A year that is a mere 18 hours TOI 849 b is an extremely unusual planet in the so-called “Neptune Desert” – a term used by astronomers for a region close to stars where we rarely see planets of Neptune’s mass or larger.
The lead author of the study, Dr. David Armstrong from the University of Warwick, says: “The planet is strangely close to its star, considering its mass. In other words, we don’t see planets with this mass at these short orbital periods.” TOI 849 b orbits so close to its host star that a year is a mere 18 hours and its surface temperature is around 1,500 °C.
Christoph Mordasini explains: “We have determined the planet’s mass and radius. TOI-849b is about 40 times heavier than the earth, but its radius is just 3.4 earth radii.” So the planet has a high density and therefore has to primarily consist of iron, rock and water, but only very little hydrogen and helium. “Such a small amount of hydrogen and helium is really astonishing for such a massive planet. We would expect a planet this massive to have accreted large quantities of hydrogen and helium when it formed.”
David Armstrong adds: “The fact that we don’t see those gases lets us know TOI 849 b is an exposed planetary core.” This is the first time that an intact exposed core of a gas giant has been discovered around a star.
Bern’s expertise in demand worldwide
The University of Bern has been continuously developing the “Bern Model of Planet Formation and Evolution” since 2003. Christoph Mordasini says: “In our model, we combine insights into the manifold processes involved in the formation and evolution of planets.” Thanks to the world-renowned Bern model, discoveries such as those of the exoplanet TOI 849 b can be interpreted theoretically.
Based on the Bern model, two theories can be formulated which explain why TOI 849 b is not a typical gas giant but an exposed planetary core. “The first is that the exoplanet was once similar to Jupiter but lost nearly all of its outer gas through a variety of processes,” Christoph Mordasini says. These could include tidal disruption, where the planet is ripped apart from orbiting too close to its star, or even a collision with another planet. Large-scale photoevaporation of the atmosphere could also play a role, but can’t account for all the gas that has been lost.
Alternatively, TOI 849 b could be a “failed” gas giant. “Once the core of the gas giant formed then something very unusual could have happened and it never formed a massive atmosphere as normally. This could have occurred if there was a gap in the disk of dust and gas that the planet formed from due to gravitational interaction with the planet, or if the disk ran out of material right at the very moment when gas accretion normally follows,” Mordasini adds.
David Armstrong says: “Our discovery proves that planets like this exist and we can track them down. We have the opportunity to look at the core of a planet in a way that we can’t do in our own solar system.”
How TOI 849 b was discovered and analyzed
TOI 849 b was found in a survey of stars by NASA’s Transiting Exoplanet Survey Satellite (TESS), using the transit method: the satellite measures the brightness of a star. A dip in brightness indicates that a planet has passed in front of them.
TOI 849 b was then analyzed using the HARPS instrument built under Swiss leadership, at the European Southern Observatory’s La Silla Observatory in Chile. This utilizes the Doppler effect to measure the mass of exoplanets by measuring their ‘wobble’ – small movements towards and away from us that register as tiny shifts in the star’s spectrum of light.
“Bern Model of Planet Formation and Evolution”
Statements can be made about how a planet was formed and how it has evolved using the “Bern Model of Planet Formation and Evolution”. The Bern model has been continuously developed at the University of Bern since 2003. Insights into the manifold processes involved in the formation and evolution of planets are integrated into the model. These are, for example, submodels of accretion (growth of a planet’s core) or of how planets interact gravitationally and influence each other, and of processes in the protoplanetary disks in which planets are formed. The model is also used to create so-called population syntheses, which show which planets develop how frequently under certain conditions in a protoplanetary disk. The world-renowned Bern model is also used for the theoretical interpretation of discoveries such as that of the TOI 849 b exoplanet.
Information about the publication:
‘A remnant planetary core in the hot-Neptune desert’, David Armstrong et al.,01.07.2020, Nature
