Accretion-powered chromospheres in classical T Tauri stars

TL;DR

This study investigates the nature of chromospheric emission and veiling in classical T Tauri stars, revealing that accretion significantly enhances chromospheric activity beyond solar-like magnetic effects.

Contribution

It demonstrates that accretion-induced chromospheric emission contributes substantially to veiling, extending the understanding of stellar atmosphere modifications in young stars.

Findings

Veiling varies from negligible to over 10 times the stellar continuum.

Chromospheric emission is powered by accreting gas, not just magnetic activity.

Extended chromospheric regions fill in photospheric absorption lines.

Abstract

(Abridged) Optical spectra of classical T Tauri stars (cTTS) are rich in emission lines of low-excitation species that are composed of narrow and broad components, related to two regions with different kinematics, densities, and temperatures. The photospheric spectrum is often veiled by an excess continuous emission. This veiling is usually attributed to radiation from a heated region beneath the accretion shock. The aim of this research is to clarify the nature of the veiling, and whether the narrow chromospheric lines of Fe I and other metals represent a standard chromosphere of a late-type star, or are induced by mass accretion. From high-resolution spectroscopy of DR Tauri we found that the amount of veiling in this star varies from practically nothing to factors more than 10 times the stellar continuum intensity, and that the veiling is caused by both a non-photospheric continuum and chromospheric line emission filling in the photospheric absorption lines. This effect can be shown to exist in several other T Tauri stars. We conclude that enhanced chromospheric emission in cTTS is linked not only to solar-like magnetic activity, but is powered to a greater extent by the accreting gas. We suggest that the area of enhanced chromospheric emission is induced by mass accretion, which modifies the local structure of stellar atmosphere in an area that is more extended than the hot accretion spot. The narrow emission lines from this extended area are responsible for the extra component in the veiling through line-filling of photospheric absorption lines.