X-ray emission from an FU Ori star in early outburst: HBC 722

TL;DR

This study presents the first X-ray observations of the FU Ori star HBC 722 during early outburst, revealing high X-ray luminosity and gas properties indicative of strong winds or accretion activity.

Contribution

It provides the first X-ray characterization of HBC 722 during early outburst, highlighting the presence of dust-free gas and potential wind or accretion phenomena.

Findings

Detected X-ray luminosity of ~4E30 erg/s from HBC 722

Gas column density exceeds optical extinction expectations

Evidence suggests presence of dust-free gas, winds, or accretion columns

Abstract

Aims: We conducted the first X-ray observations of the newly erupting FU Ori-type outburst in HBC 722 (V2493 Cyg) with the aim to characterize its X-ray behavior and near-stellar environment during early outburst. Methods: We used data from the XMM-Newton and Chandra X-ray observatories to measure X-ray source temperatures and luminosities as well as the gas column densities along the line of sight toward the source. Results: We report a Chandra X-ray detection of HBC 722 with an X-ray luminosity of LX ~ 4E30 erg s-1. The gas column density exceeds values expected from optical extinction and standard gas-to-dust ratios. We conclude that dust-free gas masses are present around the star, such as strong winds launched from the inner disk, or massive accretion columns. A tentative detection obtained by XMM-Newton two years earlier after an initial optical peak revealed a fainter X-ray source with only weak absorption.