Pre-Phase A Report - Lisa - Nasa
Pre-Phase A Report - Lisa - Nasa
Pre-Phase A Report - Lisa - Nasa
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18 Chapter 1 Scientific Objectives<br />
radius R (m)<br />
10 13<br />
10 12<br />
10 11<br />
10 10<br />
10 9<br />
10 8<br />
10 7<br />
10 6<br />
10 5<br />
10 4<br />
10 3<br />
10 -1<br />
10 2<br />
Sun<br />
close NS-NS binary<br />
10 0<br />
10 1<br />
f = 10 -4 Hz<br />
LISA band Binary lifetime = 1 yr<br />
Black hole line<br />
10 2<br />
10 3<br />
10 4<br />
10 5<br />
mass M (solar masses)<br />
f = 1 Hz<br />
Binary chirp line<br />
10 6<br />
10 6 M o BH binary<br />
10 6 M o BH burst<br />
Figure 1.2 Gravitational dynamics. This diagram shows the wide range of<br />
masses and radii of sources whose natural dynamical frequency is in the LISA<br />
band. The two heavy lines delineate the outer limits of sources accessible from<br />
space, at gravitational wave frequencies of 10 −4 Hz and 1Hz. They follow the<br />
formula f GW =(GM/R 3 ) 1/2 /π.<br />
The “black hole line” follows R =2GM/c 2 ; if general relativity is correct, there<br />
are no systems below it. The “chirp line” shows the upper limit on binary<br />
systems whose orbital frequencies change (due to gravitational-wave energy<br />
emission) by a measurable amount (3×10 −8 Hz) in one year: any circular<br />
binary of total mass M and orbital separation R that lies below this line<br />
will “chirp” in LISA’s observations, allowing LISA to determine its distance.<br />
(See text.) The curve labelled “binary lifetime = 1 yr” is the upper limit on<br />
binaries that chirp so strongly that they coalesce during a LISA observation.<br />
Any binaries formed of black holes above 10 6 M⊙ that are in the LISA band<br />
will coalesce as LISA observes them.<br />
At the lower-mass end of LISA’s range we show the Sun and the shortest-period<br />
close neutron-star binary we expect LISA to see, which is on the chirp line but<br />
not the 1-year lifetime line. Near the upper mass limit we illustrate a 10 6 M⊙<br />
black hole formation burst and a 10 6 M⊙ black hole binary chirp (vertical line).<br />
Ground-based detectors operate only in the mass range between the f =1Hz<br />
line and the black-hole line.<br />
1.1.4 Other theories of gravity<br />
When using gravitational wave observations to test general relativity, it is important to<br />
have an idea of what alternative predictions are possible. While general relativity has<br />
successfully passed every experimental and observational test so far [5, 9], it is clear that<br />
3-3-1999 9:33 Corrected version 2.08<br />
10 7<br />
10 8