The Planet "X " Theoretical Calculation of The mean Orbital Velocity & Orbital Period

2020 ◽  
Vol 1 (1) ◽  
pp. 10-25
Author(s):  
Mostafa Sayed
Keyword(s):  
Theoretical Calculation ◽  
Orbital Period ◽  
Orbital Velocity ◽  
The Mean ◽  
Planet X

scholarly journals Age Dependent Angular Momentum, Orbital Period and Total Mass of Detached Binaries

2011 ◽  
Vol 7 (S282) ◽  
pp. 464-465
Author(s):  
O. Demircan ◽  
M. Tüysüz ◽  
F. Soydugan ◽  
S. Bilir
Keyword(s):  
Mass Transfer ◽  
Orbital Period ◽  
Total Mass ◽  
Main Sequence ◽  
Space Velocity ◽  
Angular Momenta ◽  
Age Dependent ◽  
The Mean ◽  
Orbital Periods ◽  
Detached Binaries

AbstractThe orbital angular momenta OAM (J) of detached binaries (including both cool and hot binaries) were estimated and nine subgroups were formed according to their OAM (J) distribution. The mean kinematical ages of all subgroups have been estimated by using their space velocity distributions and, thus, the age dependent variations of the mean OAM (J), orbital period (P), and total mass (M) of all subgroups were investigated. It was discovered that: i) The orbital period of detached binaries with radiative components decrease very slowly during the main sequence (MS) evolution. It is interesting that the large amount of mass loss is almost balanced by the OAM loss, and not much change in the orbital periods is observed. ii) The nuclear evolution of radiative components beyond the MS initiates the increase of the periods until the components have convective upper layers, i.e. until they become later than F5 IV, and the system becomes a cool binary with sub-giant or giant components. iii) The large co-rotating distance of the magnetically-driven wind in cool binaries (CAB) carries out a large amount of OAM and then the periods of such binaries decrease significantly, and the orbits shrink until another effect such as mass transfer dominates the period changes.

scholarly journals Systematics of Dwarf Novae

1987 ◽  
Vol 93 ◽  
pp. 3-13
Author(s):  
B. Warner
Keyword(s):  
Orbital Period ◽  
Strong Correlation ◽  
Absolute Magnitude ◽  
Dwarf Novae ◽  
Maximum Light ◽  
Wide Scatter ◽  
The Mean ◽  
Tight Correlation

AbstractFrom about 30 Dwarf Novae with the best determined distances the following relationships are found.(i)a tight correlation between absolute magnitude at maximum light, Mv (max), and orbital period, P.(ii)a correlation between Mv (min) and P showing wide scatter.(iii)a correlation between Mv (mean), the mean absolute magnitude averaged over normal outbursts, and P, again with wide scatter. The scatter is shown to correlate strongly with outburst timescale Tn.(iv)a strong correlation between range, Mv (min) - Mv (max), and Tn (the Kukarkin-Parenago relationship).(v)a strong correlation between range My. (mean) - Mv (max), and both Tn and P.This final correlation is interpreted in terms of the disc instability model of dwarf novae and successfully predicts the observed width of outburst versus P relationship.

scholarly journals Superoutburst of a New Sub-Period-Minimum Dwarf Nova CSS130418 in Hercules

2015 ◽  
Vol 2 (1) ◽  
pp. 165-169 ◽  
Author(s):  
D. Chochol ◽  
S. Shugarov ◽  
N. Katysheva ◽  
I. Volkov ◽  
A. Zharova ◽  
...  
Keyword(s):  
Accretion Disk ◽  
Stellar Evolution ◽  
Orbital Period ◽  
Late Stage ◽  
Cataclysmic Variables ◽  
Light Curves ◽  
Dwarf Nova ◽  
The Mean ◽  
Normal Hydrogen

Multicolour photometry of a new dwarf nova CSS130418 in Hercules, which underwent superoutburst on April 18, 2013, allow to classified it as a WZ Sge-type dwarf nova. The phase light curves for different stages of superoutburst are presented. The early superhumps were used to determine the orbital period P<sub>orb</sub> = 64.84(1) minutes, which is shorter than the period minimum ~78 minutes for normal hydrogen-rich cataclysmic variables. We found the mean period of ordinary superhumps P<sub>sh</sub> = 65.559(1) minutes. The quiescent spectrum is rich in helium, showing double peaked emission<br />lines of H I and He I from accretion disk, so the dwarf nova is in a late stage of stellar evolution.

Outbursts of Southern Dwarf Novae

1979 ◽  
Vol 46 ◽  
pp. 89-95
Author(s):  
Frank M. Bateson
Keyword(s):  
Orbital Period ◽  
Dwarf Novae ◽  
The Mean ◽  
Rate Of Decline ◽  
Different Levels ◽  
Visual Observations

Abstract.The mean cycles and types of maxima for a number of dwarf novae are tabulated. It is shown that supermaxima are not confined to dwarf novae of short mean cycles. The decline rates for some stars are examined to ascertain if the orbital period, accurate to within ten percent, could be derived from visual observations. It is shown that, at least for some stars, the rate of decline differs widely at different levels of brightness, and, also, between dissimilar maxima of the same star.

scholarly journals Orbital Solutions for WZ Sagittae During Quiescence

1983 ◽  
Vol 72 ◽  
pp. 29-34
Author(s):  
Ronald L. Gilliland
Keyword(s):  
Binary System ◽  
Orbital Period ◽  
Cataclysmic Variables ◽  
Emission Feature ◽  
Fundamental Result ◽  
Model Parameters ◽  
Orbital Velocity ◽  
Upper Limit ◽  
Vast Literature ◽  
Velocity Changes

