Doppler imaging of the helium-variable star a Cen

TL;DR

This study uses Doppler imaging and spectral analysis to map surface element abundances of the helium-variable star a Cen, revealing distinct hemispheric differences and identifying it as a helium-3 star with magnetic features.

Contribution

It provides detailed surface abundance maps of a Cen, confirming helium hemispheric variation and discovering helium-3 enrichment, establishing it as a magnetic helium-3 star.

Findings

Helium-rich and helium-poor hemispheres confirmed with over two orders of magnitude difference.

Helium-3 is highly abundant in the helium-poor hemisphere, a novel discovery.

Metal concentrations correlate with magnetic field features and are unevenly distributed.

Abstract

The helium-peculiar star a Cen exhibits line profile variations of elements such as iron, nitrogen and oxygen in addition to its well-known extreme helium variability. New high S/N, high-resolution spectra are used to perform a quantitative measurement of the abundances of the star and determine the relation of the concentrations of the heavier elements on the surface of the star to the helium concentration and the magnetic field orientation. Doppler images have been created using programs described in earlier papers by Rice and others. An alternative surface abundance mapping code has been used to model the helium line variations after our Doppler imaging of certain individual helium lines produced mediocre results. We confirm the long-known existence of helium-rich and helium-poor hemispheres on a Cen and we measure a difference of more than two orders of magnitude in helium abundance from one side of the star to the other. Helium is overabundant by a factor of about 5 over much of the helium-rich hemisphere. Of particular note is our discovery that the helium-poor hemisphere has a very high abundance of helium-3, approximately equal to the helium-4 abundance. a Cen is therefore a new member of the small group of helium-3 stars and the first well-established magnetic member of the class. For the three metals investigated here, there are two strong concentrations of abundance near the equator consistent with the positive magnetic maximum and two somewhat weaker concentrations of abundance where the helium concentration is centered and roughly where the negative peak of the magnetic field would be found. Another strong concentration is found near the equator and this is not explainable in terms of any simple symmetry with the helium abundance or the apparent magnetic field main polar locations.