2020/12/31 by Izumi Hachisu, Mariko Kato
Physics and Astronomy · #Absolute magnitude #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Brightness #Function (biology) #Light curve #Magnitude (astronomy) #Nova (rocket) #Pulsars and Gravitational Waves Research #astro-ph.SR
paper · pdf · doi:10.3847/1538-4365/abd31e
published as ApJS, 253, 27 (2021) · 211 pages, 178 figures, typos corrected, published in ApJS, 253, 27 (2021). arXiv admin note: text overlap with arXiv:1905.10655
openalex created_date 2020/12/21 · openalex publication_date 2021/03/01 · arxiv created 2021/03/22 · arxiv updated 2021/03/23 · openalex updated_date 2026/08/05
Abstract Light curves and color evolutions of two classical novae can be largely overlapped if we properly squeeze or stretch the timescale of a target nova against that of a template nova by . Then, the brightness of the target nova is related to the brightness of the template nova by , where M [ t ] is the absolute magnitude and a function of time t , and f s is the ratio of timescales between the target and template novae. In the previous papers of this series, we show that many novae broadly overlap in the time-stretched ( B − V ) 0 – color–magnitude diagram. In the present paper, we propose two other ( U − B ) 0 – and ( V − I ) 0 – diagrams and show that their tracks overlap for 16 and 52 novae, respectively. Here ( U − B ) 0 , ( B − V ) 0 , and ( V − I ) 0 are the intrinsic U − B , B − V , and V − I colors and not changed by the time stretch, and M B , M V , and M I are the absolute B , V , and I magnitudes. Using these properties, we considerably refine the previous estimates of their distance and reddening. The obtained distances are in reasonable agreement with those of the Gaia Data Release 2 catalog.