Trends in wind velocity distribution using phase space trajectory

2016 ◽  
Author(s):  
S. Pratiher ◽  
S. Patra ◽  
P. Bhattacharya
Keyword(s):  
Phase Space ◽  
Velocity Distribution ◽  
Wind Velocity ◽  
Phase Space Trajectory

scholarly journals NIHAO project II: halo shape, phase-space density and velocity distribution of dark matter in galaxy formation simulations

2016 ◽  
Vol 462 (1) ◽  
pp. 663-680 ◽  
Author(s):  
Iryna Butsky ◽  
Andrea V. Macciò ◽  
Aaron A. Dutton ◽  
Liang Wang ◽  
Aura Obreja ◽  
...  
Keyword(s):  
Dark Matter ◽  
Phase Space ◽  
Velocity Distribution ◽  
Galaxy Formation ◽  
Phase Space Density ◽  
Space Density

Remaining useful life estimation for mechanical systems based on similarity of phase space trajectory

2015 ◽  
Vol 42 (5) ◽  
pp. 2353-2360 ◽  
Author(s):  
Qing Zhang ◽  
Peter Wai-Tat Tse ◽  
Xiang Wan ◽  
Guanghua Xu
Keyword(s):  
Phase Space ◽  
Mechanical Systems ◽  
Remaining Useful Life ◽  
Life Estimation ◽  
Useful Life ◽  
Phase Space Trajectory

scholarly journals Saltaion of Blown Sand Particles and Wind-Velocity Distribution

1994 ◽  
Vol 38 ◽  
pp. 621-626
Author(s):  
Tetsuro TSUJIMOTO ◽  
Satoshi SEKIJO
Keyword(s):  
Velocity Distribution ◽  
Wind Velocity ◽  
Sand Particles

Solar wind velocity distribution on the heliospheric current sheet during Carrington rotations 1787–1795

1995 ◽  
Vol 13 (8) ◽  
pp. 807
Author(s):  
B. Bala ◽  
S. R. Prabhakaran Nayar
Keyword(s):  
Solar Wind ◽  
Velocity Distribution ◽  
Current Sheet ◽  
Wind Velocity ◽  
Solar Wind Velocity ◽  
Heliospheric Current Sheet

Solar wind velocity distribution on the heliospheric current sheet during Carrington rotations 1787-1795

1995 ◽  
Vol 13 (8) ◽  
pp. 807-814
Author(s):  
B. Bala ◽  
S. R. Prabhakaran Nayar
Keyword(s):  
Solar Wind ◽  
Velocity Distribution ◽  
Current Sheet ◽  
Wind Velocity ◽  
Solar Wind Velocity ◽  
Neutral Line ◽  
Coronal Magnetic Field ◽  
Heliospheric Current Sheet ◽  
Source Surface ◽  
Low Speed

Abstract. The solar wind velocity distribution in the heliosphere is best represented using a v-map, where velocity contours are plotted in heliographic latitude-longitude coordinates. It has already been established that low-speed regions of the solar wind on the source surface correspond to the maximum bright regions of the K-corona and the neutral line of the coronal magnetic field. In this analysis, v-maps on the source surface for Carrington rotations (CRs) 1787–1795, during 1987, have been prepared using the interplanetary scintillation measurements at Research Institute of Atmospherics (RIA), Nagoya Univ., Japan. These v-maps were then used to study the time evolution of the low-speed (\\leq450 km s–1) belt of the solar wind and to deduce the distribution of solar wind velocity on the heliospheric current sheet. The low-speed belt of the solar wind on the source surface was found to change from one CR to the next, implying a time evolution. Instead of a slow and systematic evolution, the pattern of distribution of solar wind changed dramatically at one particular solar rotation (CR 1792) and the distributions for the succeeding rotations were similar to this pattern. The low-speed region, in most cases, was found to be close to the solar equator and almost parallel to it. However, during some solar rotations, they were found to be organised in certain longitudes, leaving regions with longitudinal width greater than 30° free of low-speed solar wind, i.e. these regions were occupied by solar wind with velocities greater than 450 km s–1. It is also noted from this study that the low-speed belt, in general, followed the neutral line of the coronal magnetic field, except in certain cases. The solar wind velocity on the heliospheric current sheet (HCS) varied in the range 300–585 km s–1 during the period of study, and the pattern of velocity distribution varied from rotation to rotation.

Wind velocity distribution measurement by PIV around the flat plate object on railway track

2019 ◽  
Vol 2019 (0) ◽  
pp. S05120
Author(s):  
Takashi NAKANO ◽  
Yutaka SAKUMA ◽  
Hajime TAKAMI ◽  
Takuya MINATO ◽  
Yutaro KOBAYASHI
Keyword(s):  
Velocity Distribution ◽  
Flat Plate ◽  
Wind Velocity ◽  
Railway Track ◽  
Distribution Measurement

scholarly journals Open cluster kinematics with Gaia DR2

2018 ◽  
Vol 619 ◽  
pp. A155 ◽  
Author(s):  
C. Soubiran ◽  
T. Cantat-Gaudin ◽  
M. Romero-Gómez ◽  
L. Casamiquela ◽  
C. Jordi ◽  
...  
Keyword(s):  
Phase Space ◽  
Velocity Distribution ◽  
Radial Velocity ◽  
Galactic Plane ◽  
Open Cluster ◽  
Open Clusters ◽  
High Resolution Spectroscopy ◽  
Weighted Mean ◽  
High Quality ◽  
Young Clusters

Context. Open clusters are very good tracers of the evolution of the Galactic disc. Thanks to Gaia, their kinematics can be investigated with an unprecedented precision and accuracy. Aims. The distribution of open clusters in the 6D phase space is revisited with Gaia DR2. Methods. The weighted mean radial velocity of open clusters was determined, using the most probable members available from a previous astrometric investigation that also provided mean parallaxes and proper motions. Those parameters, all derived from Gaia DR2 only, were combined to provide the 6D phase-space information of 861 clusters. The velocity distribution of nearby clusters was investigated, as well as the spatial and velocity distributions of the whole sample as a function of age. A high-quality subsample was used to investigate some possible pairs and groups of clusters sharing the same Galactic position and velocity. Results. For the high-quality sample of 406 clusters, the median uncertainty of the weighted mean radial velocity is 0.5 km s−1. The accuracy, assessed by comparison to ground-based high-resolution spectroscopy, is better than 1 km s−1. Open clusters nicely follow the velocity distribution of field stars in the close solar neighbourhood as previously revealed by Gaia DR2. As expected, the vertical distribution of young clusters is very flat, but the novelty is the high precision to which this can be seen. The dispersion of vertical velocities of young clusters is at the level of 5 km s−1. Clusters older than 1 Gyr span distances to the Galactic plane of up to 1 kpc with a vertical velocity dispersion of 14 km s−1, typical of the thin disc. Five pairs of clusters and one group with five members might be physically related. Other binary candidates that have been identified previously are found to be chance alignments.

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