23.03.2013 Views

Pre-Phase A Report - Lisa - Nasa

Pre-Phase A Report - Lisa - Nasa

Pre-Phase A Report - Lisa - Nasa

SHOW MORE
SHOW LESS

You also want an ePaper? Increase the reach of your titles

YUMPU automatically turns print PDFs into web optimized ePapers that Google loves.

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

Hooray! Your file is uploaded and ready to be published.

Saved successfully!

Ooh no, something went wrong!