Discovery of a Long Thermonuclear X-Ray Burst from the Ultracompact Binary 4U 1850–087

• Published in: The Astrophysical journal Vol. 969; no. 1; pp. 15 - 21
• Main Authors: Lu, Yongqi, Li, Zhaosheng, Yu, Wenhui, Pan, Yuanyue, Falanga, Maurizio
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.07.2024; IOP Publishing
• Subjects: Accretion; Accretion disks; Blackbody; Electron energy; Emission lines; Emission spectra; Emissions; Fluence; Helium; Line spectra; Low-mass x-ray binary stars; Neutron stars; X-ray bursters; X-ray bursts; X-rays
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad4d86

Abstract We report the detection of a long X-ray burst from the ultracompact binary 4U 1850–087. The type I X-ray burst was observed on MJD 60171.65 by the Monitor of All-sky X-ray Image and Neutron Star Interior Composition Explorer (NICER). We analyze the NICER data between MJD 60095.19 and 60177.43, which includes the observation covering parts of the long X-ray burst decay phase, i.e., 0.15–3.8 hr after the trigger. The persistent spectra are well described by a multicolor disk blackbody, with an inner temperature of ∼0.5 keV, a thermally Comptonized continuum, an asymptotic power-law photon index of Γ ∼ 2.2, and an electron temperature of kT e ∼ 20–30 keV. The mean persistent flux was around 3.8 × 10 −10 erg cm −2 s −1 , corresponding to a local mass accretion rate of ∼ 1 % m ̇ Edd . Part of the time-resolved burst spectra show a clear deviation from the blackbody model, which can be improved by considering the enhanced persistent emission due to the Poynting–Robertson drag or the reflected disk emission illuminated by the burst. From the burst flux during the cooling phase, we estimate the burst duration, τ ≈ 0.78 hr, the burst fluence, E b ≈ 4.1 × 10 41 erg, and the ignition column depth, y ign ≈ 3.5 × 10 10 g cm −2 . These long X-ray burst parameters from 4U 1850–087 suggest a regime of unstable burning of a thick, pure helium layer slowly accreted from a helium donor star. Moreover, we identify 7 σ significant ∼1 keV emission lines in the burst spectra, which may originate from the surrounding accretion disk.