La súper Tierra orbitando Gl 486

Un equipo científico internacional liderado por el Instituto Max Planck de Astronomía (MPIA) alemán y en el que participan astrónomos del Centro de Astrobiología (CAB, CSIC-INTA) ha descubierto recientemente una super-Tierra caliente situada en el vecindario de nuestro Sol. El hallazgo de este exoplaneta se considera de gran trascendencia, ya que su ardiente atmósfera puede ser la piedra de Rosetta para estudiar exoplanetas habitables en un futuro cercano.

Durante los últimos 25 años, los astrónomos han descubierto una gran variedad de exoplanetas compuestos de roca, hielo y gas. La puesta en operación de instrumentos astronómicos específicamente diseñados para la caza de exoplanetas ha permitido elevar a varios miles el número de mundos descubiertos fuera del Sistema Solar. De todos ellos, los que se parecen a la Tierra se pueden contar con los dedos de una mano.

Mediante la combinación de diferentes técnicas de observación, los astrónomos han sido capaces de determinar una gran cantidad de masas, tamaños e incluso densidades planetarias, lo que permite estimar su composición interna. Uno de los grandes objetivos de los astrónomos es caracterizar plenamente los exoplanetas similares a la Tierra mediante el estudio de sus atmósferas. Sin embargo, estudiar las atmósferas de estos planetas rocosos es extremadamente difícil con la instrumentación disponible en la actualidad. Por este motivo, los modelos atmosféricos disponibles de planetas rocosos siguen sin ser probados.

En este sentido, los astrónomos del consorcio CARMENES (Calar Alto high- Resolution search for M dwarfs with Exoearths with Near-infrared and optical échelle Spectrographs), en el que participa el Centro de Astrobiología (CAB, CSIC-INTA), han hecho público recientemente un estudio, liderado por Trifon Trifonov, astrónomo del Instituto Max Planck de Astronomía en Heidelberg (Alemania), sobre el descubrimiento de una super-Tierra caliente orbitando la cercana estrella enana roja Gliese 486, situada a tan solo 26 años-luz del Sol. Los científicos emplearon las técnicas combinadas de fotometría de tránsito y espectroscopia de velocidad radial para hacer el descubrimiento. Los resultados del estudio se publican mañana en la revista Science.

El planeta descubierto, bautizado como Gliese 486b, tiene 2,8 veces la masa de nuestro planeta y es solo un 30% más grande. Al calcular su densidad media a partir de las mediciones de su masa y su radio, se deduce que la composición es similar a la de Venus o la Tierra, que poseen núcleos metálicos en su interior. Un astronauta en la superficie de Gliese 486b sentiría una gravedad un 70% mayor que la que experimentaría en la Tierra.

El planeta gira en torno a su estrella anfitriona en una trayectoria circular cada 1,5 días y a una distancia de 2,5 millones de kilómetros. A pesar de estar situado muy cerca de su estrella anfitriona, Gliese 486b, ha conservado probablemente una parte de su atmósfera original. Por este motivo, Gliese 486b es un candidato ideal para examinar su atmósfera e interior con la próxima generación de telescopios espaciales y terrestres.
Para Trifonov, “la cercanía al Sol de este exoplaneta es emocionante porque será posible estudiarlo en mayor detalle utilizando potentes telescopios como el próximo Telescopio Espacial James Webb y el ELT (Extremely Large Telescope) actualmente en construcción”. En los planetas rocosos como la Tierra, cuando existe, la atmósfera consiste en una delgada capa gaseosa. Por este motivo, no todas las atmósferas planetarias que pueden ser observadas con los observatorios de próxima generación, sino solo aquellas que cumplan unos requisitos previos específicos.

