Results 221 to 230 of about 4,122 (255)

Preliminary orbital elements of six visual binary stars [PDF]

Astronomische Nachrichten, 2008
AbstractPreliminary new orbital elements were computed for the visual binary stars A 1 ‐ ADS 1345, A 2629 ‐ ADS 3610, BU 560 ‐ ADS 4371, STF 3115 ‐ ADS 4376, STF 1426 AB ‐ ADS 7730 and STF 2437 ‐ ADS 11956. Using Straizys and Kuriliene's data, we derived new formulae for computing dynamical parallaxes for luminosity classes IV and V.
L Pansecchi, M Scardia, J -L Prieur
exaly   +3 more sources

Orbital elements of six visual binary stars [PDF]

Astronomische Nachrichten, 2001
Revised orbital elements of the visual binary stars STT 515, BU 4 AB, STF 183 AB, A 207, STT 43 and A 2413 are given. Dynamical parallaxes and total masses of the systems have been calculated.
L Koechlin, J -L Prieur
exaly   +3 more sources

Some of the next articles are maybe not open access.

Related searches:

Visual binary star orbits in universal variables

Astrophysics and Space Science, 1995
zbMATH Open Web Interface contents unavailable due to conflicting licenses.
Antonio Elipe
exaly   +3 more sources

Orbits of 11 visual binary stars

New Astronomy, 2008
Abstract In this paper, the orbital elements for 11 visual binaries are given and calculated. Eight already possess orbits, but here they are recalculated. The reason is that recent measurements show higher residuals with respect to the corresponding ephemerides calculated by using the orbital elements given in the Sixth Catalog of Orbits of Visual ...
Z. Cvetković, B. Novaković, N. Todorović   +2 more
openaire   +1 more source

Orbital elements of five close visual binary stars [PDF]

Astronomische Nachrichten, 2000
Revised orbital elements of the visual binary stars STT 2, STT 4, BU 1015, STT 6 and BU 395 are given. Dynamical parallaxes and total masses of the systems have been calculated.
Jean-Louis Prieur, L Koechlin
exaly   +3 more sources

Statistics of Young Visual Binary Stars: Implications for (Binary) Star Formation

1997
It is well known that most main sequence stars are members of binary and multiple systems (e.g. Abt 1983, Herczeg 1984). Recent survey work in nearby star forming regions (such as Taurus and Ophiuchus) has demonstrated that this is also the case for young low-mass pre-main-sequence stars (Zinnecker, Brandner, Reipurth 1992; Reipurth and Zinnecker 1993,
Hans Zinnecker, Wolfgang Brandner
openaire   +1 more source

Orbit of the visual binary star 61 Cyg

Astronomische Nachrichten
AbstractWe present the orbit and the mass estimates for the components of the visual binary star 61 Cyg obtained with the positional observations, including the high‐precision Gaia data, and the measurements of differences in the radial velocities and the radial accelerations of the components.
Arina Apetyan, I S Izmailov
exaly   +2 more sources

Star formation history: Modeling of visual binaries

New Astronomy, 2018
Abstract Most stars form in binary or multiple systems. Their evolution is defined by masses of components, orbital separation and eccentricity. In order to understand star formation and evolutionary processes, it is vital to find distributions of physical parameters of binaries.
A Yu Sytov, O Yu Malkov
exaly   +2 more sources

Precise radial velocity measurements of visual binary stars

Astrophysics and Space Science, 1988
The radial Velocity of a selected number of components of visual binaries have been measured. Attention is paid to systems suspected to have third (invisible) companions. A second aim of observation are selected couples from the “Catalog of radial velocities of binary stars” by Dommanget, for which the decision between different orbits is possible by ...
S. Weichinger, K. D. Rakos
openaire   +1 more source

Evidence for mass loss in visual binary stars

Astrophysics and Space Science, 1988
The present status of the observational evidence about mass loss in visual binary and multiple systems is reviewed. Particular emphasis is placed on the importance of mass-loss rates measures in these stars, as a systematic study would provide useful constraints in two fields. First, as mass-outflows processes are not modified by the interaction of the
openaire   +1 more source