Um alinhamento cósmico e um pouco de ginástica espacial forneceram uma medição inovadora que está ajudando a resolver o mistério cósmico de 65 anos que explica por que a atmosfera do Sol é tão quente.
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)
A atmosfera externa do Sol, conhecida como coroa, pode ser vista estendendo-se pelo espaço nesta imagem obtida pelo instrumento Metis da Solar Orbiter. Metis é um dispositivo de vários comprimentos de onda, trabalhando em comprimentos de onda visíveis e ultravioleta. É um coronógrafo, o que significa que bloqueia a luz solar brilhante da superfície solar, deixando visível a luz mais fraca que dispersa as partículas na coroa. Nesta imagem, o disco vermelho difuso representa o coronógrafo, enquanto o disco branco é uma máscara para comprimir o tamanho da imagem e reduzir a quantidade de dados desnecessários transmitidos. Há um mistério duradouro em torno da coroa: a sua temperatura. Composta por um gás magnetizado chamado plasma, a coroa tem uma temperatura de cerca de um milhão de graus Celsius, mas não pode ser aquecida pela superfície solar, muito mais fria. Os físicos solares há muito que suspeitam que a turbulência deve estar envolvida, mas tem sido difícil reunir as medições necessárias para investigar esta hipótese. Recentemente surgiu uma oportunidade. Em 1 de junho de 2022, a espaçonave Solar Orbiter liderada pela ESA foi ligeiramente virada e rolada para o lado, para que Metis pudesse ver a parte da coroa através da qual a Sonda Solar Parker da NASA estava voando. Esta manobra significou que, pela primeira vez, os físicos solares registaram tanto o comportamento in-situ do plasma na coroa solar como as consequências em grande escala. Isto permitiu-lhes fazer a primeira estimativa combinada da taxa de aquecimento coronal. Os resultados fornecem fortes evidências de que a turbulência no plasma magnetizado está de fato causando o aquecimento extraordinário. Crédito: ESA e NASA/equipe Solar Orbiter/Metis; D.
Um alinhamento cósmico e um pouco de ginástica espacial forneceram uma medição inovadora que está ajudando a resolver o mistério cósmico de 65 anos que explica por que a atmosfera do Sol é tão quente.
A atmosfera do Sol é chamada de coroa. Consiste em um gás eletricamente carregado conhecido como plasma e tem uma temperatura de cerca de um milhão de graus Celsius.
Sua temperatura é um mistério duradouro porque a superfície do Sol está apenas em torno de 6.000 graus. A coroa deveria ser mais fria que a superfície porque a energia do Sol vem da fornalha nuclear em seu núcleo, e as coisas ficam naturalmente mais frias quanto mais longe estão de uma fonte de calor. No entanto, a coroa é 150 vezes mais quente que a superfície.
Outro método para transferir energia para o plasma deve estar em ação, mas qual?
Há muito que se suspeita que a turbulência na atmosfera solar poderia resultar num aquecimento significativo do plasma na coroa. Mas quando se trata de investigar este fenómeno, os físicos solares deparam-se com um problema prático: é impossível reunir todos os dados de que necessitam com apenas uma nave espacial.
Existem duas maneiras de investigar o sol: sensoriamento remoto e medições in situ. No sensoriamento remoto, a espaçonave é posicionada a uma certa distância e usa câmeras para observar o sol e sua atmosfera em diferentes comprimentos de onda. Para medições in-situ, a espaçonave voa pela região que deseja investigar e faz medições das partículas e dos campos magnéticos naquela parte do espaço.
Ambas as abordagens têm suas vantagens. O sensoriamento remoto mostra os resultados em grande escala, mas não os detalhes dos processos que acontecem no plasma. Enquanto isso, as medições in-situ fornecem informações altamente específicas sobre os processos de pequena escala no plasma, mas não mostram como isso afeta a grande escala.
Para ter uma visão completa, são necessárias duas espaçonaves. Isso é exatamente o que os físicos solares têm atualmente na forma da espaçonave Solar Orbiter liderada pela ESA e da Parker Solar Probe da NASA. O Solar Orbiter foi projetado para chegar o mais próximo possível do Sol e ainda realizar operações de sensoriamento remoto, juntamente com medições in-situ. A Parker Solar Probe renuncia em grande parte ao sensoriamento remoto do próprio Sol para chegar ainda mais perto para suas medições in-situ.
