The Evaluation of Massage Skill of Palm Press Based on Dynamics and Kinematical Data

2014 ◽  
Author(s):  
Yajuan Song ◽  
Ping Feng ◽  
Xiaoli Wang ◽  
Kai Xing
Keyword(s):  
Kinematical Data

scholarly journals The Luminosity Determination

1995 ◽  
Vol 10 ◽  
pp. 399-402
Author(s):  
A.E. Gómez ◽  
C. Turon
Keyword(s):  
Main Sequence ◽  
Small Volume ◽  
Absolute Magnitude ◽  
Fitting Procedure ◽  
Trigonometric Parallaxes ◽  
The Mean ◽  
The Absolute ◽  
Absolute Magnitudes ◽  
Kinematical Data ◽  
Magnitude Determination

The Hertzprung-Russel (HR) diagram luminosity calibration relies basically on three kinds of data: trigonometric parallaxes, kinematical data (proper motions and radial velocities) and cluster distances obtained by the zero-age main sequence fitting procedure. The most fundamental method to calculate the absolute magnitude is the use of trigonometric parallaxes, but up to now, accurate data only exist for stars contained in a small volume around the sun. Individual absolute magnitudes are obtained using trigonometric parallaxes or photometric and spectroscopic calibrations. In these calibrations the accuracy on the absolute magnitude determination ranges from ±0.m2 in the main sequence to ±0m5 in the giant branch. On the other hand, trigonometric parallaxes, kinematical data or cluster distances have been used to make statistical calibrations of the absolute magnitude. The standard error on the mean absolute magnitude calibrations ranges from ±0m3 to ±0m6 on the mean sequence, from ±0m5 to ±0m7 on thegiant branch and is of about 1mfor supergiants.Future improvements in the absolute magnitude determination will depend on the improvement of the basic data from the ground and space. A brief overview of the new available data is presented. In particular, the analysis of the first 30 months data of the Hipparcos mission (H30) (from the 37 months data of the whole mission) allows to perform a statistical evaluation of the improvements expected in the luminosity determination.

scholarly journals Kinematical data on early-type galaxies. I.

1997 ◽  
Vol 122 (3) ◽  
pp. 521-528 ◽  
Author(s):  
F. Simien ◽  
Ph. Prugniel
Keyword(s):  
Early Type ◽  
Kinematical Data

scholarly journals Properties of satellite galaxies in nearby groups

2014 ◽  
Vol 11 (S308) ◽  
pp. 475-476
Author(s):  
Jaan Vennik
Keyword(s):  
Star Formation ◽  
Rest Frame ◽  
Stellar Mass ◽  
Line Of Sight ◽  
Limited Sample ◽  
Velocity Modulation ◽  
Star Forming ◽  
Relative Line ◽  
Satellite Galaxies ◽  
Kinematical Data

AbstractWe studied the variation of stellar mass and various star-formation characteristics of satellite galaxies in a volume limited sample of nearby groups as a function of their group-centric distance and of their relative line-of-sight velocity in the group rest frame. We found clear radial dependencies, e.g. massive, red and passive satellites being distributed predominantly near the center of composite group. We also found some evidence of velocity modulation of star-forming properties of satellite galaxies near the group virial radius. We conclude that using kinematical data, it should be feasible to separate dynamical classes of bound, in-falling and 'backsplash' satellite galaxies.

scholarly journals Kinematical data on early-type galaxies. VI.

