On the birtrate of galactic supernovae     

Ian Lerche 《Astrophysics and Space Science》1981,74(2):273-286

The birthrate of galactic supernovae is estimated in three different ways:

1. on the basis of the historical record (eight events) the mean time interval between supernovae, τ, is considered to be in the range τ=60±40 yr;
2. on the basis of an approximate total of 120 supernovae events in hundreds of other galaxies, considered similar to our own, the interval obtained is in the range τ=70±50 yr; (iii) on the
3. on the basis of the 130 supernovae remnants in our own Galaxy, the interval is estimated to be in the range τ=80±30 yr. The three ranges overlap, and we suggest that 70±35 yr represents a more realistic estimate of the rate than some that have previously been made.

The galactic radio supernovae remnants, and their observed systematic brightness gradients perpendicular to the galactic plane, imply a scale height of about 200 pc for the remnant progenitors, and indicate that the galactic magnetic field's scale-height is about 300 pc. Long standing anomalies associated with (a) the young remnant AD 1006, (b) the galactic loops, and (c) faint remnants, are accounted for by the brightness gradient effect, providing independent, and firm, corroborating evidence for the fundamental validity of the remnant method of deducing the galactic supernova birthrate.  相似文献   

地质因素对源岩评价结果的影响及其相对贡献量大小模拟     

庞雄奇  陈章明 《沉积学报》1998,16(1):50-57

源岩评价是油气资源评价的基础。目前,基于源岩排烃过程模拟结果可对源岩品质、属性和有效性进行综合定量评价。本文采用盆地模拟技术和不确定性分析方法对影响源岩评价的十三种地质因素的作用大小及其相对贡献量进行评价,同时探讨各种地质因素作用下源岩品质评价指数,属性评价指数和有效性评价指数的变化情况及分布概率。  相似文献   

Reflection of wide-angle acoustic waves from a high velocity interface     

Ian Lerche 《Pure and Applied Geophysics》1990,134(1):109-115

At angles other than normal incidence a pencil of plane acoustic waves, incident on a planar interface separating a low velocity medium from a high velocity medium, gives rise to a reflected pencil of waves which is laterally displaced from the illumination point of the incident pencil. The importance of this planar shift for understanding and interpreting wide-angle acoustic reflections is discussed, as is the variation of the equivalent depth below the interface at which a point-like reflection would be considered as an equivalent reflecting horizon.  相似文献   

Concerning isothermal self-similar blast waves     

I. Lerche 《Astrophysics and Space Science》1978,53(1):21-37

We investigate the one-dimensional self-similar flow behind a blast wave from a plane explosion in a medium whose density varies with distance asx _– with the assumption that the flow is isothermal. If <0 a continuous solution passing through the origin and the shock does not exist. If 1/3>>0 one critical point exists. To be physically acceptable the flow must by-pass this critical point. It is shown that a continuous solution passing through both the origin and through the shock and by-passing the critical point does exist. If 1>>1/3 the first critical point does not exist but a second one appears. To be physically acceptable the flow must again by-pass this new critical point. We show that a continuous solution passing through both the origin and the shock and by-passing the new critical point exists in this case. If >1 no physically acceptable solution exists since the mass behind the shock is infinite.The dependence of the solutions on the parameter is analytic for >0 so that interpolation between neighboring values of is permitted.We investigate the stability of these isothermal blast waves to one-dimensional but non-self-similar perturbations. If 0<<5/7, the solutions are shown to be linearly unstable against short wavelength perturbations near the origin. If the solution crosses the shock with a normalized velocityu>2 the solution is linearly unstable against short wavelength perturbations near the shock for 1>>0. If the solution crosses the shock with normalized velocity 2>u>1 (and it must cross the shock withu>1), the solution is certainly unstable against short wavelength perturbations near the shock for >11/19 and, depending on the crossing velocity, can be unstable there for all .Thus for 1>>0, the solution is always unstable somewhere. Since there is no characteristic time scale in the system all instabilities grow as a power law of time rather than exponentially. The existence of these instabilities implies that initial deviations do not decay and the system does not tend to a self-similar form.  相似文献