The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

Villante, F. L.; Serenelli, Aldo; Delahaye, F.; Pinsonneault, Marc H.

doi:10.1088/0004-637x/787/1/13

Cited by 99 publications

(161 citation statements)

References 57 publications

(76 reference statements)

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“…This rather high oxygen abundance was supported by the work of Ayres et al (2013), who used a CO5BOLD model atmosphere to analyze molecular CO lines (assuming n(C)/n(O) = 0.5) and derived A(O) = 8.78 ± 0.02 dex. Villante et al (2014) has shown that the chemical composition presented by Caffau et al (2011), which includes a "high" A(O), is in much better agreement with the overall metal abundance inferred from helioseismology and solar neutrino data.…”

Section: Introductionmentioning

confidence: 68%

The photospheric solar oxygen project

Steffen

Prakapavičius

Caffau

et al. 2015

A&A

109

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Context. The solar photospheric oxygen abundance is still widely debated. Adopting the solar chemical composition based on the "low" oxygen abundance, as determined with the use of three-dimensional (3D) hydrodynamical model atmospheres, results in a well-known mismatch between theoretical solar models and helioseismic measurements that is so far unresolved. Aims. We carry out an independent redetermination of the solar oxygen abundance by investigating the center-to-limb variation of the O i IR triplet lines at 777 nm in different sets of spectra.Methods. The high-resolution and high signal-to-noise solar center-to-limb spectra are analyzed with the help of detailed synthetic line profiles based on 3D hydrodynamical CO5BOLD model atmospheres and 3D non-LTE line formation calculations with NLTE3D. The idea is to exploit the information contained in the observations at different limb angles to simultaneously derive the oxygen abundance, A(O), and the scaling factor S H that describes the cross-sections for inelastic collisions with neutral hydrogen relative to the classical Drawin formula. Using the same codes and methods, we compare our 3D results with those obtained from the semiempirical Holweger-Müller model atmosphere as well as from different one-dimensional (1D) reference models. Results. With the CO5BOLD 3D solar model, the best fit of the center-to-limb variation of the triplet lines is obtained when the collisions by neutral hydrogen atoms are assumed to be efficient, i.e., when the scaling factor S H is between 1.2 and 1.8, depending on the choice of the observed spectrum and the triplet component used in the analysis. The line profile fits achieved with standard 1D model atmospheres (with fixed microturbulence, independent of disk position μ) are clearly of inferior quality compared to the 3D case, and give the best match to the observations when ignoring collisions with neutral hydrogen (S H = 0). The results derived with the Holweger-Müller model are intermediate between 3D and standard 1D. Conclusions. The analysis of various observations of the triplet lines with different methods yields oxygen abundance values (on a logarithmic scale where A(H) = 12) that fall in the range 8.74 < A(O) < 8.78, and our best estimate of the 3D non-LTE solar oxygen abundance is A(O) = 8.76 ± 0.02. All 1D non-LTE models give much lower oxygen abundances, by up to −0.15 dex. This is mainly a consequence of the assumption of a μ-independent microturbulence. An independent determination of the relevant collisional cross-sections is essential to substantially improve the accuracy of the oxygen abundance derived from the O i IR triplet.

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Section: Introductionmentioning

confidence: 68%

The photospheric solar oxygen project

Steffen

Prakapavičius

Caffau

et al. 2015

A&A

109

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“…It is well known that with the current available input physics and the Asplund et al (2009) abundances a 1 M star at the current age of the Solar System does not give a structure consistent with helioseismic measurements (see e.g. Villante et al 2014, and references therein). Specifically, one cannot produce a model that fits the current radius and luminosity of the Sun which also has the correct depth of the convective envelope.…”

