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Astronomers Discover Variability in the Seven Sisters of the Pleiades Cluster

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For Immediate Release
25 August 2017


Dr. Daniel Huber
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Dr. Tim White
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Pleiades star cluster image from Kepler Space Telescope

The Pleiades star cluster, as ssen by the Kepler Space Telescope

This image from NASA's Kepler spacecraft shows members of the Pleaides star cluster taken during Campaign 4 of the K2 Mission. The cluster stretches across two of the 42 charge-coupled devices (CCDs) that make up Kepler's 95 megapixel camera. The brightest stars in the cluster - Alcyone, Atlas, Electra, Maia, Merope, Taygeta, and Pleione - are visible to the naked eye. Kepler was not designed to look at stars this bright; they cause the camera to saturate, leading to long spikes and other artifacts in the image. Despite this serious image degradation, a new technique has allowed astronomers to carefully measure changes in brightness of these bright stars as the Kepler telescope observed them for almost three months.
Image credit: NASA/ Aarhus University / T. White

High-resolution TIFF

The brightest members of the Pleiades cluster form a spectacular group of naked-eye stars that have played a central role in cultures around the world for millennia. Native Hawaiians used the Makaliʻi to mark the begining of the new year and the begining of "tax collecting season", while the "Seven Sisters" feature prominently in ancient Greek mythology. But not everything is known about these famous stars.

Now, an international team of astronomers, including Daniel Huber from the University of Hawaiʻi Institute for Astronomy, used the Kepler Space Telescope to perform the most detailed study to date of their variability - with some interesting new discoveries.

The study revealed that six of the seven stars are slowly-pulsating "B" stars, a class of variable star in which the star's brightness changes with day-long periods. The seventh star, Maia, is different: it varies with a regular period of 10 days. Follow-up observations using ground-based telescopes demonstrated that the variability is due to large chemical spot on the surface of the star, which comes in and out of view as the star rotates with a ten day period.

"Sixty years ago, astronomers had thought they could see variability in Maia with periods of a few hours and suggested this was the first of a whole new class of variable stars they called 'Maia Variables'," says lead author Dr Tim White from Aarhus University in Denmark, "but our new observations show that Maia is not itself a Maia Variable!"

The study was made possible through a new algorithm to enhance observations from the Kepler Space Telescope, now in its extended K2 Mission. Because Kepler was designed to look at thousands of faint stars at a time, stars like those in the Pleiades are too bright to observe with conventional methods. Aiming a beam of light from a bright star at a point on a camera detector will cause the central pixels of the star's image to be saturated, which makes it impossible to accurately measure the total brightness of the star. This is the same issue that makes everyday digital cameras unable to capture both faint and bright objects in the same exposure.

"The solution to observing bright stars with Kepler/K2 turned out to be rather simple. We're chiefly concerned about relative, rather than absolute, changes in brightness. We can just measure these changes from nearby unsaturated pixels, and ignore the saturated areas altogether," White explains.

But changes in the satellite's motion and slight imperfections in the detector can still hide the signal of stellar variability. To overcome this, the authors developed a new technique to weight the contribution of each pixel to find the right balance where instrumental effects are cancelled out, revealing the true stellar variability.

The Pleiades study marks only the beginning of investigating bright stars with Kepler/K2. "Naked-eye stars are benchmarks for solving many key problems in modern astrophysics," says Huber, co-author and Principal Investigator of a NASA-funded program to study bright stars with Kepler/K2. "By combining the pulsation frequencies detected by Kepler with complementary observations from the ground, for example using telescopes here on Maunakea, we will be able to study the structure and evolution of Pleiades members and other bright stars in unprecedented detail".

No signs of exoplanet transits were detected in this study, but the authors show that their new algorithm can attain the precision that will be needed for Kepler and future space telescopes such as the Transiting Exoplanet Survey Satellite (TESS) to detect planets transiting stars as bright as our neighboring star Alpha Centauri.

The results are published in the August 11th issue of the Monthly Notices of the Royal Astronomical Society, and can be found online at

The Pleiades star cluster is a beautiful and familiar sight, as seen in this image from the second Palomar Observatory Sky Survey. NASA’s Kepler space telescope was designed to look at faint stars, so images taken of the Pleiades show long spikes due to the camera becoming saturated by the brightest stars. Despite the image degradation, the continuous observations by Kepler over a period of almost three months have allowed astronomers to find fluctuations in the brightness of each star.
Credit: NASA / ESA / AURA / Caltech / Aarhus University / T. White

Plot of variability of Pleiades stars

Variability in Pleiades stars

The unique brightness fluctuations of each star reveal clues about their physical properties such as their size and rotation rate. Most of the bright stars in the Pleaides are a type of variable star called Slowly-Pulsating B stars, but Maia shows evidence of a large chemical spot on that crosses across its surface as the star rotates with a 10 day period.
Image credit: Aarhus University / T. White

High-resolution TIFF

Founded in 1967, the Institute for Astronomy at the University of Hawaii at Manoa conducts research into galaxies, cosmology, stars, planets, and the sun. Its faculty and staff are also involved in astronomy education, deep space missions, and in the development and management of the observatories on Haleakalā and Maunakea. The Institute operates facilities on the islands of Oahu, Maui, and Hawaii.