The elemental composition of the Sun

Scott, Pat; Asplund, Martin; Grevesse, N.; Bergemann, M.; Sauval, A. J.

doi:10.1051/0004-6361/201424110

Cited by 258 publications

(223 citation statements)

References 185 publications

(320 reference statements)

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“…If we restrict our average to the data of Hinode, VTT, and SST, which we think are of higher quality, we obtain: A (O) = 8.725 ± 0.012 and A (Ni) = 6.122 ± 0.034, the uncertainty being the observed-to-observed scatter. This latter value for the Ni abundance is in agreement with the value of A(Ni) = 6.17 ± 0.02 from Scott et al (2009) and in reasonable agreement with A(Ni) = 6.20 ± 0.04 from Scott et al (2015), who used an improved 3D solar model atmosphere with respect to Scott et al (2009). Our nickel abundance is almost within one σ of the Scott et al (2009) and of the Scott et al (2015) results.…”

Section: Line Profile Fittingsupporting

confidence: 90%

“…However, we believe it is unlikely that a re-analysis of the solar Ni abundance will result in a large downward revision. The recent result of Scott et al (2015), who find A(Ni) = 6.20 ± 0.04, corroborates this notion. For the meteoritic nickel abundance, Lodders (2003) recommends A(Ni) = 6.22±0.03, thus a nickel abundance as low as around 6.00 (THEMIS) would be in stark disagreement with the meteoritic nickel abundance.…”

Section: The Blending Nickel Linesupporting

confidence: 60%

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The photospheric solar oxygen project

Caffau

Ludwig

Steffen

et al. 2015

A&A

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Context. The solar photospheric abundance of oxygen is still a matter of debate. For about ten years some determinations have favoured a low oxygen abundance which is at variance with the value inferred by helioseismology. Among the oxygen abundance indicators, the forbidden line at 630 nm has often been considered the most reliable even though it is blended with a Ni i line. In Papers I and II of this series we reported a discrepancy in the oxygen abundance derived from the 630 nm and the subordinate [O I] line at 636 nm in dwarf stars, including the Sun. Aims. Here we analyse several, in part new, solar observations of the centre-to-limb variation of the spectral region including the blend at 630 nm in order to separate the individual contributions of oxygen and nickel. Methods. We analyse intensity spectra observed at different limb angles in comparison with line formation computations performed on a CO5BOLD 3D hydrodynamical simulation of the solar atmosphere. Results. The oxygen abundances obtained from the forbidden line at different limb angles are inconsistent if the commonly adopted nickel abundance of 6.25 is assumed in our local thermodynamic equilibrium computations. With a slightly lower nickel abundance, A(Ni) ≈ 6.1, we obtain consistent fits indicating an oxygen abundance of A(O) = 8.73 ± 0.05. At this value the discrepancy with the subordinate oxygen line remains. Conclusions. The derived value of the oxygen abundance supports the notion of a rather low oxygen abundance in the solar photosphere. However, it is disconcerting that the forbidden oxygen lines at 630 and 636 nm give noticeably different results, and that the nickel abundance derived here from the 630 nm blend is lower than expected from other nickel lines.

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Section: Line Profile Fittingsupporting

confidence: 90%

Section: The Blending Nickel Linesupporting

confidence: 60%

The photospheric solar oxygen project

Caffau

Ludwig

Steffen

et al. 2015

A&A

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“…For a Solar metallicity (ǫFe = 7.47 for the Sun or mFe/mH ≈ 0.0017; Scott et al 2015) we therefore see that the added iron from the planet increases the envelope metallicity too little to be observed.…”

Section: Destroying Planets and Polluting Giant Starsmentioning

confidence: 71%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

126

100

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We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zeroage main sequence mass of 3.5 M ⊙ . Dynamic in-spiral timescales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars' envelopes are somewhat puffed up. Based on relatively long timescales and even considering the fact that further inspiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star-planet interaction may be unable to lead to large scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.

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“…The Nieva & Przybilla (2012) data also provide the abundances of the main coolants: H, He, C, N, O, Ne, Mg, Si, and Fe. For the light elements, we use the Lodders et al (2009) abundances, while for all other elements the abundances are based upon Scott et al (2015aScott et al ( , 2015b and Grevesse et al (2015). Thus, in the LGC scale, the "local region" reference abundance has + = 12 log O H 8.77 ( ) , as opposed to the Grevesse et al (2010) solar value of + = 12 log O H 8.69 ( ) .…”

Section: Description Of Shock Gridmentioning

confidence: 99%

Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

Dopita

Seitenzahl

Sutherland

et al. 2016

ApJ

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We present the results of a complete integral-field survey of the bright supernova remnant (SNR) N49 in the Large Magellanic Cloud, obtained with the WiFeS instrument mounted on the ANU 2.3 m telescope at Siding Spring Observatory. From theoretical shock modeling with the new MAPPINGS 5.1 code, we have, for the first time, subjected the optical Fe emission line spectrum of an SNR to a detailed abundance and dynamical analysis covering eight separate stages of ionization. This allows us to derive the dust depletion factors as a function of ionization stage. We have shown that there is substantial (30%-90%) destruction of Fe-bearing dust grains in these fast shocks (v s ∼ 250 km s −1 ), and we have confirmed that the dominant dust destruction occurs through the nonthermal sputtering and grain-grain collision mechanisms developed in a number of theoretical works.

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The elemental composition of the Sun

Cited by 258 publications

References 185 publications

The photospheric solar oxygen project

The photospheric solar oxygen project

Hydrodynamic simulations of the interaction between giant stars and planets

Forbidden Iron Lines and Dust Destruction in Supernova Remnant Shocks: The Case of N49 in the Large Magellanic Cloud

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