Consequences of Supernovae

Branch, David; Wheeler, J. C.

doi:10.1007/978-3-662-55054-0_24

Cited by 1 publication

(1 citation statement)

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“…With these definitions, the late-time bolometric luminosity can be expressed as where M Ni is the initial mass of the radioactive 56 Ni synthesized during the explosion, S Ni and S Co are the functions for the total energy input from the Ni-and Co-decay, respectively (see Branch & Wheeler 2016;Szalai et al 2016 for further discussion). This equation corrects for the typographical error in the expression given by Valenti et al (2008), and accounts for the partial trapping of both gammarays and positrons via the deposition functions given above.…”

Section: Velocity Evolutionmentioning

confidence: 99%

EXTENSIVE SPECTROSCOPY AND PHOTOMETRY OF THE TYPE IIP SUPERNOVA 2013ej

Dhungana

Kehoe

Vinkó

et al. 2016

ApJ

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We present extensive optical (UBV RI, ¢ ¢ ¢ ¢ g r i z , and open CCD) and near-infrared (ZY JH) photometry for the very nearby Type IIP SN 2013ej extending from +1 to +461 days after shock breakout, estimated to be MJD 56496.9±0.3. Substantial time series ultraviolet and optical spectroscopy obtained from +8 to +135 days are also presented. Considering well-observed SNe IIP from the literature, we derive UBV RIJHK bolometric calibrations from UBV RI and unfiltered measurements that potentially reach 2% precision with a B−V colordependent correction. We observe moderately strong Si II l6355 as early as +8 days. The photospheric velocity (v ph ) is determined by modeling the spectra in the vicinity of Fe II l5169 whenever observed, and interpolating at photometric epochs based on a semianalytic method. This gives =  v 4500 500 ph km s −1 at +50 days. We also observe spectral homogeneity of ultraviolet spectra at +10-12 days for SNe IIP, while variations are evident a week after explosion. Using the expanding photosphere method, from combined analysis of SN 2013ej and SN 2002ap, we estimate the distance to the host galaxy to be -+ 9.0 0.6 0.4 Mpc, consistent with distance estimates from other methods. Photometric and spectroscopic analysis during the plateau phase, which we estimated to be 94±7 days long, yields an explosion energy of 0.9 0.3 10 51 erg, a final pre-explosion progenitor mass of 15.2±4.2  M and a radius of 250±70  R . We observe a broken exponential profile beyond +120 days, with a break point at +183±16 days. Measurements beyond this break time yield a 56 Ni mass of 0.013±0.001M  .

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Section: Velocity Evolutionmentioning

confidence: 99%