Local standard of rest

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In astronomy, the local standard of rest or LSR follows the mean motion of material in the Milky Way in the neighborhood of the Sun.[1] The path of this material is not precisely circular.[2] The Sun follows the solar circle (eccentricity e < 0.1 ) at a speed of about 255 km/s in a clockwise direction when viewed from the galactic north pole at a radius of ≈ 8.34 kpc[3] about the center of the galaxy near Sgr A*, and has only a slight motion, towards the Solar apex, relative to the LSR.[4][5]

The LSR velocity is anywhere from 202–241 km/s.[6] Recent very-long-baseline interferometry observations of maser emission in high mass star forming regions have placed tight constraints on combinations of kinematic parameters such as the circular orbit speed of the Sun (Θ0 + V = 255.2 ± 5.1 km/s).[3] There is significant correlation between the circular motion of the solar circle, the solar peculiar motion, and the predicted counterrotation of star-forming regions.[7] Additionally, local estimates of the velocity of the LSR based on stars in the vicinity of the Sun[8] may potentially yield different results than global estimates derived from motions relative to the Galactic center.[9]

In-line references and notes[edit]

  1. ^ Frank H Shu (1982). The Physical Universe. University Science Books. p. 261. ISBN 0-935702-05-9. 
  2. ^ James Binney, Michael Merrifield (1998). Galactic Astronomy. Princeton University Press. p. 536. ISBN 0-691-02565-7. 
  3. ^ a b Reid, M.; et al. (10 March 2014). "Trigonometric Parallaxes of High Mass Star Forming Regions: The Structure and Kinematics of the Milky Way". The Astrophysical Journal 783 (2): 130 (14pp). arXiv:arxiv:1401.5377. Bibcode:2014ApJ...783..130R. doi:10.1088/0004-637X/783/2/130. 
  4. ^ Mark Reid et al. (2008). "Mapping the Milky Way and the Local Group". In F. Combes, Keiichi Wada. Mapping the Galaxy and Nearby Galaxies. Springer. pp. 19–20. ISBN 0-387-72767-1. 
  5. ^ The Sun's peculiar motion relative to the LSR is 13.4 km/s. See, for example, Binney, J. & Merrifield, M. "§10.6". op. cit. ISBN 0-691-02565-7.  or E.E. Mamajek (2008). "On the distance to the Ophiuchus star-forming region". Astron. Nachr. AN 329: 12; §2.3. arXiv:0709.0505. Bibcode:2008AN....329...10M. doi:10.1002/asna.200710827. 
  6. ^ Steven R. Majewski1 (2008). "Precision Astrometry, Galactic Mergers, Halo Substructure and Local Dark Matter". Proceedings of IAU Symposium 248 3. arXiv:0801.4927. Bibcode:2008IAUS..248..450M. doi:10.1017/S1743921308019790. 
  7. ^ Reid, M.; et al. (20 July 2009). "Trigonometric Parallaxes of High Mass Star Forming Regions. VI. Galactic Structure, Fundamental Parameters, and Noncircular Motions". The Astrophysical Journal 700 (1): 137–148. arXiv:arxiv:0902.3913. Bibcode:2009ApJ...700..137R. doi:10.1088/0004-637X/700/1/137. 
  8. ^ Dehnen, W.; Binney, J.J. (October 1998). "Local stellar kinematics from HIPPARCOS data". Monthly Notices of the Royal Astronomical Society 298 (2): 387–394. arXiv:astro-ph/9710077. Bibcode:1998MNRAS.298..387D. doi:10.1046/j.1365-8711.1998.01600.x. 
  9. ^ Bovy, J.; et al. (10 November 2012). "The Milky Way's Circular-velocity Curve between 4 and 14 kpc from APOGEE data". The Astrophysical Journal 759 (2): 131 (20pp). arXiv:arXiv:1209.0759. Bibcode:2012ApJ...759..131B. doi:10.1088/0004-637X/759/2/131. 

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