What we learn from the X-ray grating spectra of Nova SMC 2016

TL;DR

This study analyzes X-ray spectra of Nova SMC 2016, revealing details about the white dwarf's atmosphere, composition, and dynamics during its luminous supersoft phase, with implications for understanding nova evolution and white dwarf properties.

Contribution

First detailed X-ray spectral analysis of Nova SMC 2016, providing insights into the white dwarf atmosphere, composition, and outburst dynamics, and suggesting a possible oxygen-neon white dwarf classification.

Findings

Detected blue-shifted absorption features indicating high-velocity outflows.

Observed bolometric luminosity exceeding Eddington limit for months.

Identified temperature evolution consistent with a massive white dwarf.

Abstract

Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between day 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera and the Low Energy Transmission Grating (LETG) on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon and sulfur on day 39, and oxygen, nitrogen and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blue-shifted, by about 1800 km/s on day 39 and up to 2100 km/s in the following observations. Spectral lines attributed to low ionization potential transitions in the interstellar medium are also observed. Assuming the distance of the Small Magellanic Cloud, the bolometric luminosity exceeded Eddington level for at least three months. A preliminary analysis with atmospheric models indicates effective temperature around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a 1.25 m(sol) WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show large, aperiodic ux variability, not associated with spectral variability. We detected red noise, but did not find periodic or quasi-periodic modulations.