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Résoudre une controverse d’une décennie sur la composition de notre étoile

Les astronomes ont finalement résolu le conflit entre la structure interne du Soleil déterminée à partir des oscillations solaires et la structure dérivée de la théorie fondamentale de l’évolution stellaire.

De nouveaux calculs du spectre solaire résolvent une controverse de dix ans sur la composition de notre étoile.

Bien que notre soleil soit bien plus proche que n’importe quelle autre étoile de l’univers, il a toujours ses mystères. Après tout, il se trouve encore à 93 millions de miles (150 millions de kilomètres) de la Terre et nous n’avons qu’une perspective étroite. De plus, sa surface est brûlante, son atmosphère encore plus chaude et ses particules projetées constamment à environ 1 million de miles par heure. Il n’est pas étonnant que nous fassions encore de nouvelles découvertes.

En fait, les astronomes viennent de résoudre la crise d’abondance solaire qui dure depuis une décennie : le conflit entre la structure interne du Soleil telle que déterminée à partir des oscillations solaires (héliosismologie) et la structure dérivée de la théorie fondamentale de l’évolution stellaire, qui à son tour repose sur des mesures de la composition chimique du Soleil actuel. De nouveaux calculs de la physique de l’atmosphère du Soleil donnent des résultats mis à jour pour les abondances de différents éléments chimiques, qui résolvent le conflit. Notamment, le Soleil contient plus d’oxygène, de silicium et de néon qu’on ne le pensait auparavant. Les méthodes employées promettent également des estimations beaucoup plus précises des compositions chimiques des étoiles en général.

Que faites-vous lorsqu’une méthode éprouvée de détermination de la composition chimique du Soleil semble être en contradiction avec une technique innovante et précise de cartographie de la structure interne du Soleil ? Telle était la situation à laquelle étaient confrontés les astronomes étudiant le Soleil – jusqu’à ce que de nouveaux calculs qui ont maintenant été publiés par Ekaterina Magg, Maria Bergemann et leurs collègues, et qui résolvent l’apparente contradiction.

NARVAL Soleil Spectre

Spectre du Soleil, pris avec le spectrographe très haute résolution NARVAL installé au Télescope Bernard Lyot, Observatoire Midi-Pyrénées. De tels spectres, en particulier les propriétés des raies d’absorption sombres bien visibles sur cette image, permettent aux astronomes de déduire la température et la composition chimique d’une étoile. Crédit : © M. Bergemann / MPIA / [email protected]

La méthode éprouvée en question est l’analyse spectrale. Afin de déterminer la composition chimique de notre Soleil, ou de toute autre étoile, les astronomes se tournent régulièrement vers les spectres : la décomposition en arc-en-ciel de la lumière en ses différentes longueurs d’onde. Les spectres stellaires contiennent des lignes sombres nettes et nettes, remarquées pour la première fois par William Wollaston en 1802, redécouvertes par Joseph von Fraunhofer en 1814, et identifiées comme des signes révélateurs indiquant la présence d’éléments chimiques spécifiques par Gustav Kirchhoff et Robert Bunsen dans les années 1860.

Faits sur le soleil

  • Type : étoile de séquence principale de type G (G2V)
  • Type informel : Nain jaune
  • Âge : ~4,5 milliards d’années
  • Volume : 1,3 million de fois celui de la Terre
  • Température centrale : 27 millions de degrés[{” attribute=””>Fahrenheit (15 million degrees Celsius)
  • Distance From Earth: 93 million miles (150 million kilometers)
  • Distance From Galactic Center: 26,000 light years

Pioneering work by the Indian astrophysicist Meghnad Saha in 1920 related the strength of those “absorption lines” to stellar temperature and chemical composition, providing the basis for our physical models of stars. Cecilia Payne-Gaposchkin’s realization that stars like our Sun consist mainly of hydrogen and helium, with no more than trace amounts of heavier chemical elements, is based on that work.

The underlying calculations relating spectral features to the chemical composition and physics of the stellar plasma have been of crucial importance to astrophysics ever since. They have been the foundation of a century-long progress in our understanding of the chemical evolution of the universe as well as of the physical structure and evolution of stars and exoplanets. That is why it came as something of a shock when, as new observational data became available and provided an insight into the inner workings of our Sun, the different pieces of the puzzle apparently did not fit together.

The modern standard model of solar evolution is calibrated using a famous (in solar physics circles) set of measurements of the solar atmosphere’s chemical composition, published in 2009. But in a number of important details, a reconstruction of our favorite star’s inner structure based on that standard model contradicts another set of measurements: helioseismic data, that is, measurements that track very precisely the minute oscillations of the Sun as a whole – the way that the Sun rhythmically expands and contracts in characteristic patterns, on time scales between seconds and hours.

Just like seismic waves provide geologists with crucial information about the Earth’s interior, or like the sound of a bell encodes information about its shape and material properties, helioseismology provides information about the interior of the Sun.

