Spectral Analyses Of The Hottest White Dwarfs: Grids Of Spectral Energy Distributions For Extremely Hot, Compact Stars In The Framework Of The Virtual Observatory

TL;DR

This paper introduces a new grid of spectral energy distributions for extremely hot white dwarfs, utilizing the TMAP model and accessible via the Virtual Observatory, to aid in analyzing high-resolution X-ray observations.

Contribution

It presents a comprehensive grid of spectral energy distributions for hot white dwarfs, integrated into the Virtual Observatory framework for easier access and analysis.

Findings

New grid of SEDs for hot white dwarfs in the nova and supersoft X-ray source range.

Integration of the grid into the Virtual Observatory via TheoSSA.

Enhanced tools for analyzing high-resolution X-ray spectra.

Abstract

Present X-ray missions like Chandra and XMM-Newton provide high-resolution and high-S/N observations of extremely hot white dwarfs, e.g. burst spectra of novae. Their analysis requires adequate Non-LTE model atmospheres. The T\"ubingen Non-LTE Model-Atmosphere Package TMAP can calculate such model atmospheres and spectral energy distributions at a high level of sophistication. In the framework of the Virtual Observatory, the German Astrophysical Virtual Observatory (GAVO) offers TheoSSA, a Virtual Observatory (VO) service that provides easy access to theoretical SEDs. We present a new grid of SEDs, that is calculated in the parameter range of novae and supersoft X-ray sources.