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Träfflista för sökning "WFRF:(Tomasella Lina) srt2:(2012-2014)"

Sökning: WFRF:(Tomasella Lina) > (2012-2014)

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1.
  • Bersten, Melina C., et al. (författare)
  • THE TYPE IIb SUPERNOVA 2011dh FROM A SUPERGIANT PROGENITOR
  • 2012
  • Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 757:1
  • Tidskriftsartikel (refereegranskat)abstract
    • A set of hydrodynamical models based on stellar evolutionary progenitors is used to study the nature of SN 2011dh. Our modeling suggests that a large progenitor star-with R similar to 200 R-circle dot-is needed to reproduce the early light curve (LC) of SN 2011dh. This is consistent with the suggestion that the yellow super-giant star detected at the location of the supernova (SN) in deep pre-explosion images is the progenitor star. From the main peak of the bolometric LC and expansion velocities, we constrain the mass of the ejecta to be approximate to 2 M-circle dot, the explosion energy to be E = (6-10) x 10(50) erg, and the Ni-56 mass to be approximately 0.06 M-circle dot. The progenitor star was composed of a helium core of 3-4 M-circle dot and a thin hydrogen-rich envelope of approximate to 0.1M(circle dot) with a main-sequence mass estimated to be in the range of 12-15 M-circle dot. Our models rule out progenitors with helium-core masses larger than 8 M-circle dot, which correspond to M-ZAMS greater than or similar to 25M(circle dot). This suggests that a single star evolutionary scenario for SN 2011dh is unlikely.
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2.
  • Valenti, Stefano, et al. (författare)
  • A SPECTROSCOPICALLY NORMAL TYPE Ic SUPERNOVA FROM A VERY MASSIVE PROGENITOR
  • 2012
  • Ingår i: The Astrophysical Journal Letters. - 2041-8205. ; 749:2, s. L28-
  • Tidskriftsartikel (refereegranskat)abstract
    • We present observations of the Type Ic supernova (SN Ic) 2011bm spanning a period of about one year. The data establish that SN 2011bm is a spectroscopically normal SN Ic with moderately low ejecta velocities and with a very slow spectroscopic and photometric evolution (more than twice as slow as SN 1998bw). The Pan-STARRS1 retrospective detection shows that the rise time from explosion to peak was similar to 40 days in the R band. Through an analysis of the light curve and the spectral sequence, we estimate a kinetic energy of similar to 7-17 foe and a total ejected mass of similar to 7-17 M-circle dot, 5-10 M-circle dot of which is oxygen and 0.6-0.7 M-circle dot is Ni-56. The physical parameters obtained for SN 2011bm suggest that its progenitor was a massive star of initial mass 30-50 M-circle dot. The profile of the forbidden oxygen lines in the nebular spectra shows no evidence of a bi-polar geometry in the ejected material.
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