The galactic structure and the appearance of the Milky Way

Pavlovskaya, E. D.; Sharov, A. S.

doi:10.1017/s0074180900000590

Cited by 1 publication

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“…This is due to the fact that nearby masers belong to the Local arm, while the OB-2.5 star sample is essentially the Gould belt (since we chose the stars with σπ/π < 10%) that is a part of the Local arm. Cepheids of different ages manifest the well-known effect -a gradient of the age across the spiral arm (Pavlovskaya & Suchkov 1978), which suggests that the spiral arm goes towards the Galactic center.…”

Section: Starsmentioning

confidence: 98%

The local standard of rest from data on young objects with account for the Galactic spiral density wave

Бобылев

Bajkova

2014

Monthly Notices of the Royal Astronomical Society

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To estimate the peculiar velocity of the Sun with respect to the Local Standard of Rest (LSR), we used young objects in the Solar neighborhood with distance measurement errors within 10%-15%. These objects were the nearest Hipparcos stars of spectral classes O-B2.5, masers with trigonometric parallaxes measured by means of VLBI, and two samples of the youngest and middle-aged Cepheids. The most significant component of motion of all these stars is induced by the spiral density wave. As a result of using all these samples and taking into account the differential Galactic rotation, as well as the influence of the spiral density wave, we obtained the following components of the vector of the peculiar velocity of the Sun with respect to the LSR: (U ⊙ , V ⊙ , W ⊙ ) LSR = (6.0, 10.6, 6.5) ± (0.5, 0.8, 0.3) km s −1 . We have found that components of the Solar velocity are quite insensitive to errors of the distance R 0 in a broad range of its values, from R 0 = 7.5 kpc to R 0 = 8.5 kpc, that affect the Galactic rotation curve parameters. In the same time, the Solar velocity components (U ⊙ ) LSR and (V ⊙ ) LSR are very sensitive to the Solar radial phase χ ⊙ in the spiral density wave.

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Section: Starsmentioning

confidence: 98%