By Hale Bradt
An advent to simple functional instruments, equipment and phenomena that underlie quantitative astronomy.
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Extra info for Astronomy Methods: A Physical Approach to Astronomical Observations
It is not an SI unit, but we choose to use it because of its natural physical meaning. e. 946 × 1016 m ≈ 1 × 1016 m. 25 d where “d” is the non-SI unit for the mean solar day which is about equal to 86 400 SI (atomic) seconds. See Chapter 4. 9. The globular cluster, M10. Globular clusters are remnants from the formation of galaxies. There are about 160 associated with the (MW) Galaxy. Each contains 105 to 106 stars and orbits the center of the Galaxy. M10 is about 65 000 LY from the center of the Galaxy.
To what part of the electromagnetic spectrum does this photon belong? Speculate on the astrophysical signiﬁcance of this radiation. 41. (a) Use the plots of Fig. 2 to verify the statements in Sect. 4 regarding the altitudes from which the various branches of astronomy can be carried out. (b) Where would you set up a gamma-ray observatory operating in the region of 100 MeV if you needed to detect at least 50% of the photons? (c) How high should a sounding rocket go if it is to effectively detect 2-keV x rays from an astronomical object?
2. The ordinate represents height in the atmosphere, or equivalently, the fraction of the atmosphere above the indicated height. The abscissa indicates the frequency (Hz) or the wavelength (m) of the incoming radiation. The two solid lines indicate the positions (height) in the atmosphere to which 50% and 10% of the photons from a celestial source will penetrate; the other 50% or 90% are absorbed at higher elevations. To use the curves of Fig. 2, pick a frequency on the lower horizontal axis and read vertically until you intercept the lower curve.
Astronomy Methods: A Physical Approach to Astronomical Observations by Hale Bradt