2002 ◽  
Vol 384 (2) ◽  
pp. 371-382 ◽  
Author(s):  
F. Simien ◽  
Ph. Prugniel
Keyword(s):  
Early Type ◽  
Kinematical Data

scholarly journals Kinematics and dynamics of OH/IR stars

1993 ◽  
Vol 153 ◽  
pp. 73-86 ◽  
Author(s):  
H. Dejonghe
Keyword(s):  
Kinematics And Dynamics ◽  
Dynamical Models ◽  
Ir Stars ◽  
Kinematical Data

The available kinematical data on OH/IR stars is discussed, and dynamical models for the OH/IR stars are presented.

scholarly journals Probing the Halo of Centaurus A: A Merger Dynamical Model for the PN Population

1996 ◽  
Vol 171 ◽  
pp. 411-411
Author(s):  
A. Mathieu ◽  
H. Dejonghe ◽  
X. Hui
Keyword(s):  
Elliptical Galaxy ◽  
Major Axis ◽  
Minor Axis ◽  
Programming Technique ◽  
Data Set ◽  
The Galaxy ◽  
Axis Rotation ◽  
Spherical Potential ◽  
Kinematical Data ◽  
Centaurus A

We use planetary nebulae observations (Hui et al. 1995) to build dynamical models of the dust-lane elliptical galaxy NGC 5128 (Centaurus A). The PN photometric and kinematical data extend out to 20 kpc (∼ 4re) along the major axis and 10 kpc along the minor axis. Our models are built using a Quadratic Programming technique (Dejonghe 1989). The method produces fits to the data set, which consists of the photometry field (E2, well fitted by a r1/4-law) together with the major- and minor- axis rotation curves and velocity dispersion profiles. Assuming the merger hypothesis for Cen A, we describe its kinematics in a spherical potential by two sub-systems, one rotating about the intrinsic short axis and the other about the intrinsic long axis of the galaxy.

STRUCTURES OUT OF CHAOS IN BARRED-SPIRAL GALAXIES

2012 ◽  
Vol 22 (09) ◽  
pp. 1230029 ◽  
Author(s):  
P. A. PATSIS
Keyword(s):  
Near Infrared ◽  
Spiral Galaxies ◽  
Morphological Features ◽  
Infrared Images ◽  
Chaotic Motions ◽  
Spiral Arms ◽  
Gravitational Fields ◽  
Pattern Speed ◽  
Barred Spiral Galaxies ◽  
Kinematical Data

We review the dynamical mechanisms we have found to support the morphological features in barred-spiral galaxies based on chaotic motions of stars in their gravitational fields. These morphological features are the spiral arms, that emerge out of the ends of the bar, but also shape the bar itself. The potentials used have been estimated directly from near-infrared images of barred-spiral galaxies. In this paper, we present the results from the study of the dynamics of the potentials of the galaxies NGC 4314, NGC 1300 and NGC 3359. The main unknown parameter in our models is the pattern speed of the system Ωp. By varying Ωp, we have investigated several cases trying to match the results of our modeling with available photometrical and kinematical data. We found realistic models with stars on spirals in chaotic motion, while their bars are built by stars usually on regular orbits. However, we also encountered cases, where a major part of trajectories of the stars even in the bar is chaotic as well. Finally, we examined the gas dynamics of barred-spiral systems, and found that the presence of gas reinforces the intensity of the "chaotic" spiral arms.

scholarly journals A method to estimate stellar ages from kinematical data

2018 ◽  
Vol 476 (1) ◽  
pp. 184-197 ◽  
Author(s):  
F Almeida-Fernandes ◽  
H J Rocha-Pinto
Keyword(s):  
Stellar Ages ◽  
Kinematical Data

scholarly journals Galactic kinematics near the sun from open clusters

2007 ◽  
Vol 3 (S248) ◽  
pp. 502-503 ◽  
Author(s):  
M. Shen
Keyword(s):  
Rotation Curve ◽  
Thin Disk ◽  
Open Clusters ◽  
Galactic Rotation ◽  
Galactic Kinematics ◽  
The Sun ◽  
Galactic Rotation Curve ◽  
Kinematical Data ◽  
Weak Trend

AbstractA catalogue of open clusters is used to analyze the Galactic kinematics near the Sun. The Galactic open clusters, which are components of Galactic thin disk, were selected for our analysis. Based on kinematical data for around 270 Galactic open clusters, we found the Galactic rotation curve remains flat near the Sun. We also found Ve = 6.40±3.39 km s−1 inside the solar circle, which shows a weak trend of stars moving toward the Galactic anti-center.

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