Planetas perdidos do Sistema Solar

Você já reparou como muitos dos sistemas planetários descobertos até agora têm vários planetas localizados em órbitas bem pequenas, bem menores que as da Terra? Pois bem. Agora uma dupla de astrônomos nos Estados Unidos está propondo que o Sistema Solar também pode ter sido assim nos seus primórdios, com vários planetas maiores que o nosso ocupando órbitas mais internas.

Planetas perdidos do Sistema Solar (Crédito: Nasa)


Será que o Sistema Solar já foi parecido com Kepler-11, sistema que tem seis planetas maiores que a Terra em órbitas próximas de sua estrela? Uma dupla de pesquisadores acredita que sim. (Crédito: Nasa)

Certo, fácil falar. Mas onde estão esses planetas agora?

De acordo com simulações realizadas por Greg Laughlin, da Universidade da Califórnia em Santa Cruz, e Konstantin Batygin, do Caltech (Instituto de Tecnologia da Califórnia), esses mundos primordiais teriam sido destruídos por um evento cataclísmico, e foi isso que viabilizou o posterior surgimento da Terra. Se os pesquisadores estiverem certos, mundos de pequeno porte e com atmosferas modestas, como o nosso, podem ser bem mais raros do que antes se imaginava.

A conclusão é bombástica, porque enfatiza que muitos dos planetas detectados fora do Sistema Solar que, pelo porte, se assemelhariam à Terra podem na verdade ser completamente diferentes.

“Dramaticamente, nosso trabalho implica que a maioria dos planetas com massa similar à terrestre é fortemente enriquecida em elementos voláteis e é inabitável”, escrevem os pesquisadores em seu artigo, publicado na última edição do periódico “PNAS”.

(Você se interessa pelo tema busca por vida extraterrestre e deseja se aprofundar no assunto? Dê uma olhadinha nisto aqui!)

DE ONDE VEIO ISSO?
Parece uma conclusão extraordinária. E é mesmo. Estamos falando de eventos hipotéticos ocorridos há 4,6 bilhões de anos, dos quais há praticamente nenhuma evidência. O trabalho é altamente especulativo e explora tudo que temos descoberto sobre a formação de planetas nas últimas duas décadas. Vamos recapitular esses passos, e aí a história da pesquisa vai se assemelhar muito à clássica desculpa de bêbado: “Sabe como é, uma coisa levou a outra…”

Tudo começa em 1995, quando o primeiro planeta em torno de outra estrela similar ao Sol, 51 Pegasi b, foi descoberto. Ele era um gigante gasoso, como Júpiter. Até aí tudo bem. O problema é que ele completava uma volta em torno de sua estrela em coisa de quatro dias. Era algo simplesmente impossível, a julgar por tudo que achávamos que sabíamos sobre formação de planetas. Bastou essa única e solitária descoberta para colocar nossos frágeis modelos em xeque, inspirados unicamente pela arquitetura do nosso próprio sistema. Vamos a ela.

Ao redor do Sol, os planetas estão distribuídos confortavelmente em longas órbitas, com os mundos rochosos e menores na região interna do sistema e os gigantes gasosos na região externa. O mais interno dos planetas, Mercúrio, é também o menor, e completa uma volta em torno do Sol em 88 dias.

Compare isso à bizarrice de 51 Peg b — um planeta gigante praticamente colado à sua estrela. Os cientistas estavam convencidos de que aquele mundo jamais poderia ter se formado ali, pois a estrela recém-nascida teria “soprado” todo o gás daquela região antes que o planeta pudesse acumulá-lo em sua volumosa atmosfera. Com isso, os astrônomos começaram a levar a sério a noção de migração planetária — o fato de que interações entre mundos recém-nascidos e o disco de gás e poeira que circunda a estrela e dá origem a eles poderia fazer com que suas órbitas se deslocassem.

No fim das contas, duas décadas e mais de mil exoplanetas depois, já sabemos que o caso de 51 Peg b era mesmo extremo — menos de 1% das estrelas têm um “Júpiter Quente” como ele. Contudo, também restava conclusivamente demonstrado que a migração planetária, em diferentes escalas, era um fenômeno bem possível e comum.

