2022/01/25 by Tomek Kaminski, T. Kamiński, Helena Mazurek +5
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #Ejecta #Emission spectrum #Galaxy #Interstellar medium #Millimeter #Nova (rocket) #Nuclear physics #Optics #Physics #Plasma #Spectral line #Star formation #Stars #Submillimeter Array #Supernova #Thermonuclear fusion #Wavelength #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/202142737
published as A&A 659, A109 (2022) · comments welcome, submitted to A&A
arxiv created 2022/01/25 · openalex publication_date 2022/02/03 · arxiv updated 2022/03/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Detecting molecular line emission from classical nova remnants has the potential of revealing information on the composition of the ejecta, in particular, it can deliver accurate isotopic ratios in the matter processed by a thermonuclear runaway. We conducted searches toward more than 100 classical novae for emission in lines of the CO or HCN molecules using single-dish telescopes and interferometric arrays at millimeter and submillimeter wavelengths. The survey demonstrates that classical novae, young or old, are not strong sources of molecular emission at submillimeter and millimeter wavelengths. Additionally, we mapped CO emission around Nova Persei 1901 (GK Per), earlier claimed to be circumstellar in origin. Our measurements indicate that the observed emission is from the interstellar medium. Although no molecular emission at millimeter and submillimeter wavelengths has been found in classical novae, it is still likely that some will be detected with high-sensitivity interferometers such as ALMA.