Mas para tirar o máximo partido das suas abordagens complementares, a Parker Solar Probe teria de estar dentro do campo de visão de um dos instrumentos da Solar Orbiter. Dessa forma, a Solar Orbiter poderia registrar as consequências em grande escala do que a Parker Solar Probe estava medindo in situ.
Daniele Telloni, pesquisadora do Instituto Nacional Italiano de Astrofísica (INAF) no Observatório Astrofísico de Torino, faz parte da equipe por trás do instrumento Metis da Solar Orbiter. Metis é um coronógrafo que bloqueia a luz da superfície do Sol e tira fotos da coroa. É o instrumento perfeito para medições em grande escala e, portanto, Daniele começou a procurar os momentos em que a Parker Solar Probe se alinharia.
"Taxa de aquecimento coronal no vento solar lento", de D. Telloni et al., foi publicado no The Astrophysical Journal Letters.
Ele descobriu que em 1º de junho de 2022, as duas espaçonaves estariam na configuração orbital correta – quase. Essencialmente, a Solar Orbiter estaria olhando para o sol e a Parker Solar Probe estaria ao lado, tentadoramente perto, mas fora do campo de visão do instrumento Metis.
Ao analisar o problema, Daniele percebeu que tudo o que seria necessário para trazer a Parker Solar Probe à vista seria um pouco de ginástica com o Solar Orbiter: um giro de 45 graus e, em seguida, apontá-lo ligeiramente para longe do sol.
Mas quando cada manobra de uma missão espacial é cuidadosamente planeada com antecedência, e as próprias naves espaciais são concebidas para apontar apenas em direcções muito específicas, especialmente quando lidam com o temível calor do Sol, não estava claro se a equipa de operações da nave espacial autorizaria tal manobra. um desvio. No entanto, uma vez que todos ficaram claros sobre o potencial retorno científico, a decisão foi um claro “sim”.
O rolamento e o apontamento de deslocamento prosseguiram; A Parker Solar Probe entrou no campo de visão e, em conjunto, a sonda produziu as primeiras medições simultâneas da configuração em grande escala da coroa solar e das propriedades microfísicas do plasma.
“Este trabalho é o resultado da contribuição de muitas, muitas pessoas”, diz Daniele, que liderou a análise dos conjuntos de dados. Trabalhando juntos, eles conseguiram fazer a primeira estimativa combinada observacional e in situ da taxa de aquecimento coronal.
"A capacidade de utilizar tanto a Solar Orbiter como a Parker Solar Probe abriu realmente uma dimensão inteiramente nova nesta investigação," afirma Gary Zank, da Universidade do Alabama em Huntsville, EUA, e co-autor do artigo resultante.
Ao comparar a taxa recentemente medida com as previsões teóricas feitas pelos físicos solares ao longo dos anos, Daniele mostrou que os físicos solares estavam quase certamente certos na sua identificação da turbulência como forma de transferência de energia.
A maneira específica como a turbulência faz isso não é diferente do que acontece quando você mexe sua xícara de café matinal. Ao estimular movimentos aleatórios de um fluido, seja ele gás ou líquido, a energia é transferida para escalas cada vez menores, o que culmina na transformação de energia em calor. No caso da coroa solar, o fluido também é magnetizado e, portanto, a energia magnética armazenada também fica disponível para ser convertida em calor.
Tal transferência de energia magnética e de movimento de escalas maiores para escalas menores é a própria essência da turbulência. Nas escalas menores, permite que as flutuações finalmente interajam com partículas individuais, principalmente prótons, e as aqueçam.
É necessário mais trabalho antes de podermos dizer que o problema do aquecimento solar está resolvido, mas agora, graças ao trabalho de Daniele, os físicos solares têm a sua primeira medição deste processo.
"Esta é uma inovação científica. Este trabalho representa um passo significativo na resolução do problema do aquecimento coronal", diz Daniel Müller, Cientista do Projeto.
Mais informações: Daniele Telloni et al, Taxa de aquecimento coronal no vento solar lento, The Astrophysical Journal Letters (2023). DOI: 10.3847/2041-8213/ace112
Informações do diário: Cartas de diários astrofísicos