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A Cosmic Jekyll and Hyde

  • A binary, or double, star system is acting in a very unusual way, according to Chandra data obtained over nearly a decade and a half.

  • Terzan 5 CX1 is located in a globular cluster about 19,000 light years from Earth and has shown behavior traits of two different types of objects.

  • Chandra data from 2003 show this system acted as a low-mass X-ray binary, with a neutron star pulling material from a star like the Sun.

  • Chandra and VLA data between 2009 and 2014 show the system changed into behaving like a millisecond pulsar, then in 2016 went back to acting like a low-mass X-ray binary.

A double star system has been flipping between two alter egos, according to observations with NASA's Chandra X-ray Observatory and the National Science Foundation's Karl F. Jansky Very Large Array (VLA). Using nearly a decade and a half worth of Chandra data, researchers noticed that a stellar duo behaved like one type of object before switching its identity, and then returning to its original state after a few years. This is a rare example of a star system changing its behavior in this way.

Astronomers found this volatile double, or binary, system in a dense collection of stars, the globular cluster Terzan 5, which is located about 19,000 light years from Earth in the Milky Way galaxy. This stellar duo, known as Terzan 5 CX1, has a neutron star (the extremely dense remnant left behind by a supernova explosion) in close orbit around a star similar to the Sun, but with less mass.

In this new image of Terzan 5 (right), low, medium and high-energy X-rays detected by Chandra are colored red, green and blue respectively. On the left, an image from the Hubble Space Telescope shows the same field of view in optical light. Terzan 5 CX1 is labeled as CX1 in the Chandra image.

In binary systems like Terzan 5 CX1, the heavier neutron star pulls material from the lower-mass companion into a surrounding disk. Astronomers can detect these so-called accretion disks by their bright X-ray light, and refer to these objects as "low-mass X-ray binaries."

Spinning material in the disk falls onto the surface of the neutron star, increasing its rotation rate. The neutron star can spin faster and faster until the roughly 10-mile-wide sphere, packed with more mass than the Sun, is rotating hundreds of times per second. Eventually, the transfer of matter slows down and the remaining material is swept away by the whirling magnetic field of the neutron star, which becomes a millisecond pulsar. Astronomers detect pulses of radio waves from these millisecond pulsars as the neutron star's beam of radio emission sweeps over the Earth during each rotation.

While scientists expect the complete evolution of a low-mass X-ray binary into a millisecond pulsar should happen over several billion years, there is a period of time when the system can switch rapidly between these two states. Chandra observations of Terzan 5 CX1 show that it was acting like a low-mass X-ray binary in 2003, because it was brighter in X-rays than any of the dozens of other sources in the globular cluster. This was a sign that the neutron star was likely accumulating matter.

Terzan 5 labeled
Terzan 5, Labeled (Credit: NASA/CXC/Univ. of Amsterdam/N.Degenaar, et al.)

In Chandra data taken from 2009 to 2014, Terzan 5 CX1 had become about ten times fainter in X-rays. Astronomers also detected it as a radio source with the VLA in 2012 and 2014. The amount of radio and X-ray emission and the corresponding spectra (the amount of emission at different wavelengths) agree with expectations for a millisecond pulsar. Although the radio data used did not allow a search for millisecond pulses, these results imply that Terzan 5 CX1 underwent a transformation into behaving like a millisecond pulsar and was blowing material outwards. By the time Chandra had observed Terzan 5 CX1 again in 2016, it had become brighter in X-rays and changed back to acting like a low-mass X-ray binary again.

To confirm this pattern of "Jekyll and Hyde" behavior, astronomers need to detect radio pulses while Terzan 5 CX1 is faint in X-rays. More radio and X-ray observations are planned to search for this behavior, along with sensitive searches for pulses in existing data. Only three confirmed examples of these identity-changing systems are known, with the first discovered in 2013 using Chandra and several other X-ray and radio telescopes.

The study of this binary was led by Arash Bahramian of the International Centre for Radio Astronomy Research (ICRAR), Australia and was published in the September 1st, 2018 issue of The Astrophysical Journal. A preprint is available here.

Two other recent studies have used Chandra observations of Terzan 5 to study how neutron stars in two different low-mass X-ray binaries recover after having had large amounts of material dumped on their surface by a companion star. Such studies are important for understanding the structure of a neutron star's outer layer, known as its crust.

In one of these studies, of the low-mass X-ray binary Swift J174805.3–244637 (T5 X-3 for short), material dumped onto the neutron star during an X-ray outburst detected by Chandra in 2012 heated up the star's crust. The crust of the neutron star then cooled down, taking about a hundred days to fall back to the temperature seen before the outburst. The rate of cooling agrees with a computer model for such a process.

In a separate Chandra study of a different low-mass X-ray binary in Terzan 5, IGR J17480–2446 (T5 X-2 for short) the neutron star was still cooling when its temperature was taken five and a half years after it was known to have an outburst. These results show this neutron star's crust ability to transfer, or conduct, heat may be lower than what astronomers have found in other cooling neutron stars in low-mass X-ray binaries. This difference in the ability to conduct heat may be related to T5 X-2 having a higher magnetic field compared to other cooling neutron stars, or being much younger than T5 X-3.

Both T5 X-3 and T5 X-2 are labeled in the image.

The work on the rapidly cooling neutron star, led by Nathalie Degenaar of the University of Amsterdam in the Netherlands, was published in the June 2015 issue of the Monthly Notices of the Royal Astronomical Society and a preprint is available here. The study of the slowly cooling neutron star, led by Laura Ootes, then of the University of Amsterdam, was published in the July 2019 issue of the Monthly Notices of the Royal Astronomical Society and a preprint is available here.

NASA's Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory's Chandra X-ray Center controls science and flight operations from Cambridge and Burlington, Massachusetts.

 

Fast Facts for Terzan 5:
Credit  X-ray: NASA/CXC/Univ. of Amsterdam/N.Degenaar, et al.; Optical: NASA, ESO/F.Ferraro
Release Date  February 20, 2020
Scale  Each panel is about 3.1 arcmin (17 light years) across.
Category  Normal Stars & Star Clusters
Coordinates (J2000)  RA 17h 48m 4.8s | Dec -24° 46´ 45"
Constellation  Sagittarius
Observation Date  17 observations from July 13, 2003 through July 20, 2014
Observation Time  171 hours 37 minutes (7 days 3 hours 37 minutes)
Obs. ID  3798, 10059, 12454, 13225, 13252, 13705, 13706, 14339, 14475-14479, 14625, 15615, 15750, 16638
Instrument  ACIS
References Bahramian, A. et al., 2018, ApJ, 864, 28; arXiv:1807.11589
Degenaar, N. et al., 2015, MNRAS, 451, 2071; arXiv:1505.01862
Ootes, L.S. et al., 2019, MNRAS, 487, 1447; arXiv:1805.00610
Color Code  X-ray: Red: 0.3-1.2 keV Green: 1.2-2.0 keV Blue: 2.0-6.0 keV
Optical
X-ray
Distance Estimate  About 19,000 light years
distance arrow
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