WZ Sagittae was one of the first cataclysmic variables shown to be a binary system (Kraft 1961) from spectroscopic observations. Krzeminski (1962) found that WZ Sge was an eclipsing binary with an 81 min 38 s orbital period. Krzeminski and Kraft (1964, hereafter KK) in the first of many comprehensive analyses of the WZ Sge system to appear in the literature stated “a lower limit to certain detection of orbital velocity changes for the double emission feature is 2K = 75 km s-1 .” Interpreted as an upper limit to K^ of 37.5 km s-1 this fundamental result has remained untested for two decades, although interpretations and observations of WZ Sge have led to a vast literature. Despite the lack of a well determined orbital velocity, WZ Sge is one of the most thoroughly studied cataclysmic variables. The photometric properties during quiescence have been thoroughly studied and discussed (Robinson, et al. 1978; Fabian, et al. 1978; Ritter and Schroder 1979), although a consensus on model parameters has remained elusive.

scholarly journals Spin dynamics of close-in planets exhibiting large transit timing variations

2017 ◽  
Vol 605 ◽  
pp. A37 ◽  
Author(s):  
J.-B. Delisle ◽  
A. C. M. Correia ◽  
A. Leleu ◽  
P. Robutel
Keyword(s):  
Numerical Simulations ◽  
Orbital Period ◽  
Spin Dynamics ◽  
Rotation Period ◽  
Tidal Dissipation ◽  
Link Type ◽  
Spin Evolution ◽  
Synchronous Rotation ◽  
The Mean ◽  
Good Probe

We study the spin evolution of close-in planets in compact multi-planetary systems. The rotation period of these planets is often assumed to be synchronous with the orbital period due to tidal dissipation. Here we show that planet-planet perturbations can drive the spin of these planets into non-synchronous or even chaotic states. In particular, we show that the transit timing variation (TTV) is a very good probe to study the spin dynamics, since both are dominated by the perturbations of the mean longitude of the planet. We apply our model to KOI-227 b and Kepler-88 b, which are both observed undergoing strong TTVs. We also perform numerical simulations of the spin evolution of these two planets. We show that for KOI-227 b non-synchronous rotation is possible, while for Kepler-88 b the rotation can be chaotic.

scholarly journals A Photometric and Spectroscopic Comparison of the Cataclysmic Variables on the 2 Sides of the Period Gap and at a Specific Orbital Period

1987 ◽  
Vol 93 ◽  
pp. 69-73
Author(s):  
P. Szkody
Keyword(s):  
Orbital Period ◽  
Cataclysmic Variables ◽  
Detailed Comparison ◽  
High Excitation ◽  
Accretion Rates ◽  
The Mean ◽  
Line Strengths

AbstractNew and previously existing photometric colors and spectroscopic H and He line strengths are used to compare CV disk systems below the period gap (P=80–130 min) with those directly above (P=190–240 min). Significant differences are found in the mean U-B,V-J colors and in the Hβ equivalent widths on the 2 sides of the gap. A detailed comparison from UV-IR of 3 high inclination novalike systems with periods near 3.3 hr (PG1012−029, PG1030+590 and V1315 Aql) shows similar continuum distributions (and implied mass accretion rates) but large differences in high excitation lines (HeII1640,4686;CIV1550).

scholarly journals Configuration-tree theoretical calculation of the mean-squared displacement of particles in glass formers

2019 ◽  
Vol 2019 (9) ◽  
pp. 094014 ◽  
Author(s):  
Hai-Yao Deng ◽  
Chun-Shing Lee ◽  
Matteo Lulli ◽  
Ling-Han Zhang ◽  
Chi-Hang Lam
Keyword(s):  
Theoretical Calculation ◽  
Mean Squared Displacement ◽  
The Mean

Crystallographic and N.M.R.-Relaxation Studies on Bis [{N,N'-(1,3-dimethylpropanediylidene)dianilinato}(1 - )]nickel(II)

1979 ◽  
Vol 32 (4) ◽  
pp. 727 ◽  
Author(s):  
PC Healy ◽  
MR Bendall ◽  
DM Doddrell ◽  
BW Skelton ◽  
AH White
Keyword(s):  
Theoretical Calculation ◽  
Relaxation Times ◽  
Nickel Atom ◽  
Intramolecular Interactions ◽  
Bidentate Ligands ◽  
X Ray ◽  
The Mean ◽  
Independent Molecules ◽  
Relaxation Studies

A single-crystal X-ray structure determination of bis[{N,N'-(1,3-dimethylpropanediyldene)dianilinato)(1-)]nickel(II) at 295 K shows that, within each of the two independent molecules of the complex within the structure, the nickel atom is chelated by two of the bidentate ligands and is thus four-coordinate. Because of the intramolecular interactions between the phenyl substituents of the ligands, the metal atom environments are highly irregular, although consistent between the two molecules. There are no significant deviations in the Ni-N distances from the mean of 1.965�; but the interligand N-Ni-N angles about the nickel range from 110.4 to 134.7�. A theoretical calculation of the 13C and 1H nuclear relaxation times using the X-ray-determined metal-nuclear separations reproduces the experimentally observed relaxation times for selected positions within the complex, provided ligand-centred effects are taken into account. Mathematical complexity prevents a complete theoretical calculation of the relaxation times for ligand atoms with varying distances from the nickel atom.

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