scholarly journals The stellar velocity distribution in the solar neighbourhood

2004 ◽  
Vol 350 (2) ◽  
pp. 627-643 ◽  
Author(s):  
Richard S. De Simone ◽  
Xiaoan Wu ◽  
Scott Tremaine
Keyword(s):  
Velocity Distribution ◽  
Solar Neighbourhood ◽  
Stellar Velocity

The kinematics and surface mass density in the solar neighbourhood using TGASxRAVE

2017 ◽  
Vol 12 (S330) ◽  
pp. 160-163
Author(s):  
Jorrit H. J. Hagen ◽  
Amina Helmi
Keyword(s):  
Velocity Distribution ◽  
Mass Density ◽  
Radial Distance ◽  
Radial Velocities ◽  
Solar Neighbourhood ◽  
Local Distribution ◽  
Surface Mass ◽  
Distance Range ◽  
Data Release ◽  
Surface Mass Density

AbstractWe investigate the kinematics of stars in the Solar neighbourhood by combining radial velocities from the latest data release of the RAVE survey with the Tycho-Gaia Astrometric Solution presented in Gaia Data Release 1. We use moments of the velocity distribution to characterise the kinematics over a radial distance range of 6-10 kpc and up to 1 kpc away from the plane. Our ultimate goal is to use these to put new constraints on the (local) distribution of mass using the Jeans Equations.

scholarly journals Velocity distribution of stars in the solar neighbourhood

1999 ◽  
Vol 308 (3) ◽  
pp. 731-740 ◽  
Author(s):  
J. Skuljan ◽  
J. B. Hearnshaw ◽  
P. L. Cottrell
Keyword(s):  
Velocity Distribution ◽  
Solar Neighbourhood

scholarly journals Kinematic structures found with Gaia DR1/TGAS and RAVE data in the Solar neighbourhood

2017 ◽  
Vol 13 (S334) ◽  
pp. 323-324
Author(s):  
I. Kushniruk ◽  
T. Schirmer ◽  
T. Bensby
Keyword(s):  
Wavelet Analysis ◽  
Velocity Distribution ◽  
Confidence Level ◽  
Solar Neighbourhood ◽  
Kinematic Structure ◽  
Proper Motions ◽  
Gaia Dr1

AbstractWith the much enlarged stellar sample of 55 831 stars and much increased precision in distances, proper motions, provided by Gaia DR1 TGAS we have shown with the help of the wavelet analysis that the velocity distribution of stars in the Solar neighbourhood contains more kinematic structures than previously known. We detect 19 kinematic structures between scales 3-16 km s−1 at the 3σ confidence level. Among them we identified well-known groups (such as Hercules, Sirius, Coma Berenices, Pleiades, and Wolf 630). We confirmed recently detected groups (such as Antoja12 and Bobylev16). In addition we report here about a new kinematic structure at (U, V) ≈ (37, 8) km s−1. Another three new groups are tentatively detected, but require confirmation.

scholarly journals Connecting Moving Groups to the Bar and Spiral Arms of the Milky Way

2009 ◽  
Vol 5 (H15) ◽  
pp. 192-192
Author(s):  
T. Antoja ◽  
O. Valenzuela ◽  
F. Figueras ◽  
B. Pichardo ◽  
E. Moreno
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Velocity Distribution ◽  
Test Particle ◽  
Milky Way ◽  
Solar Neighbourhood ◽  
Spiral Arms ◽  
Particle Orbit ◽  
Moving Groups ◽  
Orbit Integration

AbstractWe use test-particle orbit integration with a realistic Milky Way (MW) potential to study the effect of the resonances of the Galactic bar and spiral arms on the velocity distribution of the Solar Neighbourhood and other positions of the disk. Our results show that spiral arms create abundant kinematic substructure and crowd stars into the region of the Hercules moving group in the velocity plane. Bar resonances can contribute to the origin of low-angular momentum moving groups like Arcturus. Particles in the predicted dark disk of the MW should be affected by the same resonances as stars, triggering dark-matter moving groups in the disk. Finally, we evaluate how this study will be advanced by upcoming Gaia data.

Sign in / Sign up

Export Citation Format

Share Document