Resolvendo uma controvérsia de uma década sobre a composição de nossa estrela

Os astrônomos finalmente resolveram o conflito entre a estrutura interna do Sol determinada pelas oscilações solares e a estrutura derivada da teoria fundamental da evolução estelar.

Novos cálculos do espectro solar resolvem a controvérsia de uma década sobre a composição de nossa estrela.

Embora nosso sol esteja muito mais próximo do que qualquer outra estrela no universo, ele ainda tem seus mistérios. Afinal, ainda está a 150 milhões de quilômetros da Terra e temos apenas uma perspectiva estreita. Além disso, sua superfície é extremamente quente, sua atmosfera ainda mais quente e constantemente expelindo partículas a cerca de 1 milhão de milhas por hora. Não é à toa que ainda estamos fazendo novas descobertas.

De fato, os astrônomos acabaram de resolver a crise de abundância solar de uma década: o conflito entre a estrutura interna do Sol determinada a partir de oscilações solares (heliosismologia) e a estrutura derivada da teoria fundamental da evolução estelar, que por sua vez se baseia em medições da composição química do Sol atual. Novos cálculos da física da atmosfera do Sol fornecem resultados atualizados para abundâncias de diferentes elementos químicos, que resolvem o conflito. Notavelmente, o Sol contém mais oxigênio, silício e neon do que se pensava anteriormente. Os métodos empregados também prometem estimativas consideravelmente mais precisas das composições químicas das estrelas em geral.

O que você faz quando um método testado e comprovado para determinar a composição química do Sol parece estar em desacordo com uma técnica inovadora e precisa para mapear a estrutura interna do Sol? Essa era a situação enfrentada pelos astrônomos que estudam o Sol – até novos cálculos que agora foram publicados por Ekaterina Magg, Maria Bergemann e colegas, e que resolvem a aparente contradição.

Espectro do Sol, obtido com o espectrógrafo de altíssima resolução NARVAL instalado no Telescópio Bernard Lyot, Observatoire Midi-Pyrénées. Espectros como este, em particular as propriedades das linhas de absorção escuras que são claramente visíveis nesta imagem, permitem aos astrônomos deduzir a temperatura e a composição química de uma estrela. Crédito: © M. Bergemann / MPIA / [email protected]

O método testado e comprovado em questão é a análise espectral. A fim de determinar a composição química do nosso Sol, ou de qualquer outra estrela lá fora, os astrônomos rotineiramente recorrem aos espectros: a decomposição da luz semelhante a um arco-íris em seus diferentes comprimentos de onda. Os espectros estelares contêm linhas escuras nítidas e conspícuas, notadas pela primeira vez por William Wollaston em 1802, redescobertas por Joseph von Fraunhofer em 1814 e identificadas como sinais indicadores que indicam a presença de elementos químicos específicos por Gustav Kirchhoff e Robert Bunsen na década de 1860.

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