physics in the vicinity of black holes andrej Čadež, massimo calvani, andreja gomboc, claudio...
TRANSCRIPT
Physics in the vicinity of black holes
Andrej Čadež, Massimo Calvani, Andreja Gomboc, Claudio Fanton,Uroš Kostić
Plan of the talk
• Black hole solutions
• Light-like and time-like orbits
• Astrophysical evidence
• Acreetion disks and line profiles
• Effects due to curved space-time and tidal interaction
Schwarzschild solution
Transformation to Novikov coordinates; Introduce:
ds2 12Mrdt2 11 2Mr dr2 r2d2 Sin2d2
T 2MR 122M 2M2
R2 1
12R2 132ArcCos2MR2 1
Rr2M
1 and find that the metric
ds2 dT2R2 1R2R2dR2 2d2 Sin2d2
Can be transformed into the above, where the coordinates are related as shown in next picture
Constant Schwarzschild coordinates are shown as colored curves and constant Schw. Time as black lines
6M 10M 14M 18M 22M26MR
10
20
30
40
T
2 3 5 7 10 20 40 60rc2
GM
-0.4
-0.2
0.2
0.4
0.6
Ueffc2
Effective potential
Ueff 2
2r21 2G M
rc2 G M
r
space likeorbits:
2drd2 l2
2 r21 2G M
rc2 G M
r
1 c2
2 122c4
light likeorbits 0, 0, Limitl:12drd2 2
2r21 2G M
rc2 G M
r12c2
Angular momentum
l r2dd
Types of lightlike geodesics in the outer region of the Schwarzschild space-time
constants of motion: angular momentum, two components of orbit normal
Timelike geodesics are similar, except that there are also precessing Kepler type orbits
constants of motion: energy, angular momentum, two components of orbit normal
All equations of orbits are analyticaly solvable in terms of elliptic functions (Čadež&Kostič,Phys.Rev.D72,104024(2005))
L/=10• Left:fixed small angular momentum, increasing energy>c2
• Right:fixed >c2 energy, decreasing angular momentum
• Down bound <c2 energy
Geodesic in the outer region of Kerr space-time are similar to those in the Schwarzschild space-time, except that orbital angular momentum is
coupled to the angular momentum of the black hole, which induces a precession of the orbit about the black hole spin axis with the angular
velocity proportional to 1/r3. As a result orbits can no longer be considered planar. For light-like orbits only two constants are known:
angular momentum and Carter’s constant, which suffices to analytically express only the projection of the orbit equation on the r- “plane” (Fanton,Calvani,deFelice,Čadež:PASJ49,159-169(1997)), the
coordinate and the time are not known to be expressible analytically.
Astrophysical evidence
• Stellar mass black holes are very small
• In order to find them, people were looking for binaries with one dark and very massive (more than 3 solar masses) component. A few were found, but it was very difficult to confirm the mass of the dark component, and, in particular, to exclude the possibility that the dark component is a neutron star.
• Quasars, the superluminous galaxies, that were known to have very small (at most a few light years or light months) central engines were theorized to be powered by massive (up to 109 Solar Masses) black holes. The first strong hint of the existence of galactic black holes came from Hubble space telescope:
RS 2G Mc2
3kmMSonceM
Aktivne galaksije so podobne kvazarjem in iz njih brizgajo podobni ultrarelativistični
curki, vidni v radijski svetlobiSpodaj radijska slika, levo optična
Disks and jets are ubiquitous, but to prove that they are formed around a black hole, one must show that disk material is orbiting at a velocity close to speed of light and we do not have the resolution to distinguish
between the approaching and receding part of the disk. When observing the disk at coarser resolution, the spectral contibutions from
approaching and receding parts blend into a Doppler broadened spectral line. Doppler broadenings of a few 1000km/sec were observed in some active galaxies, but still far from the near speed of light velocity expected in a relativistic dics around the black hole. The reason is that
the temperature in the disk increases toward the center and optical lines can no longer be produced in such hot regions. So must look at
X-ray spectra. First observations by ASCA (launched 1993)
Assume thin, optically thick disk and deduce radial emisivity law;line shapes are consistent with the emitting region very close to the
black hole
Čadež, Calvani,New Astronomy 5,69,2000
Y
Zaresna črna luknja
Radijska slika galakticnega centra (NRAO, Jusef Zadek) levo in infrardeči
blišč v SgrA* (Genzel et. All, Nature 425,934,2003 )
Many flares in infrared and in X-rays have been observed in the Galactic center since, since the rate is close to 1 per day. A typical energy release per flare is of the order 1039.5erg = 3.5 1018gc2. Flares often exhibit periodic modultions on a time scale of 15 to 20 minutes and last a few thousand seconds. Can this modulation have something to do with the motion of a small source in the vicinity of the black hole?
How would one see a point source of light falling down the black hole? (Sorry, movies must be played outside Powerpoint)
A simple fit to the infrared flare is possible if one assumes that an object of the size of an asteroid is critically captured by the black hole. This requires the object to continuously loose angular momentum and
energy until it reaches the critical angular momentum for capture
The effective potential as a function of time, felt by a gravitating body that is tidaly interacting with another body (the black hole); during the process energy is dissipated by tides and angular momentum is transfered between spin and orbit (Hut’s theory is well understood for classical stars, but still needs closer
scrutiny in connection with black holes)