The elemental composition of the Sun

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

doi:10.1051/0004-6361/201424111

Cited by 210 publications

(275 citation statements)

References 150 publications

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“…12). Their strengths were well reproduced at a Mo abundance of 1.88 × 10 −4 (mass fraction), which is 35 400 times the solar value (Grevesse et al 2015). Many more weak Mo v and Mo vi lines are visible in the synthetic spectrum but they fade in the noise of the presently available observations.…”

Section: Re 0503-289: Molybdenummentioning

confidence: 77%

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Stellar laboratories

Rauch¹,

Quinet²,

Hoyer³

et al. 2016

A&A

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Context. For the spectral analysis of high-resolution and high signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation. Aims. To identify molybdenum lines in the ultraviolet (UV) spectra of the DA-type white dwarf G191−B2B and the DO-type white dwarf RE 0503−289 and, to determine their photospheric Mo abundances, reliable Mo iv-vii oscillator strengths are used. Methods. We newly calculated Mo iv-vii oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of Mo lines exhibited in high-resolution and high S/N UV observations of RE 0503−289.Results. We identified 12 Mo v and 9 Mo vi lines in the UV spectrum of RE 0503−289 and measured a photospheric Mo abundance of 1.2−3.0 × 10 −4 (mass fraction, 22 500−56 400 times the solar abundance). In addition, from the As v and Sn iv resonance lines, we measured mass fractions of arsenic (0.5−1.3 × 10 −5 , about 300−1200 times solar) and tin (1.3−3.2 × 10 −4 , about 14 300−35 200 times solar). For G191−B2B, upper limits were determined for the abundances of Mo (5.3 × 10 −7 , 100 times solar) and, in addition, for Kr (1.1 × 10 −6 , 10 times solar) and Xe (1.7 × 10 −7 , 10 times solar). The arsenic abundance was determined (2.3−5.9 × 10 −7 , about 21−53 times solar). A new, registered German Astrophysical Virtual Observatory (GAVO) service, TOSS, has been constructed to provide weighted oscillator strengths and transition probabilities. Conclusions. Reliable measurements and calculations of atomic data are a prerequisite for stellar-atmosphere modeling. Observed Mo v-vi line profiles in the UV spectrum of the white dwarf RE 0503−289 were well reproduced with our newly calculated oscillator strengths. For the first time, this allowed the photospheric Mo abundance in a white dwarf to be determined.

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Section: Re 0503-289: Molybdenummentioning

confidence: 77%

“…Since the HST/STIS spectrum of G191−B2B (Sect. 2) is of excellent quality, Mo vi λ 1469.168 Å gives a stringent upper abundance limit of 5.3 × 10 −7 by mass (about 100 times solar, Grevesse et al 2015).…”

Section: G191-b2b: Molybdenummentioning

confidence: 97%

Stellar laboratories

Rauch¹,

Quinet²,

Hoyer³

et al. 2016

A&A

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“…Table 1 lists the solar elemental abundances we obtained using spectra of the Vesta asteroid and the following solar parameters: T eff = 5770 K, log g = 4.44, and ξ = 1.10 km s −1 (see, e.g., Biazzo et al 2012). In the same table, the most recent determinations of solar abundances by Asplund et al (2009), Scott et al (2015a,b), and Grevesse et al (2015) are also given. We stress that the latter values were obtained using 3D+NLTE models.…”

Section: Differential Elemental Abundancesmentioning

confidence: 99%

The GAPS programme with HARPS-N at TNG

Biazzo

Gratton

Desidera

et al. 2015

A&A

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Binary stars hosting exoplanets are a unique laboratory where chemical tagging can be performed to measure the elemental abundances of both stellar components with high accuracy, with the aim to investigate the formation of planets and their subsequent evolution. Here, we present a high-precision differential abundance analysis of the XO-2 wide stellar binary based on high-resolution HARPS-N at TNG spectra. Both components are very similar K-dwarfs and host planets. Since they formed presumably within the same molecular cloud, we expect that they possess the same initial elemental abundances. We investigated whether planets can cause some chemical imprints in the stellar atmospheric abundances. We measure abundances of 25 elements for both stars with a range of condensation temperature T C = 40−1741 K, achieving typical precisions of ∼0.07 dex. The northern component shows abundances in all elements higher by +0.067 ± 0.032 dex on average, with a mean difference of +0.078 dex for elements with T C > 800 K. The significance of the XO-2N abundance difference relative to XO-2S is at the 2σ level for almost all elements. We discuss that this result might be interpreted as the signature of the ingestion of material by XO-2N or depletion in XO-2S that is due to locking of heavy elements by the planetary companions. We estimate a mass of several tens of M ⊕ in heavy elements. The difference in abundances between XO-2N and XO-2S shows a positive correlation with the condensation temperatures of the elements, with a slope of (4.7 ± 0.9) × 10 −5 dex K −1 , which could mean that both components have not formed terrestrial planets, but first experienced the accretion of rocky core interior to the subsequent giant planets.

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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 210 publications

References 150 publications

Stellar laboratories

Stellar laboratories

The GAPS programme with HARPS-N at TNG

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

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