Access the full text.
Sign up today, get DeepDyve free for 14 days.
T. Jeřábková, G. Beccari, H. Boffin, M. Petr-Gotzens, C. Manara, P. Moroni, E. Tognelli, S. Degl'innocenti (2019)
When the tale comes true: multiple populations and wide binaries in the Orion Nebula ClusterAstronomy & Astrophysics
(2011)
General Astrophysics, 2nd ed
M. R. Bate (2002)
705Monthly Notices Royal Astron. Soc., 336
G. Torres, D. Latham, S. Quinn (2021)
Long-term Spectroscopic Survey of the Pleiades Cluster: The Binary PopulationThe Astrophysical Journal, 921
M. Bate, I. Bonnell, V. Bromm (2002)
The formation of close binary systems by dynamical interactions and orbital decayMonthly Notices of the Royal Astronomical Society, 336
D. Heggie (1975)
Binary evolution in stellar dynamicsMonthly Notices of the Royal Astronomical Society, 173
(2022)
Astron
V. Danilov (2005)
The motion of halo stars in dynamical numerical models of open clustersAstronomy Reports, 49
H. Dwight, R. Romer (1934)
Tables of Integrals and Other Mathematical Data
J. Caballero, I. Novalbos, T. Tobal, F. Miret (2017)
Wide sigma Orionis binaries resolved by UKIDSSarXiv: Solar and Stellar Astrophysics
(2016)
Gaia Collab.), Astron. and Astrophys
N. Deacon, A. Astronomy, D. Astronomy, T. Austin (2020)
Wide binaries are rare in open clustersMonthly Notices of the Royal Astronomical Society, 496
S. J. Aarseth (1971)
324Astrophys. and Space Sci., 13
L. Pearce, A. Kraus, T. Dupuy, A. Mann, E. Newton, B. Tofflemire, A. Vanderburg (2020)
Orbital Parameter Determination for Wide Stellar Binary Systems in the Age of GaiaThe Astrophysical Journal, 894
General Astrophysics , 2 nd ed . ( Vek 2 , Fryazino , 2011 ) [ in Russian ]
G. Korn (1961)
Mathematical handbook for scientists and engineers
(1948)
Principles of Stellar Dynamics (University of Chicago Press, Chichago
Matthew Furio, M. Meyer, M. Reiter, J. Monnier, A. Kraus, T. Dupuy (2021)
Binary Formation in the Orion Nebula Cluster: Exploring the Substellar LimitThe Astrophysical Journal, 925
Aman Raju, D. Guszejnov, S. Offner (2021)
Stellar Multiplicity in an RMHD Simulation with Stellar FeedbackResearch Notes of the AAS, 5
D. Keenan, K. Innanen, F. House (1973)
Galactic orbits and tidal radii of the Clusters M67, NGC 188 and W CentauriThe Astronomical Journal, 78
L. Hillenbrand, Celia Zhang, R. Riddle, C. Baranec, C. Ziegler, N. Law, J. Stauffer (2017)
Robo-AO Discovery and Basic Characterization of Wide Multiple Star Systems in the Pleiades, Praesepe, and NGC 2264 ClustersThe Astronomical Journal, 155
L. Angeletti (1983)
183Astron. and Astrophys., 121
S. Bludman (1932)
Theoretical PhysicsNature, 129
L. Angeletti (1983)
188Astron. and Astrophys., 121
S. Christian, A. Vanderburg, J. Becker, D. Yahalomi, L. Pearce, G. Zhou, K. Collins, A. Kraus, K. Stassun, Z. Beurs, G. Ricker, R. Vanderspek, D. Latham, J. Winn, S. Seager, J. Jenkins, L. Abe, K. Agabi, P. Amado, D. Baker, K. Barkaoui, Z. Benkhaldoun, P. Benni, J. Berberian, P. Berlind, A. Bieryla, E. Esparza-Borges, Michael Bowen, P. Brown, L. Buchhave, C. Burke, M. Buttu, C. Cadieux, D. Caldwell, D. Charbonneau, Nikita Chazov, Sudhish Chimaladinne, K. Collins, D. Combs, D. Conti, N. Crouzet, J. Leon, Shila Deljookorani, B. Diamond, R. Doyon, D. Dragomir, G. Dransfield, Z. Essack, P. Evans, A. Fukui, T. Gan, G. Esquerdo, M. Gillon, E. Girardin, P. Guerra, T. Guillot, E.K.K. Habich, Andreea Henriksen, Nora Hoch, K. Isogai, E. Jehin, E. Jensen, Marshall Johnson, J. Livingston, J. Kielkopf, Kingsley Kim, K. Kawauchi, V. Krushinsky, Veronica Kunzle, D. Laloum, D. Leger, P. Lewin, F. Mallia, B. Massey, M. Mori, K. McLeod, Djamel M'ekarnia, I. Mireles, N. Mishevskiy, Motohide Tamura, F. Murgas, N. Narita, R. Naves, P. Nelson, H. Osborn, E. Palle, H. Parviainen, P. Plavchan, F. Pozuelos, M. Rabus, H. Relles, Cristina L'opez, S. Quinn, F. Schmider, J. Schlieder, R. Schwarz, Avi Shporer, L. Sibbald, G. Srdoč, Caitlin Stibbards, Hannah Stickler, O. Suárez, C. Stockdale, T. Tan, Y. Terada, A. Triaud, R. Tronsgaard, W. Waalkes, Gavin Wang, N. Watanabe, Marie-Sainte Wenceslas, Geof Wingham, J. Wittrock, C. Ziegler (2022)
A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary CompanionsThe Astronomical Journal, 163
Louette Lutjens (2006)
ResearchNursing Administration Quarterly, 15
W. Jefferys (1976)
On the dynamics and shapes of star clustersThe Astronomical Journal, 81
S. Tremaine (2005)
Galactic Dynamics
