The evolving radio jet from the neutron star X-ray binary 4U 1820−30. Issue 1 (30th July 2021)

• Record Type: Journal Article
• Authors: Russell, T D; Degenaar, N; den Eijnden, J van; Del Santo, M; Segreto, A; Altamirano, D; Beri, A; Díaz Trigo, M; Miller-Jones, J C A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 508:Issue 1(2021)
• Page Start: L6
• Page End: L11
• Publication Date: 2021-07-30
• Subjects: accretion, accretion discs -- stars: neutron -- radio continuum: transients -- X-rays: binaries; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slab087
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: The persistently bright ultracompact neutron star low-mass X-ray binary 4U 1820−30 displays an ∼170 d accretion cycle, evolving between phases of high and low X-ray modes, where the 3–10 keV X-ray flux changes by a factor of up to ≈8. The source is generally in a soft X-ray spectral state, but may transition to a harder state in the low X-ray mode. Here, we present new and archival radio observations of 4U 1820−30 during its high and low X-ray modes. For radio observations taken within a low mode, we observed a flat radio spectrum consistent with 4U 1820−30 launching a compact radio jet. However, during the high X-ray modes the compact jet was quenched and the radio spectrum was steep, consistent with optically thin synchrotron emission. The jet emission appeared to transition at an X-ray luminosity of $L_{\rm X (3-10\, keV)} \sim 3.5 \times 10^{37} (D/\rm {7.6\, kpc})^{2}$ erg s −1 . We also find that the low-state radio spectrum appeared consistent regardless of X-ray hardness, implying a connection between jet quenching and mass accretion rate in 4U 1820−30, possibly related to the properties of the inner accretion disc or boundary layer.