Die Rotation der Milchstraße

Bottlinger, K. F.

doi:10.1007/978-3-642-94252-5_2

Cited by 3 publications

(3 citation statements)

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“…These are exact formulas, and the signs of Ω follow Galactic rotation. The first of these equations was initially deduced by Bottlinger (1931), while the second one, even earlier, by Pilowski (1931), and the one for V b , -by Ogorodnikov (1948). After expanding Ω into Taylor series against the small parameter R − R0, then expanding the difference R − R0, where the distance R is…”

Section: Methodsmentioning

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: Methodsmentioning

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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“…Meanwhile, one of the intricate problems to solve today is the detection of these groups. Some of the best known methods to identify moving groups in the literature are those using kinematic diagrams, such as the Bottlinger diagram (Bottlinger 1932;Trumpler & Weaver 1953) in the U,V,W space, and Color-Magnitude (CM) diagrams (Eggen 1958(Eggen , 1959Eggen & Sandage 1959;Eggen 1960aEggen ,b, 1965bEggen , 1970Eggen , 1971aEggen ,b, 1974Eggen , 1976Eggen , 1977Eggen , 1983Eggen , 1990Eggen , 1996aSilva et al 2012). Also the method of Lynden-Bell & Lynden-Bell (1995) and of Lynden-Bell (1999) that analyses positions and velocities of globular clusters and satellite galaxies, searching for halo fossil tidal streams that mark orbits followed by satellites merging with the Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Resonant trapping in the galactic disc and halo and its relation with moving groups

Moreno

Pichardo

Schuster

2015

Monthly Notices of the Royal Astronomical Society

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With the use of a detailed Milky Way nonaxisymmetric potential, observationally and dynamically constrained, the effects of the bar and the spiral arms in the Galaxy are studied in the disc and in the stellar halo. Especially the trapping of stars in the disc and Galactic halo by resonances on the Galactic plane, induced by the Galactic bar, has been analysed in detail. To this purpose, a new method is presented to delineate the trapping regions using empirical diagrams of some orbital properties obtained in the Galactic potential. In these diagrams we plot in the inertial Galactic frame a characteristic orbital energy versus a characteristic orbital angular momentum, or versus the orbital Jacobi constant in the reference frame of the bar, when this is the only nonaxisymmetric component in the Galactic potential. With these diagrams some trapping regions are obtained in the disc and halo using a sample of disc stars and halo stars in the solar neighbourhood. We compute several families of periodic orbits on the Galactic plane, some associated with this resonant trapping. In particular, we find that the trapping effect of these resonances on the Galactic plane can extend several kpc from this plane, trapping stars in the Galactic halo. The purpose of our analysis is to investigate if the trapping regions contain some known moving groups in our Galaxy. We have applied our method to the Kapteyn group, a moving group in the halo, and we have found that this group appears not to be associated with a particular resonance on the Galactic plane.

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“…Using equations (1) to (4), we calculate the velocity perturbations of the representative stars for different collisions, each collision being characterized by a value of p and i. We then apply a method due to Bottlinger (Bottlinger, 1932(Bottlinger, , 1933 as discussed in…”

Section: Theorymentioning

confidence: 99%