Section: The Effects Of the Choice Of Solar Calibrationmentioning

confidence: 97%

Confronting uncertainties in stellar physics

Stancliffe

Fossati

Passy

et al. 2016

A&A

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We assess the systematic uncertainties in stellar evolutionary calculations for low-to intermediate-mass, main-sequence stars. We compare published stellar tracks from several different evolution codes with our own tracks computed using the stellar codes stars and mesa. In particular, we focus on tracks of 1 and 3 M at solar metallicity. We find that the spread in the available 1 M tracks (computed before the recent solar composition revision) can be covered by tracks between 0.97−1.01 M computed with the stars code. We assess some possible causes of the origin of this uncertainty, including how the choice of input physics and the solar constraints used to perform the solar calibration affect the tracks. We find that for a 1 M track, uncertainties of around 10% in the initial hydrogen abundance and initial metallicity produce around a 2% error in mass. For the 3 M tracks, there is very little difference between the tracks from the various different stellar codes. The main difference comes in the extent of the main sequence, which we believe results from the different choices of the implementation of convective overshooting in the core. Uncertainties in the initial abundances lead to a 1−2% error in the mass determination. These uncertainties cover only part of the total error budget, which should also include uncertainties in the input physics (e.g., reaction rates, opacities, convective models) and any missing physics (e.g., radiative levitation, rotation, magnetic fields). Uncertainties in stellar surface properties such as luminosity and effective temperature will further reduce the accuracy of any potential mass determinations.

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“…For solar metallicity we adopt Z ⊙ = 0.02 (Villante et al 2014). This is the result of the fact that stars at high metallicity are subject to intensive stellar wind mass loss (Vink 2011) and they do not form helium cores above 45 M ⊙ (see Fig.…”

Section: Mass Of Single Bhs and Bh-bh Mergersmentioning

confidence: 99%

The effect of pair-instability mass loss on black-hole mergers

Belczyński

Heger

Gładysz

et al. 2016

A&A

429

426

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Context. Mergers of two stellar origin black holes are a prime source of gravitational waves and are under intensive investigation. One crucial ingredient in their modeling has been neglected: pair-instability pulsation supernovae with associated severe mass loss may suppress the formation of massive black holes, decreasing black hole merger rates for the highest black hole masses. Aims. We demonstrate the effects of pair-instability pulsation supernovae on merger rate and mass using populations of double black hole binaries formed through the isolated binary classical evolution channel. Methods. The mass loss from pair-instability pulsation supernova is estimated based on existing hydrodynamical calculations. This mass loss is incorporated into the StarTrack population synthesis code. StarTrack is used to generate double black hole populations with and without pair-instability pulsation supernova mass loss. Results. The mass loss associated with pair-instability pulsation supernovae limits the Population I/II stellar-origin black hole mass to 50 M ⊙ , in tension with earlier predictions that the maximum black hole mass could be as high as 100 M ⊙ . In our model, neutron stars form with mass 1-2 M ⊙ , then we encounter the first mass gap at 2-5 M ⊙ with an absence of compact objects due to rapid supernova explosions, followed by the formation of black holes with mass 5-50 M ⊙ , with a second mass gap at 50-135 M ⊙ created by pairinstability pulsation supernovae and by pair-instability supernovae. Finally, black holes having masses above 135 M ⊙ may potentially form to arbitrarily high mass limited only by the extent of the initial mass function and the strength of stellar winds. Suppression of double black hole merger rates by pair-instability pulsation supernovae is negligible for our evolutionary channel. Our standard evolutionary model with the inclusion of pair-instability pulsation supernovae and pair-instability supernovae is fully consistent with the LIGO observations of black hole mergers: GW150914, GW151226, and LVT151012. The LIGO results are inconsistent with high ( 400 km s −1 ) BH natal kicks. We predict the detection of several, and up to as many as ∼ 60, BH-BH mergers with a total mass of 10-150 M ⊙ (most likely range: 20-80 M ⊙ ) in the forthcoming ∼ 60 effective days of the LIGO O2 observations, assuming the detectors reach the optimistic target O2 sensitivity. Conclusions.

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The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

Cited by 99 publications

References 57 publications

The photospheric solar oxygen project

The photospheric solar oxygen project

Confronting uncertainties in stellar physics

The effect of pair-instability mass loss on black-hole mergers

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