Studying data from the Kepler space telescope, Flatiron Institute researchers found that planetary shrinkage over billions of years likely explains a yearslong mystery: The scarcity of planets roughly double Earth’s size.
While planet-hunting missions have discovered thousands of worlds orbiting distant stars, there’s a severe scarcity of exoplanets that measure between 1.5 and two times Earth’s radius. That’s the middle ground between rocky super-Earths and larger, gas-shrouded planets called mini-Neptunes. Since discovering this ‘radius gap’ in 2017, scientists have been sleuthing out why there are so few midsize heavenly bodies.
What Is Happening Deep Beneath the Surface of Ice Planets?
Cut-away diagram of a water-rich sub-Neptune exo-planet highlighting, in orange color, the interaction region between a deep H2O layer and the underlying rocky mantle. Credit: S. Speziale/ GFZ
The mechanisms of water-rock interaction at the Earth ’ s surface are well known, and the picture of the complex cycle of H 2 O in the deep interior of our and other terrestrial planets is constantly improving. However, we do not know what happens at the interface between hot, dense H 2 O and the deep rocky shell of water-ice planets at pressures and temperatures orders of magnitude higher than at the bottom of the deepest oceans on Earth.
The CARMENES Search For Exoplanets Around M Dwarfs.
Parameters of all known exoplanets around M dwarfs. Left panel: Minimum planet mass versus orbital period. Right panel: RV curve semi-amplitude against host stellar mass. Black squares represent exoplanet parameters for those listed in http//exoplanets.eu on 01 February 2021 and cyan small circles represent TESS detections. Red symbols show planets detected by the CARMENES survey (solid circles) or by its follow-up of TESS detections (solid squares).
We report the discovery of two planetary systems, namely G 264-012, an M4.0 dwarf with two terrestrial planets (Mbsini=2.50+0.29−0.30 M⊕ and Mcsini=3.75+0.48−0.47 M⊕), and Gl 393, a bright M2.0 dwarf with one terrestrial planet (Mbsini=1.71±0.24 M⊕).
What Mass Effect 2 Planets Are Element Zero Rich | Screen Rant
Upgrades are an important gameplay element in Mass Effect 2 , and in order to get them, players will need to scan and probe planets across the galaxy to gather necessary resources. One of these resources is Element Zero. Significantly rarer than the other materials in the game, Element Zero - or " eezo " - may be a struggle for players to find if they don't know where to look.
The process of scanning for materials was introduced to players in Mass Effect 1 , which allowed them to find valuable minerals by accessing various planets and asteroids from the galaxy map. Players could also land on planets and explore them from within ME1 's highly polarizing Mako vehicle , examining artifacts and deposits on-foot to gain resources.
Exoplanet Surveys are Leaning Towards the Possibility That our Solar System is...
One of the unspoken caveats of most exoplanet discovery missions is that they only operate for a few years. Such a short observing window means there are planets with longer orbital periods, usually further out from the star, that those surveys would completely miss. Knowing this would be a problem, a team of astronomers arranged the California Legacy Survey three decades ago in order to monitor as many stars as possible for as long a time as possible.
The survey, now led by a team at Caltech, and headed by Dr. Andrew Howard , has been observing 719 sun-like stars as often as possible to catch any potential exoplanet candidates. They found 177 planets in total, including 14 new ones. Ranging in size from 3 to 6000 times the mass of Earth, they push the detection limits for the ground based telescopes at the Keck and Lick observatories that were used as part of the survey.
Rochester laser experiments demonstrate 'helium rain' likely falls in the solar system :
Nearly 40 years ago, scientists predicted the existence of helium rain inside planets composed primarily of hydrogen and helium, such as Jupiter and Saturn. But achieving the experimental conditions necessary to test this hypothesis has not been possible. That is, until now.
In a paper published in Nature , scientists at the University of Rochester , together with an international collaboration, reveal experimental evidence showing that helium rain—helium droplets falling through liquid metallic hydrogen, much like raindrops of water falling through the atmosphere on Earth—is possible over a range of pressure and temperature conditions that mirror those expected to occur inside planets such as Jupiter and Saturn.
PIAA lacrosse roundup: Mars boys rout Hershey, 12-0 | Pittsburgh Post-Gazette
What's Up | Jupiter & Saturn in the Dawn Sky | Weather Blog | wdrb.com
How were the carbon contents in terrestrial and lunar mantles established? | EurekAlert!
IMAGE: A schematic view of the core-mantle partitioning of carbon in planetary embryos view more
According to the theory of planet formation, rocky bodies such as the Earth were formed by repeating collisions from dusty materials. In this process, a number of Mercury- or Mars-sized planetary embryos, were formed, and eventually these bodies merged together and formed terrestrial planets in our solar system.
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