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Giant Fluffy Planet Orbiting A Cool Red Dwarf Star

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Ultra Fluffy Gas Giant Planet Orbiting A Red Dwarf Star

Artist’s impression of an ultra-fluffy gas giant planet orbiting a red dwarf star. A gas giant exoplanet [right] Detected at a marshmallow density in orbit around a cool red dwarf star [left] By the NASA-funded NEID radial velocity instrument on the 3.5-metre WIYN Telescope at Kitt Peak National Observatory, a program of NSF’s NOIRLab. The planet, designated TOI-3757 b, is the fluffiest gas giant planet ever discovered around such a star. Credits: NOIRLab/NSF/AURA/J. da Silva/Space Engine/M. the time

The Kitt Peak National Observatory telescope helps determine:[{” attribute=””>Jupiter-like Planet is the lowest-density gas giant ever detected around a red dwarf.

A gas giant

Using the WIYN 3.5-meter Telescope at Kitt Peak National Observatory in Arizona, astronomers have observed an unusual Jupiter-like planet in orbit around a cool red dwarf star. Located in the constellation of Auriga the Charioteer around 580 light-years from Earth, this planet, identified as TOI-3757 b, is the lowest-density planet ever detected around a red dwarf star and is estimated to have an average density akin to that of a marshmallow.

Red dwarf stars are the smallest and dimmest members of so-called main-sequence stars — stars that convert hydrogen into helium in their cores at a steady rate. Although they are “cool” compared to stars like our Sun, red dwarf stars can be extremely active and erupt with powerful flares. This can strip orbiting planets of their atmospheres, making this star system a seemingly inhospitable location to form such a gossamer planet.

“Giant planets around red dwarf stars were traditionally thought to be difficult to form,” says Shubham Kanodia, a researcher in the Carnegie Institute for Science’s Earth and Planets Laboratory. Astronomical DiaryI. “So far this has only been looked at with small samples from Doppler surveys, which typically find giant planets farther away from these red dwarf stars. Until now, we didn’t have a large enough planet sample to solidly locate nearby gas planets.”

There are still unexplained mysteries surrounding TOI-3757 b, the biggest of which is how a gas giant planet could form around a red dwarf star and especially such a low density planet. But Kanodia’s team thinks they can find a solution to this mystery.

WIYN 3.5 meter Telescope

The Wisconsin-Indiana-Yale-NOIRLab (WIYN) 3.5-meter Telescope appears to peer into the Milky Way as it floats over the horizon from the base of Kitt Peak National Observatory (KPNO), a program of NSF’s NOIRLab. A reddish glow of air, a natural phenomenon, also colors the horizon. KPNO is located in the Arizona-Sonoran Desert in the Tohono O’odham Nation, and this sharp view of part of the galactic plane of the Milky Way shows the favorable conditions in this environment necessary to view faint celestial bodies. These conditions, which include low levels of light pollution, a sky darker than magnitude 20, and dry atmospheric conditions, have allowed researchers at the WIYN Consortium to observe galaxies, nebulae and exoplanets and many other astronomical targets. The WIYN 3.5-metre Telescope and its sister telescope, the WIYN 0.9-metre Telescope. Credits: KPNO/NOIRLab/NSF/AURA/R. sparks

They suggest that the extra-low density of TOI-3757 b may be the result of two factors. The first relates to the planet’s rocky core; The gas giants are thought to have started as rocky cores about ten times the mass of the Earth, at which point they rapidly pull in large amounts of neighboring gas to form the gas giants we see today. TOI-3757b’s star has lower heavy element abundances compared to other M-dwarfs with gas giants, and this may have caused the rocky core to form more slowly, delaying the onset of gas accumulation and thus affecting the overall density of the planet.

The second factor may be the orbit of the planet, which is temporarily thought to be slightly elliptical. There are times when it is closer to its star than at other times, causing significant overheating that can cause the planet’s atmosphere to swell.

NASA’s Transit Exoplanet Research Satellite ([{” attribute=””>TESS) initially spotted the planet. Kanodia’s team then made follow-up observations using ground-based instruments, including NEID and NESSI (NN-EXPLORE Exoplanet Stellar Speckle Imager), both housed at the WIYN 3.5-meter Telescope; the Habitable-zone Planet Finder (HPF) on the Hobby-Eberly Telescope; and the Red Buttes Observatory (RBO) in Wyoming.

TESS surveyed the crossing of this planet TOI-3757 b in front of its star, which allowed astronomers to calculate the planet’s diameter to be about 150,000 kilometers (100,000 miles) or about just slightly larger than that of Jupiter. The planet finishes one complete orbit around its host star in just 3.5 days, 25 times less than the closest planet in our Solar System — Mercury — which takes about 88 days to do so.

The astronomers then used NEID and HPF to measure the star’s apparent motion along the line of sight, also known as its radial velocity. These measurements provided the planet’s mass, which was calculated to be about one-quarter that of Jupiter, or about 85 times the mass of the Earth. Knowing the size and the mass allowed Kanodia’s team to calculate TOI-3757 b’s average density as being 0.27 grams per cubic centimeter (about 17 grams per cubic feet), which would make it less than half the density of

“Potential future observations of the atmosphere of this planet using NASA’s new

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