- Press Release
- Feb 6, 2023
How “Hell Planet” 55 Cnc e Got So Hot
New research sheds light on how the “hell planet” got so devilishly hot and how other worlds might become too toasty for life.
That rocky world, 55 Cnc e (nicknamed “Janssen”), orbits its star so closely that a year lasts just 18 hours, its surface is a giant lava ocean, and its interior may be chock-full of diamond.
The fresh insights come thanks to a new tool called EXPRES that captured ultra-precise measurements of the starlight shining from Janssen’s sun, known as Copernicus or 55 Cnc. The light measurements ever-so-slightly shifted as Janssen moved between Earth and the star (an effect akin to our moon blocking the sun during a solar eclipse).
By analyzing those measurements, astronomers discovered that Janssen orbits Copernicus along the star’s equator — unlike Copernicus’ other planets, which are on such different orbital paths that they never even cross between the star and Earth, the researchers report December 8 in Nature Astronomy.
The implication is that Janssen probably formed in a relatively cooler orbit further out and slowly fell toward Copernicus over time. As Janssen moved closer in, the stronger gravitational pull from Copernicus altered the planet’s orbit.
“We’ve learned about how this multi-planet system — one of the systems with the most planets that we’ve found — got into its current state,” says study lead author Lily Zhao, a research fellow at the Flatiron Institute’s Center for Computational Astrophysics (CCA) in New York City.
Even in its original orbit, the planet “was likely so hot that nothing we’re aware of would be able to survive on the surface,” Zhao says. Still, the new findings could help scientists better understand how planets form and move around over time. Such information is critical to finding out just how common Earth-like environments are in the universe and, therefore, how abundant extraterrestrial life may be.
Our solar system, after all, is the only place in the cosmos where we know life exists. It’s also flat as a pancake — all the planets orbit within a few degrees of one another, having formed from the same disk of gas and dust. When exoplanet-hunting missions started discovering worlds around distant stars, they found many planets that didn’t orbit their host stars on a flat plane. This raised the question of whether our pancakelike solar system is truly a rarity.
Copernicus’ planetary system, which is 40 light-years away from Earth, is of particular interest given how well studied and complex it is: Five exoplanets orbit a main-sequence star (the most common category of star) in a binary pair with a red dwarf star. In fact, Janssen was the first ‘super-Earth’ discovered around a main-sequence star. While Janssen has a similar density to Earth and is likely rocky, it’s about eight times as massive and twice as wide.
Upon its discovery and confirmation, Janssen became the first known example of an ultra-short-period planet. Janssen’s orbit has a minimum radius of roughly 2 million kilometers. (For comparison, Mercury’s is 46 million kilometers, and Earth’s is around 147 million.) Janssen’s orbit is so snug around Copernicus that at first some astronomers doubted its existence.
Determining Janssen’s path around Copernicus could reveal much about the planet’s history, but making such measurements is incredibly hard. Astronomers have studied Janssen by measuring the dip in Copernicus’ brightness every time the planet comes between the star and Earth.
That method doesn’t tell you what direction the planet is moving in. To find that out, astronomers take advantage of the same Doppler effect used in speeding cameras. When a light source is moving toward you, the wavelength of the light you see is shorter (and therefore bluer). When it’s moving away, the frequency is shifted wider, and the light is redder.
As Copernicus rotates, half of the star is twirling toward us, and the other half is moving away. That means half the star is a bit bluer, and the other half is slightly redder (and the space in the middle is unshifted). So astronomers can track Janssen’s orbit by measuring when it’s blocking light from the redder side, the bluer side and the unaltered midsection.
The resulting difference in the starlight, however, is almost immeasurably small. Teams had tried before but couldn’t accurately determine the planet’s orbital path. The breakthrough in the new research came from the EXtreme PREcision Spectrometer (EXPRES) at the Lowell Observatory’s Lowell Discovery Telescope in Arizona. True to its name, the spectrometer offered the precision needed to notice the light’s tiny red and blue shifts.
The EXPRES measurements revealed that Janssen’s orbit is roughly aligned with Copernicus’ equator, a path that makes Janssen unique among its siblings.
Previous research suggests that the nearby orbit of the red dwarf resulted in the misalignment of the planets relative to Copernicus. In the new study, the researchers propose that interactions between the heavenly bodies shifted Janssen toward its hellish present-day location. As Janssen approached Copernicus, the star’s gravity became increasingly dominant. Because Copernicus is spinning, the centrifugal force caused its midsection to bulge outward slightly and its top and bottom to flatten. That asymmetry affected the gravity felt by Janssen, pulling the planet into alignment with the star’s thicker equator.
With Janssen’s history illuminated, Zhao and her colleagues now plan to study other planetary systems. “We’re hoping to find planetary systems similar to ours,” she says, “and to better understand the systems that we do know about.”
Zhao co-authored the new paper with Vedad Kunovac and Joe Llama of the Lowell Observatory; John Brewer of San Francisco State University; Sarah Millholland of the Massachusetts Institute of Technology; Christina Hedges of the University of Maryland and NASA’s Goddard Space Flight Center; and Andrew Szymkowiak, Rachael Roettenbacher, Samuel Cabot, Sam Weiss and Debra Fischer of Yale University.
ABOUT THE FLATIRON INSTITUTE
The Flatiron Institute is the research division of the Simons Foundation. The institute’s mission is to advance scientific research through computational methods, including data analysis, theory, modeling and simulation. The institute’s Center for Computational Astrophysics creates new computational frameworks that allow scientists to analyze big astronomical datasets and to understand complex, multi-scale physics in a cosmological context.
Measured Spin-Orbit Alignment of Ultra-Short Period Super-Earth 55 Cancri e
Lily L. Zhao, Vedad Kunovac, John M. Brewer, Joe Llama, Sarah C. Millholland, Christina Hedges, Andrew E. Szymkowiak, Rachael M. Roettenbacher, Samuel H. C. Cabot, Sam A. Weiss, Debra A. Fischer
A planet’s orbital alignment places important constraints on how a planet formed and consequently evolved. The dominant formation pathway of ultra-short period planets (P<1 day) is particularly mysterious as such planets most likely formed further out, and it is not well understood what drove their migration inwards to their current positions. Measuring the orbital alignment is difficult for smaller super-Earth/sub-Neptune planets, which give rise to smaller amplitude signals. Here we present radial velocities across two transits of 55 Cancri e, an ultra-short period Super-Earth, observed with the Extreme Precision Spectrograph (EXPRES). Using the classical Rossiter-McLaughlin (RM) method, we measure 55 Cnc e’s sky-projected stellar spin-orbit alignment (i.e., the projected angle between the planet’s orbital axis and its host star’s spin axis) to be λ=10+17−20∘ with an unprojected angle of ψ=23+14−12∘. The best-fit RM model to the EXPRES data has a radial velocity semi-amplitude of just 0.41+0.09−0.10ms−1. The spin-orbit alignment of 55 Cnc e favors dynamically gentle migration theories for ultra-short period planets, namely tidal dissipation through low-eccentricity planet-planet interactions and/or planetary obliquity tides.
Comments: 12 pages, 4 figures, published in Nature Astronomy
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2212.03953 [astro-ph.EP] (or arXiv:2212.03953v1 [astro-ph.EP] for this version)
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From: Lily Zhao
[v1] Wed, 7 Dec 2022 20:55:59 UTC (4,170 KB)