Universe Today
Red dwarf stars have proven to be a treasure trove for exoplanet hunters in recent years. In addition to multiple exoplanets candidates being detected around stars like TRAPPIST-1, Gliese 581, Gliese 667C, and Kepler 296, there was also the ESO's recent discovery of a planet orbiting within the habitable zone of our Sun's closest neighbor -
Proxima Centauri
.
And it seems the trend is likely to continue, with the latest discovery comes from a team of European scientists. Using data from the ESO's
High Accuracy Radial velocity Planet Searcher
(HARPS) and HARPS-N instruments, they detected an exoplanet candidate orbiting around GJ 536 - an M-class red dwarf star located about 32.7 light years (10.03 parsecs) from Earth.
According to their study, "
A super-Earth Orbiting the Nearby M-dwarf GJ 536
", this planet is a super-Earth - a class of exoplanet that has between more than one, but less than 15, times the mass of Earth. In this case, the planet boasts a minimum of 5.36 ± 0.69 Earth masses, has an orbital period of 8.7076 ± 0.0025 days, and orbits its sun at a distance of 0.06661 AU.
[caption id="attachment_130350" align="aligncenter" width="580"]
Artist's impression of a system of exoplanets orbiting a low mass, red dwarf star. Credit: NASA/JPL
[/caption]
The team was led by Dr. Alejandro Suárez Mascareño of the Instituto de Astrofísica de Canarias (IAC). The discovery of the planet was part of his thesis work, which was conducted under Dr Rafael Rebolo - who is also a member of the IAC, the Spanish National Research Council and a professor at the University of Laguna. And while the planet is not a potentially habitable world, it does present some interesting opportunities for exoplanet research.
As Dr. Mascareño shared with Universe Today via email:
The survey that found this planet was part of a joint effort between the IAC (Spain) and the
Geneva Observatory
(Switzerland). The data came from the HARPS and HARPS-N instruments, which are mounted on the ESO's 3.6 meter telescope at the
La Silla Observstory
in Chile and the 3.6 meter telescope at the
La Palma Observatory
in Spain. This was combined with photometric data from the
All Sky Automated Surve
y (ASAS), which has observatories in Chile and Maui.
The research team relied on radial velocity measurements from the star to discern the presence of the planet, as well as spectroscopic observations of the star that were taken over a 8.6 year period. For all this, they not only detected an exoplanet candidate with 5 times the mass of Earth, but also derived information on the star itself - which showed that it has a rotational period of about 44 days, and magnetic cycle that lasts less than three years.
[caption id="attachment_131374" align="aligncenter" width="580"]
Artist's depiction of the interior of a low-mass star, such as the one seen in an X-ray image from Chandra in the inset. Credit: NASA/CXC/M.Weiss
[/caption]
By comparison, our Sun has a rotational period of 25 days and
a magnetic cycle of 11 years
, which is characterized by changes in the levels of solar radiation it emits, the ejection of solar material and in the appearance of sunspots. In addition, a
recent study
from the the
Harvard Smithsonian Center for Astrophysics
(CfA) showed that Proxima Centauri has a stellar magnetic cycle that lasts for 7 years.
This detection is just the latest in a long line of exoplanets being discovered around low-mass, low-luminosity, M-class (red dwarf) stars. And looking ahead, the team hopes to continue surveying GJ 536 to see if there is a planetary system, which could include some Earth-like planets, and maybe even a few gas giants.
"For now we have detected only one planet, but we plan to continue monitoring the star to search for other companions at larger orbital separations," said Dr. Mascareño. "We estimate there is still room for other low-mass or even Neptune-mass planets at orbits from a hundred of days to a few years."
The research also included scientists from the Astronomical Observatory at the University of Geneva, the University of Grenoble, The Astrophysical and Planetological Insitute of Grenoble, Institute of Astrophysics and Space Sciences in Portugal, and the University of Porto, Portugal.
Further Reading: arXiv
