Kinematics of T Tauri Stars Close to the Sun from the Gaia DR2 Catalogue

Бобылев, В. В.

doi:10.1134/s1063773720020024

Cited by 7 publications

(5 citation statements)

References 29 publications

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“…Bobylev [5] performed a kinematic analysis of the T Tauri stars from the list by Zari et al [4]. For example, when solving the kinematic equations using only the proper motions of the stars from the PMS3 sample, the error per unit weight was σ 0 = 6.9 km s −1 .…”

Section: Parametersmentioning

confidence: 99%

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Kinematic Properties of Open Star Clusters with Data from the Gaia DR2 Catalogue

Бобылев

Bajkova

2019

Astron. Lett.

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We consider open star clusters (OSCs) with the proper motions, parallaxes, and line-of-sight velocities calculated by various authors from Gaia DR2 data. The distance scale factor has been found by analyzing the separate solutions of the basic kinematic equations to be p = 1.00 ± 0.04. It shows that the distances calculated using the parallaxes from the Gaia DR2 catalogue do not need any correction factor. We have investigated the solutions obtained from various OSC samples differing in both age and accuracy of their parallax and line-of-sight velocity measurements. The solution obtained from a sample of 930 OSCs satisfying the constraints on the age log t < 9 and the relative trigonometric parallax error <30% is recognized to be the best one, with 384 OSCs in this sample having the mean line-of-sight velocities calculated from at least three probable members of the corresponding clusters. As a result of the simultaneous solution of all the basic kinematic equations, we have found the following kinematic parameters from this sample: (U, V, W ) ⊙ = (8. 53, 11.22, 7.83) ± (0.38, 0.46, 0.32) km s −1 , Ω 0 = 28.71 ± 0.22 km s −1 kpc −1 , Ω ′ 0 = −4.100±0.058 km s −1 kpc −2 , and Ω ′′ 0 = 0.736±0.033 km s −1 kpc −3 . The linear rotation velocity at the adopted at the adopted solar distance R 0 = 8 ± 0.15 kpc is V 0 = 229.7 ± 4.6 km s −1 . An analysis of the proper motions for these 930 OSCs has shown that, apart from the rotation around the Galactic z axis, there is rotation of the entire sample around the x axis with an angular velocity of 0.48 ± 0.15 km s −1 kpc −1 differing significantly from zero.1

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Section: Parametersmentioning

confidence: 99%

“…All these stars are no farther than 500 pc from the Sun and are closely associated with the Gould Belt. Their spatial and kinematic properties were studied in detail in [5].…”

Section: Introductionmentioning

confidence: 99%

Kinematic Properties of Open Star Clusters with Data from the Gaia DR2 Catalogue

Бобылев

Bajkova

2019

Astron. Lett.

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“…The two other constants, currently denoted as C and K, characterize the radial shear and divergence of the velocity field and account for a non-axisymmetric component of the distribution of stellar velocities (Ogrodnikoff, 1932;Milne, 1935) 1 . The four constants define the local rotational properties of the kinematic vector field of stellar velocities and give us insight in the mass density profile of the galactic disc within the solar neighborhood (A and B constants) as well as allows us to evaluate the physically important parameters of the Galactic spiral density wave (C and K constants) (Bobylev and Bajkova, 2013;Bobylev, 2020).…”

Section: The Oort Constantsmentioning

confidence: 99%

The Science of Fundamental Catalogs

Kopeikin

Makarov

2021

Front. Astron. Space Sci.

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This review paper discusses the science of astrometric catalogs, their current applications and future prospects for making progress in fundamental astronomy, astrophysics and gravitational physics. We discuss the concept of fundamental catalogs, their practical realizations, and future perspectives. Particular attention is paid to the astrophysical implementations of the catalogs such as the measurement of the Oort constants, the secular aberration and parallax, and asteroseismology. We also consider the use of the fundamental catalogs in gravitational physics for testing general theory of relativity and detection of ultra-long gravitational waves of cosmological origin. PACS numbers: 04.20.Cv, 04.30.−w, 95.10.−a, 95.10.Jk, 95.30.−k.

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“…The two other constants, currently denoted as C and K, characterize the radial shear and divergence of the velocity field and account for a non-axisymmetric component of the distribution of stellar velocities [55,56] 1 . The four constants define the local rotational properties of the kinematic vector field of stellar velocities and give us insight in the mass density profile of the galactic disc within the solar neighborhood (A and B constants) as well as allows us to evaluate the physically important parameters of the Galactic spiral density wave (C and K constants) [57,58].…”

Section: Astrophysics Of Fundamental Catalogsmentioning

confidence: 99%

The Science of Fundamental Catalogs

Kopeikin,

Makarov

2021

Preprint

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This review paper discusses the science of astrometric catalogs, their current applications and future prospects for making progress in fundamental astronomy, astrophysics and gravitational physics. We discuss the concept of fundamental catalogs, their practical realizations, and future prospects. Particular attention is paid to the astrophysical implementations of the catalogs such as the measurement of the Oort constants, the secular aberration and parallax, and asteroseismology. We also consider the use of the fundamental catalogs in gravitational physics for testing general theory of relativity and detection of ultra-long gravitational waves of cosmological origin.

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Kinematics of T Tauri Stars Close to the Sun from the Gaia DR2 Catalogue

Cited by 7 publications

References 29 publications

Kinematic Properties of Open Star Clusters with Data from the Gaia DR2 Catalogue

Kinematic Properties of Open Star Clusters with Data from the Gaia DR2 Catalogue

The Science of Fundamental Catalogs

The Science of Fundamental Catalogs

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