The extended molecular envelope of the asymptotic giant branch star π1 Gruis as seen by ALMA I. Large-scale kinematic structure and CO excitation properties
Abstract
The S-type asymptotic giant branch (AGB) star π1 Gruis has a known companion at a separation of ≈400 AU. The envelope structure, including an equatorial torus and a fast bipolar outflow, is rarely seen in the AGB phase and is particularly unexpected in such a wide binary system. Therefore a second, closer companion has been suggested, but the evidence is not conclusive. The new ALMA 12CO and 13CO J=3-2 data, together with previously published 12CO J=2-1 data from the Submillimeter Array (SMA), and the 12CO J=5-4 and J=9-8 lines observed with Herschel/Heterodyne Instrument for the Far-Infrared (HIFI), is modeled with the 3D non-LTE radiative transfer code SHAPEMOL. The data analysis clearly confirms the torus-bipolar structure. The 3D model of the CSE that satisfactorily reproduces the data consists of three kinematic components: a radially expanding torus with velocity slowly increasing from 8 to 13 km s-1 along the equator plane; a radially expanding component at the center with a constant velocity of 14 km s-1; and a fast, bipolar outflow with velocity proportionally increasing from 14 km s-1 at the base up to 100 km s-1 at the tip, following a linear radial dependence. The results are used to estimate an average mass-loss rate during the creation of the torus of 7.7×10-7 M yr-1. The total mass and linear momentum of the fast outflow are estimated at 7.3×10-4 M and 9.6×1037 g cm s-1, respectively. The momentum of the outflow is in excess (by a factor of about 20) of what could be generated by radiation pressure alone, in agreement with recent findings for more evolved sources. The best-fit model also suggests a 12CO/13CO abundance ratio of 50. Possible shaping scenarios for the gas envelope are discussed