Interplanetary Dust and Near-Earth Objects: a source of noise for LISA?
Errata-corrige
pg.123, footnote: [. . . ] while NEOs are almost all brighter than H = 13. reads:
[. . . ] while NEOs are almost all fainter than H = 13. pg. 140: L is the arm length, f is the laser frequency [. . . ]
reads:
L is the arm length, f = ω/2π is the Fourier frequency [. . . ]
pg. 143: [. . . ] thus replacing the fluxes (6.17) and the first of (6.18) in Case (A). reads:
[. . . ] thus replacing the fluxes (6.17) and (6.18) in Case (A). pg. 211: We have used L = 5 × 109
m, λ = 1.064 µm, w0 = 30 cm and ¯v =
2 × 104
m/sec as the LISA and dust parameters. reads:
We have used L = 5×109
m, λ = 1.064 µm and ¯v = 2×104
m/sec as the LISA and dust parameters. Concerning the beam diameter, in phase noise calculations either the beam radius or diameter can be used, so we will adopt w0= 30 cm, the difference between the two approaches
being just a factor √2. Since the beam overfills the mirror, smaller beam diameters are more efficient in light loss, while larger diameters would produce a smoother far field pattern.
pg. 216, Table 1.2: (106
g/cm3) reads:
(g/cm3)