Highly accurate helioseismic measurements gave results about the Sun’s interior structure that were at odds with the solar standard models. According to helioseismology, the so-called convective region within our Sun where matter rises and sinks down again, like water in a boiling pot, was considerably larger than the standard model predicted. The speed of sound waves near the bottom of that region also deviated from the standard model’s predictions, as did the overall amount of helium in the Sun. To top it off, certain measurements of solar neutrinos – fleeting elementary particles, hard to detect, reaching us directly from the Sun’s core regions – were slightly off compared to experimental data, as well.

Astronomers had what they soon came to call a “solar abundances crisis,” and in search of a way out, some proposals ranged from the unusual to the downright exotic. Did the Sun maybe accrete some metal-poor gas during its planet-forming phase? Is energy being transported by the notoriously non-interacting dark matter particles?

The newly published study by Ekaterina Magg, Maria Bergemann and colleagues has managed to resolve that crisis, by revisiting the models on which the spectral estimates of the Sun’s chemical composition are based. Early studies of how the spectra of stars are produced had relied on something known as local thermal equilibrium. They had assumed that locally, energy in each region of a star’s atmosphere has time to spread out and reach a kind of equilibrium. This would make it possible to assign to each such region a temperature, which leads to a considerable simplification in the calculations.

But as early as the 1950s, astronomers had realized that this picture was oversimplified. Since then, more and more studies incorporated so-called Non-LTE calculations, dropping the assumption of local equilibrium. The Non-LTE calculations include a detailed description of how energy is exchanged within the system – atoms getting excited by photons, or colliding, photons getting emitted, absorbed or scattered. In stellar atmospheres, where densities are far too low to allow the system to reach thermal equilibrium, that kind of attention to detail pays off. There, Non-LTE calculations yield results that are markedly different from their local-equilibrium counterparts.

Maria Bergemann’s group at the Max Planck Institute for Astronomy is one of the world leaders when it comes to applying Non-LTE calculations to stellar atmospheres. As part of the work on her PhD in that group, Ekaterina Magg set out to calculate in more detail the interaction of radiation matter in the solar photosphere. The photosphere is the outer layer where most of the Sun’s light originates, and also where the absorption lines are imprinted on the solar spectrum.

In this study they tracked all chemical elements that are relevant to the current models of how stars evolved over time, and applied multiple independent methods to describe the interactions between the Sun’s atoms and its radiation field in order to make sure their results were consistent. For describing the convective regions of our Sun, they used existing simulations that take into account both the motion of the plasma and the physics of radiation (“STAGGER” and “CO5BOLD”). For the comparison with spectral measurements, they chose the data set with the highest available quality: the solar spectrum published by the Institute for Astro- and Geophysics, University of Göttingen. “We also extensively focused on the analysis of statistical and systematic effects that could limit the accuracy of out results,” notes Magg.

The new calculations showed that the relationship between the abundances of these crucial chemical elements and the strength of the corresponding spectral lines was significantly different from what previous authors had claimed. Consequently, the chemical abundances that follow from the observed solar spectrum are somewhat different than stated in previous analysis.

“We found, that according to our analysis the Sun contains 26% more elements heavier than helium than previous studies had deduced,” explains Magg. In astronomy, such elements heavier than helium are called “metals.” Only on the order of a thousandth of a percent of all atomic nuclei in the Sun are metals; it is this very small number that has now changed by 26% of its previous value. Magg adds: “The value for the oxygen abundance was almost 15% higher than in previous studies.” The new values are, however, in good agreement with the chemical composition of primitive meteorites (“CI chondrites”) that are thought to represent the chemical make-up of the very early solar system.

When those new values are used as the input for current models of solar structure and evolution, the puzzling discrepancy between the results of those models and helioseismic measurements disappears. The in-depth analysis by Magg, Bergemann and their colleagues of how spectral lines are produced, with its reliance on considerably more complete models of the underlying physics, manages to resolve the solar abundance crisis.

Maria Bergemann says: “The new solar models based on our new chemical composition are more realistic than ever before: they produce a model of the Sun that is consistent with all the information we have about the Sun’s present-day structure – sound  waves, neutrinos, luminosity, and the Sun’s radius – without the need for non-standard, exotic physics in the solar interior.”

As an added bonus, the new models are easy to apply to stars other than the Sun. At a time where large-scale surveys like SDSS-V and 4MOST are providing high-quality spectra for an ever greater number of stars, this kind of progress is valuable indeed – putting future analyses of stellar chemistry, with their broader implications for reconstructions of the chemical evolution of our cosmos, on a firmer footing than ever before.

Reference: “Observational constraints on the origin of the elements: IV. Standard composition of the Sun” by Ekaterina Magg, Maria Bergemann, Aldo Serenelli, Manuel Bautista, Bertrand Plez, Ulrike Heiter, Jeffrey M. Gerber, Hans-Günter Ludwig, Sarbani Basu, Jason W. Ferguson, Helena Carvajal Gallego, Sébastien Gamrath, Patrick Palmeri and Pascal Quinet, 20 May 2022, Astronomy & Astrophysics.
DOI: 10.1051/0004-6361/202142971

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