| Summary: | We present a spectral analysis of NuSTAR and NICER observations of the luminous, persistently accreting
neutron star (NS) low-mass X-ray binary Cygnus X-2. The data were divided into different branches that the
source traces out on the Z-track of the X-ray color–color diagram; namely, the horizontal branch, the normal
branch, and the vertex between the two. The X-ray continuum spectrum was modeled in two different ways that
produced comparable quality fits. The spectra showed clear evidence of a reflection component in the form of a
broadened Fe K line, as well as a lower-energy emission feature near 1 keV likely due to an ionized plasma located
far from the innermost accretion disk. We account for the reflection spectrum with two independent models
(RELXILLNS and RDBLUR*
RFXCONV). The inferred inclination is in agreement with earlier estimates from optical
observations of ellipsoidal lightcurve modeling (RELXILLNS: i = 67° ± 4°; RDBLUR*
RFXCONV: i = 60° ± 10°).
The inner disk radius remains close to the NS (Rin 1.15 RISCO) regardless of the source position along the
Z-track or how the 1 keV feature is modeled. Given the optically determined NS mass of 1.71 ± 0.21 Me, this
corresponds to a conservative upper limit of Rin 19.5 km for M = 1.92 Me or Rin 15.3 km for M = 1.5 Me. We
compare these radius constraints to those obtained from NS gravitational wave merger events and recent NICER
pulsar lightcurve modeling measurements.
|
|---|