Radiation Hydrodynamics of SN 1987A. I. Global Analysis of the Light Curve for the First 4 Months

Abstract

The optical/UV light curves of SN 1987A are analyzed with the multienergy group radiation hydrodynamics code STELLA. The calculated monochromatic and bolometric light curves are compared with observations shortly after shock breakout, during the early plateau, through the broad second maximum, and during the earliest phase of the radioactive tail. We have concentrated on a progenitor model calculated by Nomoto & Hashimoto and Saio, Nomoto, & Kato, which assumes that 14 of the stellar M _ mass is ejected. Using this model, we have updated constraints on the explosion energy and the extent of mixing in the ejecta. In particular, we determine the most likely range of E/M (explosion energy over ejecta mass) and (radius of the progenitor). In general, our best models have energies in the range R 0 E \ (1.1^0.3) ] 1051 ergs, and the agreement is better than in earlier, Ñux-limited di †usion calculations for the same explosion energy. Our modeled B and V Ñuxes compare well with observations, while the Ñux in U undershoots after D10 days by a factor of a few, presumably owing to NLTE and line transfer e †ects. We also compare our results with IUE observations, and a very good quantitative agreement is found for the Ðrst days, and for one IUE band (2500È3000 as long as for 3 months. We point out A ) that the V Ñux estimated by McNaught & Zoltowski should probably be revised to a lower value.

Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars

“…For example, the 56Ni mass yield of our 13 model M _ has to be less than 0.006 which appears to be inconsis-M _ , tent with the observed luminosities (and thus the 56Ni mass) of core collapse supernovae SN 1993J and SN 1994I, whose progenitor masses are estimated to be 13È15 (see, e.g., M _ Fig. 10 of Iwamoto et al 2000). …”

“…Recent observations suggest that at least some core collapse SNe explode with large explosion energies, which may be called "" hypernovae ÏÏ (e.g., Galama et al 1998 ;Iwamoto et al 1998Iwamoto et al , 2000Nomoto et al 2000). These SNe likely originate from relatively massive SNe (M Z 25 M _ ).…”

“…5 Blinnikov et al 2000). On the other hand, the masses of the progenitors of hypernovae with (SN 1998bw, SN E 51 [ 10 1997ef, and SN 1997cy) are estimated to be M Z 25 M _ Iwamoto et al 1998Iwamoto et al , 2000Woosley, Eastman, & Schmidt 1999 ;Turatto et al 2000). This could be related to the stellar mass dependence of the explosion Ðgure.…”

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

“…Radiation hydrodynamic calculations of the explosion and evolution of Type II SNe have been presented by Grassberg et al (1971), Falk & Arnett (1977), Falk (1978), Klein & Chevalier (1978), Hillebrandt & Müller (1981), and Litvinova & Nadezhin (1983, 1985, as well as more specifically for SNe II-P by Young (2004), Utrobin (2007), Utrobin & Chugai (2009), Bersten et al (2011), and Dessart & Hillier (2011), for SNe II-L by Swartz et al (1991) and Blinnikov & Bartunov (1993) and for the peculiar Type II-P SN 1987A by Blinnikov et al (2000), Dessart & Hillier (2010) and Pumo & Zampieri (2011). Here we give a summary view of the physical processes at play and the various evolutionary stages seen in these simulations.…”

Photometric Identification of Population III Core-Collapse Supernovae: Multicolor Light Curve Simulations

“…For calculation of the light curves we use the multigroup radiation hydrodynamic code STELLA [1]. We calculate the light curves of zero-and solar metallicity progenitors with the main-sequence masses M MS = 25, 40, 100 M and the explosion energies corresponding to SNe (E 51 ≡ E/10 51 erg = 1) and hypernovae (HNe)(E 51 ≥ 10).…”