A type II supernova is a huge source of neutrinos of all flavors. This supernova is identified with the collapse of the iron core of a massive ( > 8 M ⊙ ) evolved star. Present type II supernova detectors are able to mainly observe neutrinos coming from the so-called cooling phase.

2023年7月1日 · SN2009dd is a Type II supernova that displays characteristics of both the bright branch and weak interaction between the circumstellar material and the ejecta, as indicated by high-velocity features in the Balmer lines (Inserra et al., 2013). This feature is commonly observed in Type IIn SNe and Type IIL SNe (Bostroem et al., 2019). Our graph ...

1988年6月1日 · The shock dies into an accretion shock within milliseconds and the purely hydrodynamical explosion is aborted [3, 7, 9-12]. Implosion should, in many cases, lead to explosion - the Type II supernova [13]. The failure of the direct mechanism has focused attention on long-term shock revitalization schemes [2, 14-16] to power the supernova.

Supernova dynamics has seen much intense research from the astrophysics community across a broad spectrum of topics (see for example studies by Arnett et al. [566–568] regarding Supernova 1987A, a well-known Type-II core-collapse supernova), so that a full survey of the results cannot be given here (see [3,13]). However, we can discuss ...

2008年1月9日 · Type II Supernovae (SNII) have hydrogen in their spectra and their light curves peak around 10 42 erg s −1. In contrast, SNI do not show hydrogen in their spectra. If their spectra contain some silicon lines, they are called Type Ia. If the spectra contain helium lines they are called Type Ib. If they do not contain helium lines, they are ...

2008年1月9日 · Astronomy with Radioactivities. V. John F. Beacom, in New Astronomy Reviews, 2006 1 Introduction. The initial state that leads to a type-II (or type-Ib or type-Ic) supernova is essentially an iron white dwarf (the endpoint of nuclear fusion reactions) in the center of a massive star; when it reaches the Chandrasekhar mass, this core will collapse, along with the rest of …

1984年1月1日 · Major observatiori constraints for type ii supernova (SNii) are the existence of neutron stars in the center of SNil remnants and the observation of hydrogen iines in SN1I spectra. The first tact Is interpreted by the core bounce mechanism after the onset of a gravitationai coiiapse foiiowing core silicon burning of massive stars, leaving a ...

Type II and type Ia supernovae provide the dominant sites in which this “explosive nucleosynthesis” mechanism is known to operate. These two supernova sites operate on distinctively different timescales and eject different amounts of iron.

1999年4月1日 · The principal effects of evolution in a close binary system on the progenitor of a Type II supernova can be broadly divided into three categories (Podsiadlowski et al., 1992; hereafter PJH): (1) loss of a portion of the stellar envelope to the companion star, (2) accretion of matter from the companion star, or (3) merger of the two stars in a common-envelope phase.

2015年9月1日 · For a type II supernova, instead, it is often the case that the explosion takes place in the wind produced by a red giant pre-supernova progenitor star. The density of the wind can be written as (8) ρ ( R ) ≅ M ̇ 4 π R 0 2 V w R 0 R 2 = ρ ( R 0 ) R 0 R 2 , where M ̇ is the rate of mass loss of the red giant and V w is the wind velocity.