2022/03/03 by E. De la Fuente, M. A. Trinidad, Daniel Tafoya +2 · 1 citation
Physics and Astronomy · #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #Astro and Planetary Science #Physics #Collimated light #Nebula #Core (optical fiber) #Astronomy #Ionization #Astrophysics #Planetary nebula #Plasma #Stars #Ion #Nuclear physics #Optics #Laser
paper · pdf · doi:10.1093/pasj/psac020
openalex publication_date 2022/03/03 · openalex created_date 2022/03/05 · openalex updated_date 2026/08/05
Abstract We studied the central region of bipolar nebula M 2-9 using radio-continuum observations obtained from the Jansky Very Large Array (JVLA) and the Atacama Large Millimeter Array (ALMA) interferometers. This work presents new images at ∼43 GHz (∼7.0 mm) and ∼345 GHz (∼0.9 mm) with angular resolutions of ∼ 0′ ′.047 and 0′ ′.09, respectively. The continuum emission at ∼43 GHz shows an elongated jet-like structure perpendicular to the ∼345 GHz observation. We conclude that both emissions could correspond to tracing an isothermal collimated fast wind with constant expansion velocity and being driven by the circumstellar ring traced by ALMA. Although this configuration has been discussed within the scope of planetary nebulae models, there is a remarkable fact: the collimated fast wind shows morphological spatial variability. This supports the idea of a symbiotic binary system within the innermost part of M 2-9, which would be composed of a white dwarf and an AGB star. The latter could explain the mirror symmetry observed at larger scales due to their orbital motion.