coupling

Chaotic diffusion caused by close encounters with several massive asteroids

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