Ao mesmo tempo, com o aumento da amostra de sistemas, descobrimos que o nosso Sistema Solar também não era lá a coisa mais comum do Universo. Muitos dos exoplanetas menores que Júpiter se distribuem em órbitas bem mais próximas de suas estrelas que as vistas nos nossos quatro mundos rochosos — Mercúrio, Vênus, Terra e Marte.

Laughlin e Batygin citam em seu artigo o caso emblemático do sistema Kepler-11, descoberto em 2011, que tem seis planetas, todos eles com diâmetros entre duas e quatro vezes o da Terra, distribuídos por uma região apenas um pouco maior que a órbita de Mercúrio. Ou seja, onde aqui temos apenas um mundo com meio décimo da massa terrestre, lá existem seis planetas com uma massa total equivalente a pelo menos 40 Terras. E o detalhe sinistro: o Sol e a estrela Kepler-11 são bem parecidos, o que faz supor que talvez ambos tenham tido mais ou menos a mesma quantidade de material ao seu redor para formação planetária. Para onde foi essa joça toda em nosso Sistema Solar, considerando que os nossos quatro planetas rochosos não somam nem três massas terrestres?

REFINANDO O SISTEMA SOLAR
Enquanto isso, os modelos de formação do Sistema Solar encontravam suas próprias dificuldades. Mesmo modulando a quantidade de material para acabar com uma massa compatível com a dos planetas que temos por aqui, as simulações não produziam de jeito nenhum um Marte com o tamanho certo. Ele sempre saía “maior que a encomenda”, mais ou menos como a Terra.

Isso até 2011, quando um grupo de pesquisadores publicou na “Nature” um artigo sugerindo uma solução. A resposta estaria na migração de Júpiter. Suponha que ele tenha se formado a 3,5 UA de distância do Sol (uma unidade astronômica é a distância média Terra-Sol, cerca de 150 milhões de quilômetros) e depois migrado para dentro até uma posição a cerca de 1,5 UA, perturbando o disco de gás e poeira naquela região, para finalmente migrar para fora, até 5,2 UA (sua posição atual), puxado por Saturno, recém-nascido. Se tudo isso aconteceu, as simulações resultantes produzem Marte no tamanho certo e também explicam a distribuição dos objetos do cinturão de asteroides e a presença de água nos planetas rochosos.

A farra do Grand Tack, a migração temporária de Júpiter e Saturno e os Planetas perdidos do Sistema Solar (Crédito:Nasa) e (Crédito: Kevin Walsh et. al)

A farra do Grand Tack, a migração temporária de Júpiter e Saturno (Crédito: Kevin Walsh et al.)

Desde então, essa hipótese, conhecida como “Grand Tack”, tem sido levada bastante a sério. Afinal, os exoplanetas mostram que migração planetária é um fenômeno mais que comum. Por que não poderia ter acontecido em nosso próprio sistema?

E foi aí que “uma coisa levou a outra” no trabalho de Laughlin e Batygin. Eles pensaram: e se o nosso Sistema Solar também começou com um monte de planetas na região interna do disco, que teriam se formado na mesma época de Júpiter, o que o Grand Tack teria causado em suas órbitas?

DEVASTAÇÃO
O resultado foi basicamente um massacre. As órbitas são bagunçadas, os planetas acabam colidindo uns com os outros, produzem uma reação em cadeia, tudo vira um monte de pedregulhos novamente e a maior parte desse material acaba caindo na direção do Sol. O que sobra acaba formando novos planetas — dessa vez bem menores e mais espaçados. Mercúrio, Vênus, Terra e Marte. Nós.

Imagem de uma das simulações de Batygin e Laughlin do que teria acontecido no nosso Sistema Solar -- uma bagunça. e os Planetas perdidos do Sistema Solar (Crédito:Nasa) e (Crédito: Batygin et. al)

Imagem de uma das simulações de Batygin e Laughlin do que teria acontecido no nosso Sistema Solar — uma bagunça. (Crédito: Konstantin Batygin et al.)

Uma pergunta que pode ter ocorrido a você a essa altura: foi isso mesmo que aconteceu? Atenção para a resposta mais honesta que se pode dar em ciência: não sabemos.

