The solar siblings in the Gaia era

Martínez-Barbosa, C. A.; Zwart, Simon Portegies

doi:10.1051/eas/1567021

Cited by 3 publications

(5 citation statements)

References 12 publications

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“…400 and 1 000 M⊙, it is possible for a star similar to the Sun to end on a Sun-like orbit after 4.5 Gyr. The most likely Sun-candidates will be stars coming from clusters that were born at 8 kpc which is in agreement with the dynamically inferred results for the solar birth location in Minchev et al (2013) and Martínez-Barbosa et al (2014). Stars from clusters born at 4 kpc can reach the Solar orbit in 4.5 Gyr but this is much less likely.…”

Section: Radiussupporting

confidence: 86%

Tracking Cluster Debris (TraCD) – I. Dissolution of clusters and searching for the solar cradle

Loyola

Flynn

Hurley

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The capability to reconstruct dissolved stellar systems in dynamical and chemical space is a key factor in improving our understanding of the evolution of the Milky Way. Here we concentrate on the dynamical aspect and given that a significant portion of the stars in the Milky Way have been born in stellar associations or clusters that have lived a few Myr up to several Gyr, we further restrict our attention to the evolution of star clusters. We have carried out our simulations in two steps: (1) we create a simulation of dissolution and mixing processes which yields a close fit to the presentday Milky Way dynamics and (2) we have evolved three sets of stellar clusters with masses of 400, 1 000 and 15 000 M ⊙ to dissolution. The birth location of these sets was 4, 6, 8 and 10 kpc for the 400 and 1 000 M ⊙ clusters and 4, 6, 8, 10 and 12 kpc for the 15 000 M ⊙ . We have focused our efforts on studying the state of the escapers from these clusters after 4.5 Gyr of evolution with particular attention to stars that reach the Solar annulus, i.e. 7.5 R gc 8.5 kpc. We give results for Solar twins and siblings over a wide range of radii and cluster masses for two dissolution mechanisms. From kinematics alone, we conclude that the Sun was ∼50 per cent more likely to have been born near its current Galactocentric radius, rather than have migrated (radially) ∼ 2 kpc since birth. We conclude our analysis by calculating magnitudes and colours of our single stars for comparison with the samples that the Gaia, Gaia-ESO and GALAH-AAO surveys will obtain. In terms of reconstructing dissolved star clusters we find that on short time-scales we cannot rely on kinematic evolution alone and thus it will be necessary to extend our study to include information on chemical space.

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Section: Radiussupporting

confidence: 86%

Tracking Cluster Debris (TraCD) – I. Dissolution of clusters and searching for the solar cradle

Loyola

Flynn

Hurley

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…The Milky Way was modeled as an analytical potential consisting of an axisymmetric component together with a central bar and spiral arms. We adopted the same Galactic model as Martínez-Barbosa et al (2014) where the axisymmetric part of the Galaxy is modelled by using the potential of Allen & Santillan (1991) which consist of a bulge, disk and a dark matter halo.…”

Section: Radial Velocity Of the Sun's Siblingsmentioning

confidence: 99%

“…The motion of the stars due to their selfgravity was computed by the HUAYNO code (Pelupessy et al 2012). The motion of the stars under the external tidal field of the Milky Way was computed by a 6th-order rotating BRIDGE (Martínez- Barbosa et al 2014). Additionally, we used the SeBa code(Portegies Zwart & Verbunt 1996;Toonen et al 2012) to model the stellar evolution of the stars.…”

Section: Radial Velocity Of the Sun's Siblingsmentioning

confidence: 99%

“…The initial phase-space coordinates of the Sun's birth cluster center of mass (x cm , y cm , v x cm , v y cm ) were obtained by evolving the orbit of the Sun backwards in time taking into account the uncertainty in the Sun's current position and velocity, as is shown in Martínez-Barbosa et al (2014). The orbit integration backwards in time gives a distribution of all the possible positions and velocities of the Sun at its birth, we therefore choose one position and velocity from this distribution to be the initial phase-space coordinates of the Sun's birth cluster center of mass.…”

Section: Radial Velocity Of the Sun's Siblingsmentioning

confidence: 99%

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Quest for the lost siblings of the Sun

Liu¹,

Ruchti²,

Feltzing³

et al. 2015

A&A

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Aims. The aim of this paper is to find lost siblings of the Sun by analyzing high resolution spectra. Finding solar siblings will enable us to constrain the parameters of the parental cluster and the birth place of the Sun in the Galaxy. Methods. The solar siblings can be identified by accurate measurements of metallicity, stellar age and elemental abundances for solar neighbourhood stars. The solar siblings candidates were kinematically selected based on their proper motions, parallaxes and colours. Stellar parameters were determined through a purely spectroscopic approach and partly physical method, respectively. Comparing synthetic with observed spectra, elemental abundances were computed based on the stellar parameters obtained using a partly physical method. A chemical tagging technique was used to identify the solar siblings.Results. We present stellar parameters, stellar ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Ti, Cr, Fe, and Ni for 32 solar sibling candidates. Our abundances analysis shows that four stars are chemically homogenous together with the Sun. Technique of chemical tagging gives us a high probability that they might be from the same open cluster. Only one candidate -HIP 40317 -which has solar metallicity and age could be a solar sibling. We performed simulations of the Sun's birth cluster in analytical Galactic model and found that most of the radial velocities of the solar siblings lie in the range −10 ≤ V r ≤ 10 km s −1 , which is smaller than the radial velocity of HIP 40317 (V r = 34.2 km s −1 ), under different Galactic parameters and different initial conditions of the Sun's birth cluster. The sibling status for HIP 40317 is not directly supported by our dynamical analysis.

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“…Possibly, the migration happened while the Sun was still a member of its birth cluster. Extensive numerical analysis of the orbit of the Sun in the Galactic potential however indicates that this radial migration in the current Galactic potential would be negligible (Martínez-Barbosa et al, 2014).…”

Section: As a Possible Host Clustermentioning

confidence: 99%

The formation of the solar system

Pfalzner,

Davies,

Gounelle

et al. 2015

Preprint

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The solar system started to form about 4.56 Gyr ago and despite the long intervening time span, there still exist several clues about its formation. The three major sources for this information are meteorites, the present solar system structure and the planetforming systems around young stars. In this introduction we give an overview of the current understanding of the solar system formation from all these different research fields. This includes the question of the lifetime of the solar protoplanetary disc, the different stages of planet formation, their duration, and their relative importance. We consider whether meteorite evidence and observations of protoplanetary discs point in the same direction. This will tell us whether our solar system had a typical formation history or an exceptional one. There are also many indications that the solar system formed as part of a star cluster. Here we examine the types of cluster the Sun could have formed in, especially whether its stellar density was at any stage high enough to influence the properties of today's solar system. The likelihood of identifying siblings of the Sun is discussed. Finally, the possible dynamical evolution of the solar system since its formation and its future are considered.

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The solar siblings in the Gaia era

Cited by 3 publications

References 12 publications

Tracking Cluster Debris (TraCD) – I. Dissolution of clusters and searching for the solar cradle

Tracking Cluster Debris (TraCD) – I. Dissolution of clusters and searching for the solar cradle

Quest for the lost siblings of the Sun

The formation of the solar system

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