Gliese 486b tarda el mismo tiempo en rotar alrededor de su eje de giro que en describir la órbita alrededor de su estrella anfitriona, por lo que siempre muestra la misma cara hacia la estrella. Aunque la estrella Gliese 486 es mucho más débil y fría que el Sol, la irradiación es tan intensa que la superficie del planeta se calienta hasta al menos 700 K (unos 430 °C). Debido a ello, la superficie de Gliese 486b probablemente se parece más a la de Venus que a la de la Tierra, con un paisaje caliente y seco, surcado por ardientes ríos de lava. Sin embargo, a diferencia de Venus, Gliese 486b posiblemente tiene una atmósfera tenue, si la tiene. Los cálculos realizados con los modelos existentes de atmósferas planetarias pueden ser consistentes con ambos escenarios de superficie caliente y atmósfera tenue, porque la irradiación estelar tiende a evaporar la atmósfera, mientras que la gravedad del planeta tiende a retenerla. Determinar el equilibrio entre ambas contribuciones es difícil en la actualidad.

“El descubrimiento de Gliese 486b ha sido un golpe de suerte. Si hubiera estado un centenar de grados más caliente, toda su superficie sería de lava y su atmósfera consistiría en rocas vaporizadas” señala José Antonio Caballero, investigador del CAB y coautor del estudio. “Por otro lado, si Gliese 486b fuera un centenar de grados más frío, no habría sido adecuado para observaciones de seguimiento”, concluye Caballero.

Las futuras mediciones que el equipo de CARMENES tiene previsto tratarán de determinar la orientación orbital, que hace posible que Gliese 486b cruce la superficie de la estrella anfitriona desde nuestro punto de vista, eclipsándola. Cada vez que esto sucede, y que los astrónomos denominan tránsitos, una pequeña fracción de la luz estelar pasa a través de la fina capa atmosférica de Gliese 486b antes de llegar a la Tierra. Los gases que componen la atmósfera absorben la luz a longitudes de onda específicas, “dejando su huella dactilar” en la señal que llega a los instrumentos. Mediante el uso de espectrógrafos, los astrónomos descomponen la luz en las diferentes longitudes de onda y buscan las características de absorción presentes, para derivar de ellas la composición atmosférica. Este método se conoce como espectroscopia de tránsito.

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También se realizarán mediciones espectroscópicas, mediante la llamada espectroscopia de emisión, cuando las zonas del hemisferio iluminado por la estrella se hacen visibles en forma de fases (no lunares, sino planetarias en este caso) durante la órbita de Gliese 486b hasta que desaparece detrás de la estrella. El espectro obtenido contiene información sobre las condiciones de la superficie planetaria iluminada y caliente.
“Esperamos ansiosos que los nuevos telescopios estén disponibles”, admite Trifonov, “los resultados que obtengamos con ellos nos ayudarán a entender mejor las atmósferas de los planetas rocosos, su extensión, densidad, composición y su influencia en la distribución de energía en los planetas”.
Tanto Trifonov como Caballero colaboran en el proyecto CARMENES, cuyo consorcio está integrado por once instituciones de investigación en España y Alemania. Su propósito es monitorear un conjunto de 350 estrellas enanas rojas en busca de planetas como la Tierra, utilizando para ello un espectrógrafo instalado en el telescopio de 3,5 m del observatorio de Calar Alto (España). El presente estudio ha contado, además, con mediciones espectroscópicas adicionales para inferir la masa de Gliese 486b. Se obtuvieron observaciones con el instrumento MAROON-X en el telescopio Gemini North de 8,1 m (EE.UU.) y se recuperaron datos de archivo del telescopio Keck de 10 m (EE.UU.) y del telescopio ESO de 3,6 m (Chile).
Las observaciones fotométricas provienen del observatorio espacial TESS (Transiting Exoplanet Survey Satellite) (NASA, EE. UU.), cuyos datos fueron fundamentales para determinar el radio del planeta, del instrumento MuSCAT2 (Multicolour Simultaneous Camera for studying Atmospheres of Transiting exoplanets 2) instalado en el Telescopio Carlos Sánchez de 1,52 m en el Observatorio del Teide (España), y el LCOGT (Telescopio Global del Observatorio Las Cumbres) en Chile, entre otros.

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