EP Aquarii: a new picture of the circumstellar envelope

Abstract

Abstract New analyses of earlier ALMA observations of oxygen-rich AGB star EP Aquarii are presented, which complete a previously published
analysis and offer a different interpretation of the morpho-kinematics of the circumstellar envelope. The birth of the equatorial density enhancement (EDE) is shown to occur very close to the star where evidence for rotation has been obtained. Close to the star and where outflows have been observed: their interaction with the gas of the nascent EDE, is seen to play an important role in the development of the wind and the evolution of its radial velocity from 8-10 km s−1 on the polar symmetry axis to ~2 km s−1 at the equator. It implies a complex morpho-kinematics: making reliable interpretations with reasonable confidence is difficult. In particular, it weakens an earlier interpretation implying the presence of a white dwarf companion orbiting the star at an angular distance of ~0.4 arcsec from its centre. It proposes instead an interpretation in terms of a standard mass ejection associated with a shock wave leaving a void of emission in its wake. High Doppler velocity wings are seen to consist of two components, the upper velocity end of the global wind, reaching above ±12 km s−1 , and an effective line broadening, confined within 200 mas from the centre of the star, reaching above ± 20 km s−1 and interpreted as caused by the pattern of shock waves resulting from the interaction between stellar pulsation and convective cell granulation.