2007/10/10 by Benjamin F. Lane, B. F. Lane, A. Retter +4
Physics and Astronomy · #Advanced X-ray Imaging Techniques #Angular diameter #Astrophysical Phenomena and Observations #Astrophysics #Brightness #Interferometry #Laser-Plasma Interactions and Diagnostics #Measure (data warehouse) #Nova (rocket) #Optics #Physics #Stars #astro-ph
paper · pdf · doi:10.1086/521700
6 Pages, Accepted for publication in ApJ
arxiv created 2007/10/10 · openalex publication_date 2007/11/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have resolved the classical nova V1663 Aql using long-baseline near-IR interferometry covering the period from ~5 to 18 days after peak brightness. We directly measure the shape and size of the fireball, which we find to be asymmetric. In addition, we measure an apparent expansion rate of 0.21 ± 0.03 mas day -1 . Assuming a linear expansion model, we infer a time of initial outburst approximately 4 days prior to peak brightness. When combined with published spectroscopic expansion velocities, our angular expansion rate implies a distance of 8.9 ± 3.6 kpc. This distance measurement is independent of, but consistent with, determinations made using widely available photometric relations for novae.