Giant planet discovered

  124 light-years away from Earth, giant planet discovered 

Astronomers report the detection of a new Jupiter-like exoplanet using the High Accuracy Radial velocity Planet Searcher (HARPS). The newfound alien world orbits a nearby M-dwarf star designated GJ 2126. A nearby star has a new heavyweight companion, and it swings around on a path which is anything but neat. The world, labelled GJ 2126 b, traces a stretched orbit which pushes close to its star, then races far away again. Researchers identified a giant world 124 light years away that circles its star every 272.7 days on a highly stretched path, eccentricity equals 0.85. In addition, it has a minimum mass of about 1.3 Jupiter masses at roughly 0.71 astronomical units, about 66 million miles, from its star. These values come from 112 radial velocity measurements with the HARPS spectrograph. “This planet orbits a low-mass star and ranks among the most eccentric exoplanets discovered,” wrote Arbel Schorr from the School of Physics and Astronomy at Tel Aviv University (TAU) who led the study. 

The radial velocity (RV) method of detecting an exoplanet is based on the detection of variations in the velocity of the central star, due to the changing direction of the gravitational pull from an unseen exoplanet as it orbits the star. Thanks to this technique, more than 600 exoplanets have been detected so far. HARPS is a high-resolution visible-light echelle spectrograph installed at the European Southern Observatory (ESO) 3.6-m telescope in Chile. Thanks to its radial-velocity accuracy of about 1 m/s, it is one of the most successful planet finders in history. Most planets in our own neighbourhood move on nearly round routes, so an orbit this stretched stands out. High eccentricity often points to a chaotic past shaped by strong gravitational run-ins. A path like this can reshape a planet’s temperature and atmospheric behaviour across a single year. The extremes also make modeller's revisit how giant planets form and later get knocked around.

"We report the discovery of GJ 2126 b, a highly eccentric (e = 0.85) Jupiter-like planet orbiting its host star every 272.7 days. The planet was detected and characterized using 112 RV measurements from HARPS, provided by HARPS-RVBank," the researchers wrote. The team used HARPS which maintains about 1 meter per second velocity stability. The level of steadiness lets astronomers watch a star’s tiny wobble over many years. They mined the publicly curated HARPS-RVBank, which compiles 252,615 velocities for 5,239 stars observed before January 2022. Public datasets like this let independent teams test ideas and spot signals which earlier searches may have missed. With a semi-major axis of 0.71 AU and eccentricity of 0.85, periastron, the closest approach, sits near 0.11 AU, about 9.9 million miles. The farthest point stretches to roughly 1.31 AU, about 122 million miles. Those swings mean large changes in stellar heating across a single 272.7 day year. Timing, chemistry, and cloud formation likely shift dramatically between close pass and far turn.

The inclination of GJ 2126 b is unknown, its mass could be much greater and the possibility that this object may be a brown dwarf cannot be completely excluded. The host star, often listed as an M-dwarf of type M0V, is a cool, low-mass object with about 0.65 times the Sun’s mass and 0.73 times its radius. Its temperature sits near 4,159 kelvin and its metal content is high for a dwarf star. GJ 2126 is a high proper-motion star about 124 light years from Earth. Its brightness and proximity make follow-up work practical with existing instruments. Because the orbital tilt is unknown, the mass estimate is a lower limit. The team considered whether the companion might cross into brown dwarf territory if the orbit is nearly face-on. They argue that Gaia astrometry and the absence of long-term trends disfavor a very massive companion around this star. The paper reports a renormalized astrometric error near unity, a value not expected for a heavy hidden object. The researchers compared different ways to search for periodicity in uneven time series. They leaned on the Phase Distance Correlation periodogram, designed to handle non-sinusoidal signals like those from eccentric orbits. They also considered a known trap in velocity work, where two planets in a 2:1 resonance can masquerade as one eccentric planet. Their modelling rejected such alternatives for this dataset.

Astronomers underline that GJ 2126 b is one of the most eccentric exoplanets discovered around an M-dwarf. They added that the unique properties of GJ 2126 b place it in a relatively sparse region of the detected exoplanet population. Therefore, its further observations could help better understand planetary formation and evolution scenarios. Cool stars frequently show magnetic activity that adds noise to velocity data. Teams monitor spectral activity indicators to avoid mistaking star spots for planets and to validate true orbits. In this case, the auxiliary indicators did not line up with the 272.7 day signal. That mismatch supports a planetary cause rather than rotating surface features. When it comes to the host GJ 2126, it is a high proper motion star of spectral type M0V, with a radius of about 0.73 solar radii and a mass of around 0.65 solar masses. The star, which is estimated to be at a distance of approximately 124 light years away, has a metallicity at a level of 0.6 dex and its effective temperature is 4,159 K.

Their dataset spans about fifteen years around the critical phases of the orbit. The coverage anchored the fit and strengthened the case for a single object on an extreme path. Giant planets can acquire extreme eccentricities through planet-planet scattering after their birth in a gas disk. Numerical experiments show this process can drive e above 0.9 without invoking a distant stellar companion. As per these details, the system once hosted additional massive bodies that jostled each other until only one remained on a wild orbit. That would line up with the lack of a long-term drift in the present data. The planet’s radius is unknown because no transit has been seen in the available survey photometry. Without the tilt, the true mass remains uncertain, so further work aims to refine those values. Future velocity campaigns could detect subtle variations tied to mutual interactions, if any undiscovered companions exist. Continued astrometric monitoring may also tighten the mass constraints. Thermal measurements and reflected-light studies would be challenging, yet not out of the question for future facilities. The close approach near periastron may offer the best shot at characterization time. Long-baseline velocities will also test for secular changes which hint at additional bodies or tidal effects. A refined inclination would settle the mass question and finally close the door on the brown-dwarf scenario. Further observations of GJ 2126 b are required in order to determine its radius and to constrain its mass, which would shed more light regarding the composition of this exoplanet.