2007/07/24 by Kuntal Misra, Dave Pooley, Poonam Chandra +4 · 4 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Cosmic Phenomena #Epoch (astronomy) #Gamma-ray bursts and supernovae #Light curve #Luminosity #Pair-instability supernova #Plateau (mathematics) #RADIUS #Supernova #Type II supernova #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.12258.x
13 Figures, Accepted for Publication in MNRAS
arxiv created 2007/07/24 · openalex publication_date 2007/09/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present X-ray, broad-band optical and low-frequency radio observations of the bright type IIP supernova SN 2004et. The Chandra X-ray Observatory observed the supernova at three epochs, and the optical coverage spans a period of ∼470 d since explosion. The X-ray emission softens with time, and we characterize the X-ray luminosity evolution as LX∝t−0.4. We use the observed X-ray luminosity to estimate a mass-loss rate for the progenitor star of ∼2 × 10−6 M⊙ yr−1. The optical light curve shows a pronounced plateau lasting for about 110 d. Temporal evolution of photospheric radius and colour temperature during the plateau phase is determined by making blackbody fits. We estimate the ejected mass of 56Ni to be 0.06 ± 0.03 M⊙. Using the expressions of Litvinova & Nadëzhin we estimate an explosion energy of (0.98 ± 0.25) × 1051 erg. We also present a single epoch radio observation of SN 2004et. We compare this with the predictions of the model proposed by Chevalier, Fransson & Nymark. These multiwavelength studies suggest a main-sequence progenitor mass of ∼20 M⊙ for SN 2004et.