The Kinematics and Ages of Stars in Gliese’s Catalogue

This contribution gives some results on the kinematics and ages of stars near the Sun. These results are mainly based on the catalogue of nearby stars compiled by Gliese (1957, 1969 and minor recent modifications). Table I shows the number of objects under consideration. While the old catalogue (1957) contained only stars with distances r up to 20 pc, the new edition (1969) includes many stars with slightly larger distances. In Table I, a ‘system’ is either a single star or a binary or a multiple system. The number of systems with known space velocities nearer than 20 pc has increased by about 30% from 1957 to 1969. The first edition of Gliese’s catalogue (1957) has been analyzed in detail by Gliese (1956) and von Hoerner (1960).

Desiderata for the Catalogue of Nearby Stars

10.1017/s0252921100052842 ◽

1977 ◽

Vol 35 ◽

pp. 37-39

Author(s):

W. Gliese

Keyword(s):

The Sun ◽

Royal Observatory ◽

Trigonometric Parallaxes ◽

In 1969 the second edition of the “Catalogue of Nearby Stars” was published. It contains 1529 single stars and systems with a total of 1890 components. The catalogue lists all stars with parallaxes equal to or larger than 0.”045. Only 1049 of these objects are nearer than 20 pc. The “Catalogue of Stars within 25 pc of the Sun”, published 1970 in the Royal Observatory Annals No. 5 consists of 1744 systems of which 1566 trigonometric parallaxes.

Blended Visual Binaries as Tests of Low Amplitude Orbit Detection and Determination Capability in Long-Focus Photographic Astrometry

10.1017/s0252921100009805 ◽

1983 ◽

Vol 62 ◽

pp. 45-51

Author(s):

Sarah Lee Lippincott ◽

John L. Hershey

Keyword(s):

Main Sequence ◽

Orbital Motion ◽

Orbital Elements ◽

Detection Capability ◽

Single Star ◽

Planetary Mass ◽

Residual Series ◽

Nearby Stars ◽

Low Amplitude ◽

Visual Binaries

AbstractPhotocentric orbital motions from 60-year Sproul plate series are shown for three visual binaries, ζ Her, 85 Peg and Ho 296. Mass ratios of the first two pairs, which have large-amplitude blended orbits, carry internal errors at the level of one percent. Orbital elements computed independently from the blended photographic observations agree closely with the well-determined visual orbits. Ho 296 serves as a test of the Sproul plate series to detect a 20-year orbit with an amplitude of two, or one, micron. Simulations of orbital motion in single star residual series confirm this detection capability, which corresponds to planetary mass for dark objects around nearby stars. A mass-luminosity diagram of the lower main sequence is shown, including one for invisible astrometric companions.

A New Value for the Rotation Speed of the Spiral Structure

10.1017/s0252921100067683 ◽

1977 ◽

Vol 45 ◽

pp. 293-296 ◽

Cited By ~ 1

Author(s):

J. Palouš

Keyword(s):

Surface Density ◽

Galactic Center ◽

Local Density ◽

Outer Part ◽

Density Variation ◽

The Sun ◽

Basic Model ◽

Rr Lyrae ◽

The Galaxy ◽

The basic model of our Galaxy, like the Schmidt (1965) model, obeys the density law ρ(R) for the Galaxy based on divers evidence, less or better known from observation. The interpretation of the interstellar hydrogen radio profiles yields the rotation curve and the run of the force component in the radial direction. The Oort constants A, B known from radial velocities and proper motions of nearby stars, the distance from the Sun to the galactic center Roestablished from the distances of RR Lyrae stars, the local density and density gradients in the vicinity of the Sun, known from the star counts, are involved in this basic model of the Galaxy. The r.m.s. velocity component in the z direction yields the approximate mass distribution in this direction. The model surface density is computed by integrating the density along the z direction in the model. The local surface density in the Schmidt model is 114 solar masses per pc2; it depends rather strongly on the assumed density variation in the outer part of the Galaxy.

High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun

The Astronomical Journal ◽

10.1086/514336 ◽

2007 ◽

Vol 133 (6) ◽

pp. 2524-2536 ◽

Cited By ~ 102

Author(s):

Russel J. White ◽

Jared M. Gabor ◽

Lynne A. Hillenbrand

Keyword(s):

Optical Spectra ◽

High Dispersion ◽

The Sun ◽

Investigating the dynamical history of the interstellar object ’Oumuamua

Astronomy and Astrophysics ◽

10.1051/0004-6361/201732309 ◽

2018 ◽

Vol 610 ◽

pp. L11 ◽

Cited By ~ 14

Author(s):

Piotr A. Dybczyński ◽

Małgorzata Królikowska

Keyword(s):

