The local standard of rest and the well in the velocity distribution

2013/11/30 by Charles Francis, Erik Anderson
Physics and Astronomy · #astro-ph.GA

paper · pdf · doi:10.1007/s10569-014-9541-z

published as Celestial Mechanics and Dynamical Astronomy: Volume 118, Issue 4 (2014), Page 399-413 · Supplements and updates New Ast., 14, pp. 615-629 (arXiv:0812.4032) and AstL, 38, 5, 374-392 (arXiv:1108.4971)

arxiv created 2014/05/11 · arxiv updated 2014/05/13

Abstract

It is now recognised that the traditional method of calculating the LSR fails. We find an improved estimate of the LSR by making use of the larger and more accurate database provided by XHIP and repeating our preferred analysis from Francis & Anderson (2009a). We confirm an unexpected high value of U₀ by calculating the mean for stars with orbits sufficiently inclined to the Galactic plane that they do not participate in bulk streaming motions. Our best estimate of the solar motion with respect to the LSR (U₀, V₀, W₀) = (14.1 ± 1.1, 14.6 ± 0.4, 6.9 ± 0.1) km s^-1.

Citations

• Calculation of the local standard of rest from 20574 local stars in the New Hipparcos Reduction with known radial velocities