ALTERNATIVA
Em contrapartida, outra hipótese tem sido defendida em trabalhos recentes pelo astrônomo brasileiro André Izidoro, pesquisador da Unesp (Universidade Estadual Paulista) e da Universidade de Nice, na França. Em 2014, ele publicou um artigo no “Astrophysical Journal” mostrando que o Grand Tack não era realmente necessário para a formação de Marte — em vez disso, uma mera flutuação na densidade do disco na região poderia explicar o surgimento do planeta vermelho com seu tamanho observado.

“Ou seja, não pode ser assumido como verdade absoluta que Júpiter de fato migrou tanto para as regiões mais internas e voltou depois para uma região mais externa”, disse ao Mensageiro Sideral o astrônomo Jorge Meléndez, da USP (Universidade de São Paulo), que não participou de nenhum dos trabalhos. “O que eu não gostei do artigo da ‘PNAS’ é que ele não discute muito explicações alternativas, como a do trabalho do Izidoro”, completa.

Mas, se não houve Grand Tack, por que o Sistema Solar não tem lá suas superterras? Em parceria com alguns dos proponentes originais do Grand Tack, Izidoro acaba de mostrar que as superterras podem ser planetas originários das regiões mais externas que então migram para dentro — exceto se houver um gigante gasoso no meio do caminho para barrá-los. Em seu mais novo artigo, submetido em janeiro deste ano e aceito para publicação no “Astrophysical Journal Letters”, ele apresenta essa hipótese, sugerindo que Urano e Netuno — e possivelmente Saturno — talvez tivessem migrado para dentro e se tornado superterras ou mininetunos (terminando menores que seu tamanho atual por viajarem para regiões com menos gás durante sua formação), se Júpiter não estivesse no meio do caminho para impedi-los de passar.


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Continuando...

Ou seja, Izidoro e seus colegas preveem que sistemas com muitas superterras próximas à estrela devem não ter gigantes gasosos afastados. E isso fornece um meio de testar a hipótese. No momento, apesar de quase 2 mil planetas descobertos, ainda nos faltam estatísticas confiáveis para apontar em qualquer direção. Se encontrarmos muitas superterras em sistemas com gigantes gasosos, saberemos que Izidoro está errado e Laughlin e Batygin devem estar na trilha certa. Por outro lado, se encontrarmos gigantes gasosos com no máximo uma superterra mais interna (as simulações mostram que, em algumas raras ocasiões, a superterra consegue “pular” o gigante gasoso e migrar para dentro sem ser ejetada do sistema), e mais frequentemente nenhuma, então saberemos que Izidoro e seus colegas acabaram acertando o alvo. Nesse caso, poderemos concluir que o Sistema Solar provavelmente nunca teve as superterras primordiais que a dupla da Califórnia propõe.

Talvez essa história toda seja cifrada demais para quem espera da ciência respostas claras e inequívocas. Mas hoje fizemos uma visita aos “porões da astronomia”, por assim dizer. Tiramos os esqueletos do armário e mostramos muito mais o que não sabemos do que o que de fato compreendemos. É aquele estágio de confusão que antecede os consensos, em meio a debates de hipóteses conflitantes, todas passíveis de teste por experimentos (no caso, simulações) e observações (no estudo de exoplanetas). E essa na verdade é a grande força da ciência. Ela não permite que as ideias — por mais belas que sejam — se sobreponham aos fatos. E, no processo, ainda ganhamos um lampejo mais claro da incrível força criativa da natureza. Ainda não sabemos com que receita exata se produzem as arquiteturas dos exoplanetas. Mas já temos a convicção de que elas são mais variadas do que sequer conseguimos imaginar. Que bom!

Acompanhe o Mensageiro Sideral no Facebook e no Twitter

PARA IR MAIS FUNDO
Em tese, o texto acabou aí em cima. Mas, se você ainda não se cansou do tema, logo abaixo vai a entrevista que fiz com o russo Konstantin Batygin, um dos autores da hipótese das superterras solares, sobre seu trabalho na “PNAS”. Com 28 anos, ele é professor assistente do Caltech e foi eleito um dos “30 abaixo de 30″ da revista “Forbes”, que destaca os cientistas que despontam ainda jovenscomo expoentes acadêmicos. (Aviso aos navegantes: o papo é tão cabeludo quanto ele.)

