High Precision Abundances of the Old Solar Twin HIP 102152: Insights On Li Depletion from the Oldest Sun

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Date

2013-09

Authors

Monroe, TalaWanda R.
Melendez, Jorge
Ramirez, Ivan
Yong, David
Bergemann, Maria
Asplund, Martin
Bedell, Megan
Maia, Marcelo Tucci
Bean, Jacob
Lind, Karin

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Abstract

We present the first detailed chemical abundance analysis of the old 8.2 Gyr solar twin, HIP 102152. We derive differential abundances of 21 elements relative to the Sun with precisions as high as 0.004 dex (<= 1%), using ultra high-resolution (R = 110,000), high S/N UVES spectra obtained on the 8.2 m Very Large Telescope. Our determined metallicity of HIP 102152 is [Fe/H] = -0.013 +/- 0.004. The atmospheric parameters of the star were determined to be 54 K cooler than the Sun, 0.09 dex lower in surface gravity, and a microturbulence identical to our derived solar value. Elemental abundance ratios examined versus dust condensation temperature reveal a solar abundance pattern for this star, in contrast to most solar twins. The abundance pattern of HIP 102152 appears to be the most similar to solar of any known solar twin. Abundances of the younger, 2.9 Gyr solar twin, 18 Sco, were also determined from UVES spectra to serve as a comparison for HIP 102152. The solar chemical pattern of HIP 102152 makes it a potential candidate to host terrestrial planets, which is reinforced by the lack of giant planets in its terrestrial planet region. The following non-local thermodynamic equilibrium Li abundances were obtained for HIP 102152, 18 Sco, and the Sun: log epsilon (Li) = 0.48 +/- 0.07, 1.62 +/- 0.02, and 1.07 +/- 0.02, respectively. The Li abundance of HIP 102152 is the lowest reported to date for a solar twin, and allows us to consider an emerging, tightly constrained Li-age trend for solar twin stars.

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Monroe, TalaWanda R., Jorge Meléndez, Iván Ramírez, David Yong, Maria Bergemann, Martin Asplund, Megan Bedell et al. "High precision abundances of the old solar twin HIP 102152: insights on Li depletion from the oldest sun." The Astrophysical Journal Letters, Vol. 774, No. 2 (Sep., 2013): L32.