The outburst and nature of two young eruptive stars in the North America/Pelican Nebula Complex

TL;DR

This study investigates two young eruptive stars in the North America/Pelican Nebula, analyzing their outburst behaviors and spectral energy distributions to determine their classification and accretion properties.

Contribution

The paper provides detailed monitoring and analysis of two eruptive stars, challenging their classification as classical FUors and highlighting their unique outburst characteristics.

Findings

HBC 722's brightness increased monotonically over two months.

VSX J205126.1+440523 reached an unprecedented high amplitude.

Both objects do not fit the classic FUor profile.

Abstract

Context. In August 2010, the sudden optical brightening of two young stellar objects, located in the North America/Pelican Nebula Complex, was announced. Early observations indicated that these objects may belong to the FUor or EXor class of young eruptive stars. The eruptions of FUors and EXors are often explained by enhanced accretion of material from the circumstellar disk to the protostar. Aims. In order to determine the true nature of these two objects, we started an optical and near-infrared monitoring program, and complemented our data with archival observations and data from the literature. Methods. We plot and analyze pre-outburst and outburst spectral energy distributions (SEDs), multi-filter light curves, and color-color diagrams. Results. HBC 722 brightened monotonically in about two months, and the SED obtained during maximum brightness indicates the appearance of a hot, single-temperature blackbody. The current fading rate implies that the star will return to quiescence in about a year, questioning its classification as a bone fide FUor. The outburst of VSX J205126.1+440523 happened more gradually, but reached an unprecedentedly high amplitude. At 2.5 months after the peak, its light curves show a deep minimum, when the object was close to its pre-outburst optical brightness. Further monitoring indicates that it is still far from being quiescent. Conclusions. The shape of the light curves, the bolometric luminosities and accretion rates suggest that these objects do not fit into the classic FUor group. Although HBC 722 exhibit all spectral characteristics of a bona fide FUor, its luminosity and accretion rate is too low, and its timescale is too fast compared to classical FUors. VSX J205126.1+440523 seems to be an example where quick extinction changes modulate the light curve.