Tidal tails of open star clusters as probes to early gas expulsion: II. Predictions for Gaia

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10423264" target="_blank" >RIV/00216208:11320/20:10423264 - isvavai.cz</a>

Result on the web

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=4YIHTSHyRC" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=4YIHTSHyRC</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201936572" target="_blank" >10.1051/0004-6361/201936572</a>

Result language

angličtina

Original language name

Tidal tails of open star clusters as probes to early gas expulsion: II. Predictions for Gaia

Original language description

Aims. We study the formation and evolution of the tidal tail released from a young star Pleiades-like cluster, due to expulsion of primordial gas in a realistic gravitational field of the Galaxy. The tidal tails (as well as clusters) are integrated from their embedded phase for 300 Myr. We vary star formation efficiencies (SFEs) from 33% to 100% and the timescales of gas expulsion as free parameters, and provide predictions for the morphology and kinematics of the evolved tail for each of the models. The resulting tail properties are intended for comparison with anticipated Gaia observations in order to constrain the poorly understood early conditions during the gas phase and gas expulsion.Methods. The simulations are performed with the code NBODY6 including a realistic external gravitational potential of the Galaxy, and an analytical approximation for the natal gaseous potential.Results. Assuming that the Pleiades formed with rapid gas expulsion and an SFE of approximate to 30%, the current Pleiades are surrounded by a rich tail extending from approximate to 150 to approximate to 350 pc from the cluster and containing 0.7x to 2.7x the number of stars in the present-day cluster. If the Pleiades formed with an SFE close to 100%, then the tail is shorter (less than or similar to 90 pc) and substantially poorer with only approximate to 0.02x the number of present-day cluster stars. If the Pleiades formed with an SFE of approximate to 30%, but the gas expulsion was adiabatic, the tail signatures are indistinguishable from the case of the model with 100% SFE. The mass function of the tail stars is close to that of the canonical mass function for the clusters including primordial gas, but it is slightly depleted of stars more massive than approximate to 1 M-circle dot for the cluster with 100% SFE, a difference that is not likely to be observed. The model takes into account the estimated contamination due to the field stars and the Hyades-Pleiades stream, which constitutes a more limiting factor than the accuracy of the Gaia measurements.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

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Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2020

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

—

Volume of the periodical

640

Issue of the periodical within the volume

srpen

Country of publishing house

FR - FRANCE

Number of pages

24

Pages from-to

A85

UT code for WoS article

000564318500003

EID of the result in the Scopus database

2-s2.0-85090140894