The Energy Sources, the Physical Properties, and the Mass-loss History of SN 2017dio

Abstract

We study the energy sources, the physical properties of the ejecta and the circumstellar medium (CSM), and the mass-loss history of the progenitor of SN 2017dio, which is a broad-lined Ic (Ic-BL) supernova (SN) having unusual light curves (LCs) and signatures of hydrogen-rich CSM in its early spectrum. We find that the temperature of SN 2017dio began to increase linearly about 20 days after the explosion. We use the ^56 Ni plus the ejecta–CSM interaction model to fit the LCs of SN 2017dio, finding that the masses of the ejecta, the ^56 Ni, and the CSM are ∼12.41 M _⊙ , ∼0.17 M _⊙ , and ∼5.82 M _⊙ , respectively. The early-time photosphere velocity and the kinetic energy of the SN are, respectively, ∼1.89 × 10 ^4 km s ^−1 and ∼2.66 × 10 ^52 erg, which are comparable to those of SNe Ic-BL and hypernovae (HNe), respectively. We suggest that the CSM of SN 2017dio might be from a luminous blue variable–like outburst or pulsational pair instability ∼1.2−11.4 yr prior to the SN explosion or binary mass transfer. Moreover, we find that its ejecta mass is larger than those of many SNe Ic-BL and that its ^56 Ni mass ( M _Ni ) is approximately equal to the mean (or median) value of M _Ni of SNe Ic-BL in the literature but lower than M _Ni of prototype HNe (e.g., SN 1998bw and SN 2003dh).

Keywords

• Supernovae
• Type Ic supernovae
• Circumstellar matter