O astrônomo russo Konstantin Batygin, autor do artigo das superterras solares. E os Planetas perdidos do Sistema Solar (Créditos:Nasa e Caltech)

O astrônomo russo Konstantin Batygin, autor do artigo das superterras solares. (Crédito: Caltech)

Mensageiro Sideral – É interessante propor que o Sistema Solar tinha mais planetas mais internos que Mercúrio, mas isso não entra em conflito com nossos modelos mais aceitos de formação planetária quando aplicados ao Sistema Solar? A maioria dos pesquisadores tende a explicar exoplanetas próximos à estrela por meio de migração, em vez de formação in-situ. Por que vocês acharam que deviam inverter isso?

Konstantin Batygin - O modo exato de formação planetária, aplicado a sistemas planetários compactos, permanece uma questão controversa, mas de fato não é muito crucial para o modelo que apresentamos. Se nosso entendimento de formação de planetas gigantes está correto, então a formação de planetas sólidos, como superterras e netunos, deve acontecer antes da formação de Júpiter e Saturno, porque eles agem como núcleos que mais tarde acretam gás para se tornar gigantes. Além disso, formação de planetas gigantes é fundamentalmente não muito eficiente, de forma que o número de núcleos provavelmente excedeu o número de gigantes gasosos por uma fração substancial (as estatísticas extra-solares confirmam isso). Portanto, independentemente de as superterras terem se formado in-situ ou distantes e depois carregadas para dentro por migração extensa, é provável que elas tenham existido no Sistema Solar antes que Júpiter e Saturno tenham se formado e iniciado sua jornada.

Mensageiro Sideral – Eu pensei que neste momento a maioria dos pesquisadores concordasse com a ideia de que os planetas gigantes (Júpiter e Saturno, no nosso caso) se formassem antes, porque eles precisavam acretar rápido o suficiente de forma que o gás não tenha ainda sido inteiramente dissipado pela estrela nascente. Esse é um problema antigo dos estudos de acreção de núcleos, mas eu estava com a impressão de que a maioria dos cientistas hoje já favorece modelos em que Júpiter vem primeiro, e os planetas terrestres têm mais tempo de crescer até seus tamanhos finais. Não é isso? A maioria dos cientistas planetários não acredita que Júpiter veio primeiro em nosso Sistema Solar?

Batygin - Bem, esse é um assunto complicado.

No Sistema Solar, a formação de planetas evidentemente aconteceu em duas ondas

A primeira gerou os planetas massivos: Júpiter, Saturno, Urano e Netuno. Essa primeira onda levou menos de 10 milhões de anos para se completar.

A segunda onda ocorreu numa escala de 100 milhões de anos e gerou os planetas de baixa massa:

Mercúrio, Vênus, Terra e Marte. É convencionalmente presumido que a maioria dos exoplanetas em órbitas compactas participou de migração induzida pelo disco (embora, como eu disse antes, esse ponto seja discutível). Então eles devem ter sido gerados enquanto o gás estava por aí, e portanto deveriam pertencer ao mesmo grupo de planetas que Júpiter, Saturno, Urano e Netuno. Note que até mesmo no Sistema Solar, Urano e Netuno representam núcleos que fracassaram em acretar quantidades substanciais de gás (eles têm apenas cerca de uma massa terrestre de hidrogênio e hélio cada um). O que o nosso estudo faz é sugerir que Urano e Netuno não foram os únicos núcleos fracassados do Sistema Solar. Em vez disso, sugerimos que antes que Júpiter tivesse se formado (de acordo com modelos de formação convencionais, a acreção de Júpiter leva cerca de 3 milhões de anos), o Sistema Solar gerou vários núcleos que eram parte do mesmo processo dominante de formação planetária que é comumente responsável por planetas com órbitas compactas que observamos em torno de outras estrelas.

