The age of the Sun and the relativistic corrections in the EOS

Bonanno, A.; Schlattl, Helmut; Paternò, L.

doi:10.1051/0004-6361:20020749

Cited by 121 publications

(97 citation statements)

References 17 publications

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“…3 shows the density of stars in the likely r 0 -range, estimated from stars in a narrow age-bin around the solar value (4.6 ± 0.1 Gyr, consistent with, e.g., Bonanno et al 2002;Christensen-Dalsgaard 2009;Houdek & Gough 2011). We find the highest probability to be around 5.6 kpc, followed by 7 kpc.…”

Section: The Birth Place Of the Sunsupporting

confidence: 84%

Chemodynamical evolution of the Milky Way disk

Minchev

Chiappini

Martig

2013

A&A

426

574

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In the first paper of this series, we present a new approach for studying the chemo-dynamical evolution in disk galaxies, which consists of fusing disk chemical evolution models with compatible numerical simulations of galactic disks. This method avoids known star formation and chemical enrichment problems encountered in simulations. Here we focus on the Milky Way, by using a detailed thindisk chemical evolution model (matching local observables, which are weakly affected by radial migration) and a simulation in the cosmological context, with dynamical properties close to those of our Galaxy. We examine in detail the interplay between in situ chemical enrichment and radial migration and their impact on key observables in the solar neighborhood, e.g., the age-metallicityvelocity relation, the metallicity distribution, and gradients in the radial and vertical directions. We show that, due to radial migration from mergers at high redshift and the central bar at later times, a sizable fraction of old metal-poor high-[α/Fe] stars can reach the solar vicinity. This naturally accounts for a number of recent observations related to both the thin and thick disks, despite the fact that we use thin-disk chemistry only. Although significant radial mixing is present, the slope in the age-metallicity relation is only weakly affected, with a scatter compatible with recent observational work. While we find a smooth density distribution in the [O/Fe]-[Fe/H] plane, we can recover the observed discontinuity by selecting particles according to kinematic criteria used in high-resolution samples to define the thin and thick disks. We outline a new method for estimating the birth place of the Sun and predict that the most likely radius lies in the range 4.4 < r < 7.7 kpc (for a current location at r = 8 kpc). A new, unifying model for the Milky Way thick disk is offered, where both mergers and radial migration play a role at different stages of the disk evolution. We show that in the absence of early-on massive mergers the vertical velocity dispersion of the oldest stars is underestimated by a factor of ∼2 compared with observations. We can, therefore, argue that the Milky Way thick disk is unlikely to have been formed through a quiescent disk evolution. An observational test involving both chemical and kinematic information must be devised to ascertain this possibility.

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Section: The Birth Place Of the Sunsupporting

confidence: 84%

Chemodynamical evolution of the Milky Way disk

Minchev

Chiappini

Martig

2013

A&A

426

574

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“…The cyan curve shows the input solar-age metallicity gradient. This is taken to be 4.6 Gyr look-back time, consistent with, e.g., Bonanno et al (2002), ChristensenDalsgaard (2009), andHoudek &Gough (2011). Assuming an error of ±0.06 dex in [Fe/H], we find a possible Sun birth radius in the range 5.0 < r ,birth < 6.8 kpc (where the horizontal green, transparent strip meets the cyan curve).…”

Section: The Birth Place Of the Sunsupporting

confidence: 82%

Constraining the Milky Way assembly history with Galactic Archaeology

Minchev

2016

Astron Nachr

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The aim of Galactic Archaeology is to recover the evolutionary history of the Milky Way from its present day kinematical and chemical state. Because stars move away from their birth sites, the current dynamical information alone is not sufficient for this task. The chemical composition of stellar atmospheres, on the other hand, is largely preserved over the stellar lifetime and, together with accurate ages, can be used to recover the birthplaces of stars currently found at the same Galactic radius. In addition to the availability of large stellar samples with accurate 6D kinematics and chemical abundance measurements, this requires detailed modeling with both dynamical and chemical evolution taken into account. An important first step is to understand the variety of dynamical processes that can take place in the Milky Way, including the perturbative effects of both internal (bar and spiral structure) and external (infalling satellites) agents. We discuss here (1) how to constrain the Galactic bar, spiral structure, and merging satellites by their effect on the local and global disc phase-space, (2) the effect of multiple patterns on the disc dynamics, and (3) the importance of radial migration and merger perturbations for the formation of the Galactic thick disc. Finally, we discuss the construction of Milky Way chemo-dynamical models and relate to observations.

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“…during the lifetime of the Sun (Bonanno et al 2002). We model the Milky Way as a fully analytical potential that contains an axisymmetric component together with a rotating central bar and spiral arms.…”

Section: Galactic Modelmentioning

confidence: 99%

Radial migration of the Sun in the Milky Way: a statistical study

Martínez-Barbosa

Brown

Zwart

2014

Monthly Notices of the Royal Astronomical Society

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The determination of the birth radius of the Sun is important to understand the evolution and consequent disruption of the Sun's birth cluster in the Galaxy. Motivated by this fact, we study the motion of the Sun in the Milky Way during the last 4.6 Gyr in order to find its birth radius. We carried out orbit integrations backward in time using an analytical model of the Galaxy which includes the contribution of spiral arms and a central bar. We took into account the uncertainty in the parameters of the Milky Way potential as well as the uncertainty in the present day position and velocity of the Sun. We find that in general the Sun has not migrated from its birth place to its current position in the Galaxy (R ). However, significant radial migration of the Sun is possible when: 1) The 2 : 1 Outer Lindblad resonance of the bar is separated from the corrotation resonance of spiral arms by a distance ∼ 1 kpc. 2) When these two resonances are at the same Galactocentric position and further than the solar radius. In both cases the migration of the Sun is from outer regions of the Galactic disk to R , placing the Sun's birth radius at around 11 kpc. We find that in general it is unlikely that the Sun has migrated significantly from the inner regions of the Galactic disk to R .

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The age of the Sun and the relativistic corrections in the EOS

Cited by 121 publications

References 17 publications

Chemodynamical evolution of the Milky Way disk

Chemodynamical evolution of the Milky Way disk

Constraining the Milky Way assembly history with Galactic Archaeology

Radial migration of the Sun in the Milky Way: a statistical study

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