The paper estimates the tidal distances \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$|\xi_{c,1,2}|$$\end{document} between the components of wide binary stars (BS) in the Pleiades. We used data on the parameters of the Pleiades cluster and wide BSs in the Pleiades, obtained earlier from the Gaia DR2 data. Two models of a cluster are considered in the form of a gravitating sphere, homogeneous and inhomogeneous in density. Using the integrals of angular momentum and energy of the motion of the centers of mass of the BSs, two elliptical orbits and two open ‘‘rosette-like’’ trajectories of the centers of mass of the BSs relative to the center of mass of the three-body system (the BS components and the cluster) are constructed. For three bodies in a coordinate system nonuniformly rotating relative to their center of mass with the origin at the center of mass of the BS the equations of motion are written. For the model of a homogeneous cluster, a formula is obtained for the value \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$|\xi_{c,1,2}|$$\end{document} for a BS moving along an elliptical orbit. The integrals of angular momentum and energy of motion of the components of the BS and three bodies of the system are obtained. The sizes of the area under the surface of zero velocities (SZV) of the BS components along the axes of the coordinate system with the origin in the center of mass of the BS are estimated. It is shown that in the model of a homogeneous cluster, the sizes of the area under the SZV of the BS components in the pericenters of the considered orbits are smaller than in the apocenters, and on the inner and outer parts of the BS orbits there are restrictions on the size of the area under the SZV of the BS components that differ in number and magnitude. For the model of an inhomogeneous cluster, an equation is obtained for the quantity \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$|\xi_{c,1,2}|$$\end{document} for the BS moving along the ‘‘rosette’’ trajectory relative to the center of mass of three bodies. The quantities \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$|\xi_{c,1,2}|$$\end{document} are numerically determined for the BS at different points of two such trajectories. With the help of the energy integral \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$E_{1,2,3}$$\end{document} of the motion of three bodies, the sizes of the area under the SZV of the BS components are determined. With an increase in the distance of the center of mass of the BS from the center of mass of three bodies in the model of an inhomogeneous cluster, an increase in the size of the area under the SZV of the BS components was noted, as well as the existence of more complex restrictions on the size of this area than in a homogeneous cluster. Mutual distances \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$r_{i,j}$$\end{document} between the components of wide BSs in the Pleiades are between the maximum and minimum values of \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$|\xi_{c,1,2}|$$\end{document} for BSs on ‘‘rosette’’ trajectories. The increase in \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$r_{i,j}$$\end{document} with the distances \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$r_{i}$$\end{document} of the BS components from the center of the cluster is mainly due to the motion of the BS along its trajectories in the Pleiades. Other applications of the integral \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$E_{1,2,3}$$\end{document} for estimating the BS parameters in the Pleiades are also considered.
Astrophysical Bulletin – Springer Journals
Published: Mar 1, 2023
Keywords: stars: kinematics and dynamics; open clusters and associations: individual: Pleiades
Read and print from thousands of top scholarly journals.
Already have an account? Log in
Bookmark this article. You can see your Bookmarks on your DeepDyve Library.
To save an article, log in first, or sign up for a DeepDyve account if you don’t already have one.
Copy and paste the desired citation format or use the link below to download a file formatted for EndNote
Access the full text.
Sign up today, get DeepDyve free for 14 days.
All DeepDyve websites use cookies to improve your online experience. They were placed on your computer when you launched this website. You can change your cookie settings through your browser.