We have calculated the cosmic ray(CR) acceleration at young remnants from Type Ia supernovae expanding into a uniform interstellar medium(ISM). Adopting quasi-parallel magnetic fields, gasdynamic equations and the diffusion convection equation for the particle distribution function are solved in a comoving spherical grid which expands with the shock. Bohm-type diffusion due to self-excited Alfven waves, drift and dissipation of these waves in the precursor and thermal leakage injection were included. With magnetic fields amplified by the CR streaming instability, the particle energy can reach up to 1016Z eV at young supernova remnants(SNRs) of several thousand years old. The fraction of the explosion energy transferred to the CR component asymptotes to 40-50 % by that time. For a typical SNR in a warm ISM, the accelerated CR energy spectrum should exhibit a concave curvature with the power-law slope flattening from 2 to 1.6 at E ≳ 0.1 TeV.

The wind-formed features observed in the early SNe spectra type II and Ia give an evidence of the existence of an ellipsoidal shell formed by the stellar wind prior to the explosion. Such non-spherical shell can occur not only at scales of parsec (the case of SN 1987 A progenitor), but at the scales of 1000 times less. Such shells can be the result of the radial pulsation. The prolate multi-shell structures are interpreted as a result of a pulsation processes with recurrent wind ejections with velocity increasing.

Observed spectra of supernovae allow the empirical classification of supernovae into two basic categories, Type I with little or no evidence of hydrogen, and Type II with obvious evidence for hydrogen. The broad class of Type I can be subdivided depending on whether helium or silicon and other intermediate mass elements is observed. Understanding the physical processes that underlie these classifications---the progenitor evolution. the explosion mechanism, and end products---requires calculation of radiative transfer and model spectra. While most Type II occur in evolved massive stars that undergo core collapse. some may span the dividing line between degenerate and non-degenerate carbon burning and involve both core collapse and thermonuclear explosion. Type Ia are still most plausibly explained as thermonuclear explosions in carbon/oxygen white dwarfs in binary systems. Type Ib reveal helium atmospheres and are probably the result of core collapse in the helium core of a massive star that has lost its hydrogen envelope to a binary companion or to a wind. Type Ic supernovae are probably related to Type Ib but have also lost their helium envelope to reveal a mantle rich in oxygen.

16세기 후반에서 17세기 초에 우리나라에서 관측된 4개의 초신성(Tycho Supernova, Kepler Supernova, Cassiopeia Nova 및 Cassiopeia A)의 기록은 세계 어느 나라 천문관측기록 보다 더 자세히, 또 더 정확히 표시되어 있다. 특히 Kepler Supernova의 기록은 우리나라 이조 왕조실록에 가장 자세하게 실려있다. 위치뿐만 아니라 밝기, 관측시간 및 관측상태를 낱낱이 표기한 이 관측치로부터 다음과 같은 광도곡선상의 특징을 알아낼 수 있다. 1. 준극대광도(Pre-max-halt)는 1604년 10월 20일부터 10월 26일 사이 2. 극대광도(Maximum Luminosity)는 1604년 10월 29일부터 11월6일 사이 3. 천이과정(Transition)은 아마도 1604년 11월 28일부터 1604년 12월 26일 사이에 있었을 것이다.

1. 28 candidates of novae and supernovae were selected from ancient Korean observational records. 2. 4 Supernovae were confirmed. 3. 1 guest star was suspected as the original explosion of Cas A. 4. 9 asterisked positions were suggested for further study in the hope of finding additional supernovae-radio sources.