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Article overview
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Searching for Solar Siblings in APOGEE and $Gaia$ DR2 with N-body Simulations | | Jeremy J. Webb
; Natalie Price-Jones
; Jo Bovy
; Simon Portegies Zwart
; Jason A. S. Hunt
; J. Ted Mackereth
; Henry W. Leung
; | | Date: |
3 Oct 2019 | | Abstract: | We make use of APOGEE and $Gaia$ data to identify stars that are consistent
with being born in the same star cluster as the Sun. We limit our analysis to
stars that match solar abundances within their uncertainties, as they could
have formed from the same Giant Molecular Cloud (GMC) as the Sun. We constrain
the range of orbital actions that solar siblings can have with a suite of
simulations of solar birth clusters evolved in static and time-dependent tidal
fields. In the static tidal field, which contains a bulge, disk, and halo,
simulated solar siblings all have $5.8 < J_R < 7.4$ km $
m s^{-1}$ kpc, $1848
< L_z < 1868$ km $
m s^{-1}$ kpc, and $0.27 < J_z < 0.49$ km $
m s^{-1}$ kpc.
Given the actions of stars in APOGEE and $Gaia$, we find one star (Solar
Sibling 1) that meets these criteria and shares chemistry with the Sun.
Incorporating the effects of a bar and spiral arms increases the range of
possible $J_R$ and $L_z$ for cluster escapers, extending the candidate list to
203 stars. Adding GMCs to the potential can eject solar siblings out of the
plane of the disk and increase their $J_z$, resulting in a final candidate list
of 550 stars. The entire suite of simulations indicate that solar siblings
should have $J_R < 116$ km $
m s^{-1}$ kpc, $353 < L_z < 2110$ km $
m s^{-1}$
kpc, and $J_z < 0.8$ km $
m s^{-1}$ kpc. Given these criteria, it is most
likely that the Sun’s birth cluster has reached dissolution and is not the
commonly cited open cluster M67. | | Source: | arXiv, 1910.1646 | | Services: | Forum | Review | PDF | Favorites | |
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