But Hubble wasn’t done. His second major discovery also transformed astronomers’ understanding of the universe. As he dispersed the light fromdozens of galaxies into a spectrum, which recorded the amount of l
Finding cosmological distances is pretty challenging. Although you can calculate it, the best approach is to use a cosmological calculator with some standard parameters already input. Enter the redshift of the object you want to find the distance to, using the parameters suggested by the calculator...
cosmological redshift preserves wavelength ratios (it shifts uniformly the whole electromagnetic spectrum), it is scale invariant, it is a monotonically increasing function of distance, and it is source independent. It agrees with all experimental data. The distortion introduced by imaging from ...
Now, to calculate the gravitational force between the Earth and the Sun at the Earth's average orbital radius from the Sun, here is the basic data: Sun: mass 1.989 X 1032 gr Earth: mass 5.976 X 1027 gr; average orbital radius from Sun 1.49596 X 1013 cm So that… F = 1.989 X 1032...
What instrument is used to measure the redshift? How are wavelength and frequency of light related? How do you determine the magnification of a microscope's eyepiece? How does light have momentum? How to calculate refractive index using speed of light How does normal light differ from a laser...
How are wavelength and frequency of light related? How does a glass prism disperse light? How can you run at the speed of light? How does electromagnetic radiation work? How do worms react to light? During refraction, what happens to a wave when it travels from one medium to another? How...
Hubble took many photos through the observatory's telescope, and it allowed him to calculate the distance of other galaxies by comparing the varying degrees of luminosity in the stars themselves. Although there was no evidence suggesting the size of the other galaxies that Hubble discovered, he ...
# Calculate the product of flux and filter transmission flux_times_transmission = flux_mW_per_m2 * transmission_values # Integrate the product over the wavelength range to get erg/s/cm² erg_per_s_per_cm2 = simps(flux_times_transmission, wavelengths) # Convert the result to erg/s/cm...
The only problem is, similar phenomena have been observed around other types of compact objects – such as neutron stars, pulsars, and white dwarfs. As a result, astronomers need to observe accretion disks, energy sources and nearby objects closely to calculate the mass of the object affecting ...
What wavelength does the Hubble Telescope use? How does redshift help astronomers? How does a Newtonian telescope work? How did the ancient Greeks use astronomy? How does the Kepler Space Telescope discover planets? How often did the Kepler Space Telescope take measurements?