A Semi-Numerical Expansion of the Averaged Disturbing Function for Some Very-High-Eccentricity Orbits

1989 ◽  
pp. 65-68
Author(s):  
S. Ferraz-Mello
Keyword(s):  
Disturbing Function ◽  
High Eccentricity ◽  
Very High

scholarly journals Modelling Very-High-Eccentricity Asteroidal Librations with the Andoyer Hamiltonian

1999 ◽  
Vol 172 ◽  
pp. 389-390
Author(s):  
A. Simula ◽  
S. Ferraz-Mello ◽  
C. Giordano
Keyword(s):  
Explicit Form ◽  
Main Part ◽  
Order Approximation ◽  
High Eccentricity ◽  
Order Resonance ◽  
First Order ◽  
Main Effect ◽  
Realistic Description ◽  
First Order Approximation ◽  
Very High

High-eccentricity asteroidal librations are modelled using the high-eccentricity non-planar asymmetric expansion (Roig et al 1997). This second-degree expansion gives us the potential of the perturbing forces acting on a resonant asteroid in a first order resonance in explicit form, as a quadratic polynomial in the canonical non-singular variables. Secular and short periodic perturbations are introduced in the model, giving a more realistic description of the dynamics.The reducing Sessin’s transformation (Sessin, 1981; Sessin & Ferraz-Mello, 1984) is used to include the main effect of Jupiter’s ecc entricity in the main part of the Hamiltonian. It leads to an integrable first-order approximation known as the second fundamental model for resonance (Henrard & Lemaitre 1983) or Andoyer Hamiltonian (Andoyer 1903).

scholarly journals Separated Fringe Packet Observations with the CHARA Array. III. The Very High-eccentricity Binary HR 7345

2018 ◽  
Vol 156 (4) ◽  
pp. 144
Author(s):  
C. D. Farrington ◽  
Francis C. Fekel ◽  
G. H. Schaefer ◽  
T. A. ten Brummelaar
Keyword(s):  
High Eccentricity ◽  
Chara Array ◽  
Very High

scholarly journals Eccentric grazing envelope evolution towards Type IIb supernova progenitors

2020 ◽  
Vol 497 (1) ◽  
pp. 855-864
Author(s):  
Dmitry Shishkin ◽  
Noam Soker
Keyword(s):  
Parameter Space ◽  
Binary Systems ◽  
Circular Orbits ◽  
High Eccentricity ◽  
Mass Removal ◽  
Common Envelope ◽  
Hydrogen Mass ◽  
Very High ◽  
Initial Orbit

ABSTRACT We simulate the evolution of eccentric binary systems in the frame of the grazing envelope evolution (GEE) channel for the formation of Type IIb supernovae (SNe IIb), and find that extra mass removal by jets increases the parameter space for the formation of SNe IIb in this channel. To explore the role of eccentricity and the extra mass removal by jets, we use the stellar evolutionary code mesa binary. The initial primary and secondary masses are M1, i = 15 and M2, i = 2.5 M⊙. We examine initial semimajor axes of 600–1000 R⊙, and eccentricities of e = 0–0.9. Both Roche lobe overflow (RLOF) and mass removal by jets, followed by a wind, leave a hydrogen mass in the exploding star of MH, f ≈ 0.05 M⊙, compatible with an SN IIb progenitor. When the initial orbit is not circular, the final orbit might have a very high eccentricity. In many cases, with and without the extra mass removal by jets, the system can enter a common envelope evolution (CEE) phase, and then gets out from it. For some ranges of eccentricities, the jets are more efficient in preventing the CEE. Despite the large uncertainties, extra mass removal by jets substantially increases the likelihood of the system to get out from a CEE. This strengthens earlier conclusions for circular orbits. In some cases, RLOF alone, without mass removal by jets, can form SN IIb progenitors. We estimate that the extra mass removal by jets in the GEE channel increases the number of progenitors relative to that by RLOF alone by about a factor of 2.

scholarly journals Very-High-Eccentricity Librations at Some Higher Order Resonances

1992 ◽  
Vol 152 ◽  
pp. 153-158 ◽  
Author(s):  
J.C. Klafke ◽  
S. Ferraz-Mello ◽  
T. Michtchenko
Keyword(s):  
Phase Space ◽  
Numerical Integration ◽  
Higher Order ◽  
Planar Problem ◽  
High Eccentricity ◽  
Disturbing Potential ◽  
Numerical Exploration ◽  
Numerical Integrations ◽  
Short Period ◽  
Very High

Motions near the 3:1, 4:1 and 5:2 resonances with Jupiter are studied by means of numerical integrations of a semi-analytically averaged Sun-Jupiter-asteroid planar problem. In order to have a model including the very-high-eccentricity regions of the phase space, we adopted a set of local expansions of the disturbing potential, adequate to perform the numerical exploration of regions in the phase space with eccentricities higher than 0.9 (Ferraz-Mello and Klafke, 1991). Individual solutions and qualitative results thus obtained are completely reproduced by numerical integration of the complete equations by filtering off the short-period components of these solutions.

scholarly journals The origin of retrograde hot Jupiters

2010 ◽  
Vol 6 (S276) ◽  
pp. 263-266
Author(s):  
Smadar Naoz ◽  
Will M. Farr ◽  
Yoram Lithwick ◽  
Frederic A. Rasio
Keyword(s):  
Angular Momentum ◽  
Equatorial Plane ◽  
Rotation Axis ◽  
Order Effects ◽  
High Eccentricity ◽  
Tidal Friction ◽  
Hot Jupiters ◽  
Secular Dynamics ◽  
Accurate Treatment ◽  
Very High

AbstractMany hot Jupiters are observed to be misaligned with respect to the rotation axis of the star (as measured through the Rossiter–McLaughlin effect) and some (about ~ 25%) even appear to be in retrograde orbits. We show that the presence of an additional, moderately inclined and eccentric massive planet in the system can naturally explain close, inclined, eccentric, and even retrograde orbits. We have derived a complete and accurate treatment of the secular dynamics including both the key octupole-order effects and tidal friction. The flow of angular momentum from the inner orbit to the orbit of the perturber can lead to both high eccentricities and inclinations, and even flip the inner orbit. In our treatment the component of the inner orbit's angular momentum perpendicular to the stellar equatorial plane can change sign; a brief excursion to very high eccentricity during the chaotic evolution of the inner orbit can then lead to rapid “tidal capture,” forming a retrograde hot Jupiter. Previous treatments of the secular dynamics focusing on stellar-mass perturbers would not allow for such an outcome, since in that limit the component of the inner orbit's angular momentum perpendicular to the stellar equatorial plane is strictly conserved. Thus, the inclination of the planet's orbit could not change from prograde to retrograde.

Very High Resolution Analysis of the Dynamics of a Coronal Plasmoid

1994 ◽  
Vol 144 ◽  
pp. 593-596
Author(s):  
O. Bouchard ◽  
S. Koutchmy ◽  
L. November ◽  
J.-C. Vial ◽  
J. B. Zirker
Keyword(s):  
High Resolution ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Field Of View ◽  
Small Field ◽  
High Resolution Analysis ◽  
Ccd Observations ◽  
Resolution Analysis ◽  
Very High ◽  
Small Field Of View

AbstractWe present the results of the analysis of a movie taken over a small field of view in the intermediate corona at a spatial resolution of 0.5“, a temporal resolution of 1 s and a spectral passband of 7 nm. These CCD observations were made at the prime focus of the 3.6 m aperture CFHT telescope during the 1991 total solar eclipse.

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