Solar System ◽

Numerical Results ◽

The Sun ◽

Distant Source ◽

Kinematic Data ◽

Close Encounters ◽

Nearby Stars ◽

History Of ◽

Open Question

Here we try to find the origin of 1I/2017 U1 ’Oumuamua, the first interstellar object recorded inside the solar system. To this aim, we searched for close encounters between ’Oumuamua and all nearby stars with known kinematic data during their past motion. We had checked over 200 thousand stars and found just a handful of candidates. If we limit our investigation to within a 60 pc sphere surrounding the Sun, then the most probable candidate for the ’Oumuamua parent stellar habitat is the star UCAC4 535-065571. However GJ 876 is also a favourable candidate. However, the origin of ’Oumuamua from a much more distant source is still an open question. Additionally, we found that the quality of the original orbit of ’Oumuamua is accurate enough for such a study and that none of the checked stars had perturbed its motion significantly. All numerical results of this research are available in the appendix.

Commission 26: Double and Multiple Stars (Etoiles Doubles Et Multiples)

Transactions of the International Astronomical Union ◽

10.1017/s0251107x00002856 ◽

2000 ◽

Vol 24 (1) ◽

pp. 186-189

Author(s):

H. Zinnecker ◽

C. Scarfe ◽

C. Allen ◽

T. Armstrong ◽

W. Hartkopf ◽

...

Keyword(s):

San Francisco ◽

Large Scale ◽

Binary Systems ◽

Extrasolar Planets ◽

Binary Star ◽

The Sun ◽

Double And Multiple Stars ◽

Nearby Stars ◽

Solar Type ◽

Low Mass

This triennial report (1996-1999) reviews the subject from a somewhat personal angle, mostly related to binary star formation and young binary star populations – a subject whose time had come in the early 1990s and is now in full swing.Many astronomers have searched for binary systems among main-sequence stars, and two large-scale surveys published in 1991 and 1992 have already become classics. Well before they became famous for finding extrasolar planets (see below), observing teams led by Michel Mayor (Geneva Observatory) and Geoffrey Marcy (San Francisco State Univ., now Univ. of Calif, at Berkeley) spent many years searching for low-mass stellar companions of nearby stars. The late Antoine Duquennoy and Mayor surveyed all solar-type dwarfs (spectral types F7 through G9) within 20 pc of the Sun, while Debra Fischer and Marcy studied stars with somewhat lower mass (M dwarfs) slightly nearer to the Sun.

Trigonometric Parallaxes and Their Calibration

Symposium - International Astronomical Union ◽

10.1017/s0074180900078761 ◽

1985 ◽

Vol 111 ◽

pp. 31-51

Author(s):

Arthur R. Upgren

Keyword(s):

Solar System ◽

Linear Dimension ◽

Angular Dimension ◽

Single Star ◽

Distance Methods ◽

Trigonometric Parallaxes ◽

Nearby Stars ◽

System Errors ◽

The Universe ◽

Better Than

The precision obtained in equating a very precise linear dimension to a very small and imprecise angular dimension sets a limit on the precision of the distance scale of the Universe. Within the Solar System, errors in distances are of the order of one part in one hundred million, but beyond its limits only a single star, Barnard's star, has a distance known to better than one part in one hundred, and distances known to one part in twenty from parallaxes are limited to only a few hundred nearby stars. Yet most other distance methods and results must ultimately be calibrated against distances to nearby stars derived from the heliocentric parallax method and its observations and uncertainties.

Approaches of stars to the Sun

10.1017/s0252921100031651 ◽

1999 ◽

Vol 173 ◽

pp. 345-352 ◽

Cited By ~ 2

Author(s):

P.A. Dybczyński ◽

P. Kankiewicz

Keyword(s):

Minimum Distance ◽

Galactic Disk ◽

Equations Of Motion ◽

Oort Cloud ◽

The Sun ◽

The Past ◽

Straight Line ◽

The Galaxy ◽

Hipparcos Catalogue ◽

AbstractClose approaches of stars to the Solar System perturb comets from the Oort cloud so that they pass into the planetary system − the gravitational impulse changes the distribution of observable comets. This paper presents the results of calculations of the motion of stars in the solar neighbourhood in the past and future. The main results for each star are: the time of the encounter and the minimum distance between the Sun and the star. They are calculated using three different methods: a straight line motion model, a model with a Sun − star Keplerian interaction, and the numerical integration of the equations of motion with galactic perturbations included. In the last case, two models of the Galactic potential are used: a simplified potential of the Galactic disk and the more complex potential of the Galaxy by Dauphole and Colin. Coordinates and velocities of nearby stars are taken from several different catalogues: the Gliese catalogue, the Hipparcos catalogue, and the Barbier-Brossat catalogue of Radial Velocities.