Mensageiro Sideral – Se vocês estiverem certos, então planetas do tamanho da Terra encontrados em órbitas mais compactas em torno de outras estrelas deveriam ser fundamentalmente diferentes da Terra. Contudo, para a maioria dos planetas com massa e tamanho similares aos da Terra que tiveram sua densidade medida, encontramos valores entre os da Terra e de Mercúrio. Isso não entra em conflito com sua expectativa de que esses planetas mais internos tivessem maior quantidade de material volátil e fossem menos densos que a Terra?

Batygin - Na verdade, medidas de densidade de superterras extra-solares variam enormemente. Algumas são consistentes com a densidade de rocha, outras com gelo, enquanto outras são muito mais baixas, indicando que devem ser enriquecidas em hidrogênio e hélio. Há um viés, contudo: é mais fácil medir as massas de planetas com densidades maiores, então eles tendem a ter barras de erro melhores. Mas geralmente composições de planetas extra-solares sugerem que planetas como a Terra (aqueles sem atmosferas apreciáveis) são uma exceção à regra, em vez da norma.

Mensageiro Sideral – Eu sei que as densidades variam bastante para planetas do tipo superterra, mas estudos mais recentes, apresentados na última reunião da AAS, parecem mostrar que há uma forte correlação com tamanho: menos que 1,6 raio terrestre tende a ser planeta rochoso, mais que 1,6 raio terrestre tende a ser mininetuno. Isso não derruba a ideia de que é a história do sistema, em vez de suas propriedades intrínsecas, o que determina quem acaba se parecendo com planeta gigante ou não?

Batygin - Essa é uma pergunta excelente, mas a resposta a essa questão não é trivial por duas razões. Primeiro é que a evaporação importa. Deve existir algum tamanho crítico de objeto numa dada órbita aquém do qual, mesmo que você comece com uma atmosfera rica em hidrogênio, ela acaba soprada durante os estágios iniciais de formação planetária (porque o fluxo extremo de UV pode ser muito alto). Esse tamanho pode ser muito bem 1,6 raio terrestre para órbitas típicas de exoplanetas. Segundo é que uma vez que frações significativas de gás são introduzidas, as relações de massa-raio dos planetas podem se tornar bem complicadas. Ou seja, torna-se difícil traduzir o que um objeto de 1,6 raio terrestre significa em termos de massa. Pode ser um objeto rochoso com 4 massas terrestres ou um objeto rico em gás com 1,5 massa terrestre. Ambos podem produzir o mesmo raio. No fim das contas, parece que uma fração substancial dos exoplanetas observados (na classe das superterras) se formou enquanto havia gás, o que é a premissa inicial do nosso trabalho.

Mensageiro Sideral – Por fim, não temos de lidar com o fato de que temos um viés observacional forte em favor de sistemas compactos, seja qual for o método, velocidade radial ou trânsito? Isso não deveria contar para determinarmos quão estranho nosso próprio sistema planetário parece ser?

Batygin - Com certeza sim, e esse viés observacional é cuidadosamente levado em conta. Considerando isso, cálculos estatísticos sugerem que cerca de metade das estrelas similares ao Sol observadas possuem planetas em órbitas compactas menos massivos que 20 massas terrestres. Isso deveria ser comparado com a taxa de ocorrência de gigantes gasosos como Júpiter e Saturno, que é de apenas cerca de 10%. Então, embora a formação de planetas seja comum, seu modo dominante gera preferencialmente objetos sub-jovianos em órbitas compactas.

Fonte:Salvador Nogueira é jornalista de ciência e autor de oito livros

Todos os direitos da Adaptação reservados a Suporte Ninja
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As caixas-pretas utilizadas para registro de dados em navios e aviões possuem diversas vulnerabilidades que permitem um atacante modificar ou apagar os dados presentes nestes dispositivos Caixas-Pretas de navios ...
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Pablo The Roots

Usuário de MS-DOS e Windows 3.11, profissional de Suporte desde 1999, autodidata e entusiasta da cultura Hacker, Pesquisador autônomo da Segurança da Informação além de amante da Shell Unix. [email protected] ~$ sudo su - [email protected] ~# find / -iname corrupção -exec rm -rfv {} \+

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