I. Recall these cases where there is no radiation and no cosmological constant:
ID: 112888 • Letter: I
Question
I. Recall these cases where there is no radiation and no cosmological constant: For 0-1 Hor-2 (1-ya). For ,-0, Hor = 2(1/a-a). For ,-2, Hor = (1-a). (2 pt.) The spectral flux is nearly independent of the density parameter for nearby supernovae. Calculate numerical values for = 0 and ,-1 and a=0.99. How much brighter is the spectral flux for 10-1? a. b. (2 pt.) Explain why part (a) is important in finding the luminosity of supernovae. (2 pt.) Calculate numerical values for the spectral flux for 0-0 and 0-1 and a-0.5. How much brighter is the spectral flux for = 1? C. (2 pt.) Explain why part (c) is important in finding the density parameter of the universe. d.Explanation / Answer
A) Spectral flux is a measure of how quickly the power spectrum of a signal is changing, calculated by comparing the power spectrum for one frame against the power spectrum from the previous frame. More precisely, it is usually calculated as the 2-norm (also known as the Euclidean distance) between the two normalised spectral.
=integrated 0-1(1-a)
=(1-.99)1-0=.01
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B) Supernovae in other galaxies cannot be predicted with any meaningful accuracy.Most scientific research that deals with the luminosity of the galaxy are in the interest in supernovae as standard candles for measuring distance, for example—require an observation of their peak luminosity. It is therefore important to discover them well before they reach their maximum.
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C) In spectroscopy, spectral flux density is the quantity that is used to describes the rate at which energy is transferred by electromagnetic radiation through which a real or can take as virtual surface per unit surface area and per unit wavelength. It is a radiometric measure, as distinct from measures that characterize light in terms of the electromagnetic field or photons. In SI units of it is measured in W m3 or W m2 m1 W·m2·Hz1, Jansky or solar flux units. The terms irradiance, radiant exitance, radiant emittance, and radiosity are closely related to spectral flux density.
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D) The density parameter can be defined as it is the ratio of the average density of matter and energy in the Universe to the critical density (the density at which theUniverse would stop expanding only after an infinite time). It is important to note that the used in the calculation of 0 is the total mass/energy density of the universe. It have the importance because it enables us to detect the life of Universe with it size. Although it also help us to determine As well as analysis the increasing in the entropy of univerae.