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Ultracool Dwarf Binary Stars Break Records
Maunakea, Hawaiʻi – Northwestern University and the University of California San Diego (UC San Diego) astrophysicists using W. M. Keck Observatory on Maunakea, Hawaiʻi Island have discovered the tightest ultracool dwarf binary system ever observed.
The two stars are so close that it takes them less than one Earth day to revolve around each other; each star’s “year” lasts just 17 hours.
The newly discovered system, named LP 413-53AB, is composed of a pair of ultracool dwarfs, a class of very low-mass stars that are so cool that they emit their light primarily in the infrared, making them completely invisible to the human eye. They are nonetheless one of the most common types of stars in the universe.
Previously, astronomers had only detected three short-period ultracool dwarf binary systems, all of which are relatively young — up to 40 million years old. LP 413-53AB is estimated to be billions of years old — similar in age to our Sun — but has an orbital period that is about four times shorter than all the ultracool dwarf binaries discovered so far.
The study is published in The Astrophysical Journal Letters.
“It’s exciting to discover such an extreme system,” said Chih-Chun “Dino” Hsu, a Northwestern astrophysicist who led the study. “In principle, we knew these systems should exist, but no such systems had been identified yet.”
Hsu is a postdoctoral researcher in physics and astronomy at Northwestern’s Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). He began this study while a Ph.D. student at UC San Diego, where he was advised by Professor Adam Burgasser.
The team first discovered the strange binary system while exploring archival data. Hsu developed an algorithm that can model a star based on its spectral data. By analyzing the spectrum of light emitted from a star, astrophysicists can determine the star’s chemical composition, temperature, gravity, and rotation. This analysis also shows the star’s motion as it moves toward and away from the observer, known as radial velocity.
When examining the spectral data of LP 413-53AB, Hsu noticed something strange. Early observations caught the system when the stars were roughly aligned and their spectral lines overlapped, leading Hsu to believe it was just one star. But as the stars moved in their orbit, the spectral lines shifted in opposite directions, splitting into pairs in later spectral data. Hsu realized there were actually two stars locked into an incredibly tight binary.
Using Keck Observatory’s Near-Infrared Spectrograph (NIRSPEC), Hsu decided to observe the phenomenon for himself. On March 13, 2022, the team turned the Keck II telescope toward the constellation Taurus, where the binary system is located, and observed it for two hours. Then, they followed up with more observations in July, October, and December in 2022 as well as January 2023.
“When we were making this measurement, we could see things changing over a couple of minutes of observation,” Burgasser said. “Most binaries we follow have orbit periods of years. So, you get a measurement every few months. Then, after a while, you can piece together the puzzle. With this system, we could see the spectral lines moving apart in real time. It’s amazing to see something happen in the universe on a human time scale.”
The observations confirmed what Hsu’s model predicted. The distance between the two stars is about 1% of the distance between the Earth and the Sun.
“This is remarkable, because when they were young, something like 1 million years old, these stars would have been nearly on top of each other,” said Burgasser.
Illustration of the oldest known pair of ultracool dwarf stars that orbit each other so closely, they take less than one Earth day to revolve around each other. Credit: Adam Burgasser/UC San Diego
The team speculates that the stars either migrated toward each other as they evolved, or they could have come together after the ejection of a third — now lost — stellar member. More observations are needed to test these ideas.
Hsu also said that by studying similar star systems researchers can learn more about potentially habitable planets beyond Earth. Ultracool dwarfs are much fainter and dimmer than the Sun, so any worlds with liquid water on their surfaces — a crucial ingredient to form and sustain life — would need to be much closer to the star. However, for LP 413-53AB, the habitable zone distance happens to be very close to the size of the stellar orbit, making it likely impossible to form habitable planets in this system.
“These ultracool dwarfs are neighbors of our Sun,” Hsu said. “To identify potentially habitable hosts, it’s helpful to start with our nearby neighbors. But if close binaries are common among ultracool dwarfs, there may be few habitable worlds to be found.”
To fully explore these scenarios, Hsu, Burgasser, and their collaborators hope to pinpoint more short-period ultracool dwarf binary systems to create a full data sample. New observational data could help strengthen theoretical models for binary-star formation and evolution. Until now, however, finding ultracool binary stars has remained a rare feat.
“These systems are rare,” said co-author Chris Theissen, a Chancellor’s Postdoctoral Fellow at UC San Diego. “But we don’t know whether they are rare because they rarely exist or because we just don’t find them. That’s an open-ended question. Now we have one data point that we can start building on. This data had been sitting in the archive for a long time. Dino’s tool will enable us to look for more binaries like this.”
ABOUT NIRSPEC
The Near-Infrared Spectrograph (NIRSPEC) is a unique, cross-dispersed echelle spectrograph that captures spectra of objects over a large range of infrared wavelengths at high spectral resolution. Built at the UCLA Infrared Laboratory by a team led by Prof. Ian McLean, the instrument is used for radial velocity studies of cool stars, abundance measurements of stars and their environs, planetary science, and many other scientific programs. A second mode provides low spectral resolution but high sensitivity and is popular for studies of distant galaxies and very cool low-mass stars. NIRSPEC can also be used with Keck II’s adaptive optics (AO)system to combine the powers of the high spatial resolution of AO with the high spectral resolution of NIRSPEC. Support for this project was provided by the Heising-Simons Foundation.
ABOUT W. M. KECK OBSERVATORY
The W. M. Keck Observatory telescopes are among the most scientifically productive on Earth. The two 10-meter optical/infrared telescopes atop Maunakea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometers, and world-leading laser guide star adaptive optics systems. Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c) 3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
