VLA 9 GHz image of GX 1+4. The black cross shows the most accurate position of GX 1+4, from 2MASS (nearinfrared), which is accurate to 0.1 arcsec. The half-power contour of the synthesized beam is shown in the bottom left corner. Credit: Van den Eijnden et al., 2017.
Using the Karl G. Jansky Very Large Array (VLA), an international group has detected radio emissions from the accreting X-ray pulsar and symbiotic X-ray binary system designated GX 1+4. It is the first discovery of radio emissions from a symbiotic X-ray binary and the first indication of a jet from an accreting X-ray pulsar with a strong magnetic field.
Discovered in 1970, GX 1+4 is an accreting X-ray pulsar some 14,000 light years away with a relatively long rotation period of about 120 seconds. It accretes matter from its companion M6III-type red giant, V2116 Oph, which is circling the pulsar every 1,161 days. Therefore, the system was classified as a symbiotic X-ray binary (SyXRB) as it consists of a neutron star low-mass X-ray binary accreting from stellar wind of a M-type giant donor.
GX 1+4’s long-term spin has been a subject of interest for astronomers observing this system for many years. More recently, a team of astronomers led by Jakob van den Eijnden of the University of Amsterdam, Netherlands, has used the VLA observatory in New Mexico to conduct radio observations of GX 1+4 as part of larger program studying persistent low-mass X-ray binaries. As a result, they detected radio emissions from this pulsar.
VLA allowed the astronomers to detect radio emission at 9.0 GHz with a flux density of about 105.3 µJy. However, the origin of this emission remains uncertain and the team takes into account several hypothesis that could explain this activity. The scientists argue that the detected emission could be most likely caused by one of the 3 mechanisms: shocks in the interaction of the accretion flow with the magnetosphere, a synchrotron-emitting jet, or a propeller-driven outflow. They exclude the possibility that it is due the stellar wind from the red giant companion.
“We might observe radio emission from shocks as the accretion flow interacts with the magnetosphere. (…) Such shocks are compatible with the properties of GX 1+4 if the magnetic field is indeed as high as about 1,014 G,” the paper reads. The researchers added that the shock scenario could be invalid if GX 1+4 has weaker magnetic field than estimated. When it comes to the second possibility, the radio emission could also be synchrotron emission from a collimated jet. The authors noted that the luminosity of GX 1+4 is in agreement with the radio and X-ray luminosities in a large sample of low-magnetic field accreting neutron stars, where radio emission originates from such jets. They added that if this hypothesis is true, it would show that strong magnetic fields (above one trillion G) do not necessarily suppress jet formation.
Finally, the researchers suggest that the radio emission could be explained by a magnetic propeller. They emphasized that such an outflow has been inferred from previous X-ray observations in two other high magnetic field X-ray pulsars. All in all, more observations of GX 1+4 are needed, especially simultaneously at radio and X-ray wavelengths, in order to choose the most plausible theory and to better understand the nature of its radio emission.
https://phys.org/news/2017-11-astronomers-radio-emission-symbiotic-x-ray.htmljCp
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