Accretion High Energy Astrophysics
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Transcript of Accretion High Energy Astrophysics
Introduction
• Mechanisms of high energy radiation
X-ray sources
Supernova remnants Pulsars
thermalsynchrotron
loss rotational energymagnetic dipole
Accretion onto a compact object
• Principal mechanism for producing high-energy radiation
• Most efficient of energy production known in the Universe.
RMmGEacc
Gravitational potential energy released for body mass M and radius R when mass m accreted
Example - neutron star
Accreting mass m=1kg onto a neutron star:
neutron star mass = 1 solar massR = 10 km=> ~10 m Joules, ie approx 10 Joules per kg of accreted matter - as electromagnetic radiation
R
M
m
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16
Efficiency of accretion
• Compare this to nuclear fusion H => He releases ~ 0.007 mc ~ 6 x 10 m Joules - 20x smaller (for ns)
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RMmGEacc
So energy released proportional to M/R ie the more compact a body is, the more efficient accretion will be.
Accretion onto white dwarfs
• For white dwarfs, M~1 solar mass and R~10,000km so nuclear burning more efficient by factor of ~50.
• Accretion still important process however - nuclear burning on surface => nova outburst - accretion important for much of lifetime
Origin of accreted matter
• Given M/R, luminosity produced depends on accretion rate, m.
• Where does accreted matter come from? ISM? No - too small. Companion? Yes.
.
RGMm
dtdm
RGM
dtdEL acc
acc .
Accretion onto AGN
• Active Galactic Nuclei, M ~ 10 solar mass - very compact, very efficient (cf nuclear) - accretes surrounding gas and stars
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Fuelling a neutron star
• Mass = 1 solar mass observed luminosity = 10 J/s (in X-rays)
• Accretion produces ~ 10 J/kg
• m = 10 / 10 kg/s ~ 3 x 10 kg/year ~ 10 solar masses per year
31
16
31 16 22
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.
The Eddington Luminosity
• There is a limit to which luminosity can be produced by a given object, known as the Eddington luminosity.
• Effectively this is when the inward gravitational force on matter is balanced by the outward transfer of momentum by radiation.
Eddington Luminosity
Outgoing photons from M scatter material (electrons and protons) accreting.
rM m
Fgrav Frad
Accretion rate controlled by momentum transferred from radiation to mass
Newtonr
MmGFgrav 2 Note that R is now negligible wrt r
Scattering
L = accretion luminosity
Scattering cross-section will be Thomson cross-section ; so no. scatterings per sec:
hrL 1
4 2 photons m s no. photons crossing at r per second
-2 -1
hrL e
24
e
Momentum transferred from photon to particle:
Momentum gained by particle per second = force exerted by photons on particles
h e-, p ch
Newtoncr
Lc
hhr
L ee22 44
Eddington Limit
radiation pressure = gravitational pullAt this point accretion stops, effectively
imposing a ‘limit’ on the luminosity of a given body.
224 rMmG
crL e
e
cGMmL
4So the Eddington
luminosity is:
Assumptions made
• Accretion flow steady + spherically symmetric: eg. in supernovae, L exceeded by many orders of magnitude.
• Material fully ionized and mostly hydrogen: heavies cause problems and may reduce ionized fraction - but OK for X-ray sources
Edd
What should we use for m?
Electrostatic forces between e- and p binds them so act as a pair.
pep mmmm Thus:
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27118
1065.61067.1.1067.61034
EddL M Joule/sec
3.6 M Joule/sec
SUNMM31103.1 Joule/sec
Black Holes
• Black hole does not have hard surface - so what do we use for R?
• Use efficiency parameter,
• at a maximum = 0.42, typically = 0.1
• solar mass bh as efficient as neutron star
2McLacc then.
Emitted Spectrum
• define temperature T such that h~kT• define ‘effective’ BB temp T
• thermal temperature, T such that:
rad rad
b
4/124/ RLT accb
th
thep kT
RmmM
G232
kRGMm
T pth 3
=>
Accretion temperatures• Flow optically-thick:
• Flow optically-thin:
brad TT ~
thrad TT ~
Accretion energies
• In general,
• For a neutron star,
• assuming
thradb TTT
KTth11104.5
KTb7102
sJMMLL
SunEddacc /103.1 31
Neutron star spectrum
• Thus expect photon energies in range:
• similarly for a stellar mass black hole• For white dwarf, L ~10 J/s, M~M ,
R=5x10 m,
• => optical, UV, X-ray sources
MeVhkeV 501
keVheV 1006
acc 26
Sun6
Accretion modes in binaries
ie. binary systems which contain a compact star, either white dwarf, neutron star or black hole.
(1) Roche Lobe overflow(2) Stellar wind- correspond to different types of X-ray
binaries
Roche Lobe Overflow
• Compact star M and normal star M
• normal star expanded or binary separation decreased => normal star feeds compact
1 2
+CM MM 12
a
Roche equipotentials• Sections in the orbital plane
+ ++M
M12CM
L1
v
12 MM
Accretion disk formationMatter circulates around the compact object:
matter inwards
ang mom outwards
• Material transferred has high angular momentum so must lose it before accreting => disk forms
• Gas loses ang mom through collisions, shocks and viscosity: kinetic energy converted into heat and radiated.
• Matter sinks deeper into gravity of compact object
Disk Luminosity
The total energy available from the accretion of mass m onto M with radius R is:
But not all of this has to be lost (ie radiated from) the accretion disk – there may be other processes involved…
Eacc = GMm R
Energy losses from the disk
Ebind = GMm 2R
Ebind ~ 0
R
and Lbind = GMM 2R
So the energy which has been lost in the disk by m is:
Edisk = GMm 2R
and Ldisk = GMM 2R
= ½Lacc
Disk structureThe other half of the accretion luminosity is
released very close to the star.
X-ray UV optical
Hot, optically-thin inner region; emits bremsstrahlung
Outer regions are cool, optically-thick and emit blackbody radiation
bulge
Stellar Wind Model
Early-type stars have intense and highly supersonic winds. Mass loss rates - 10 to 10 solar masses per year.
For compact star - early star binary, compact star accretes if
-6-5
GMmr > 1
2m(v + v )2 2
w ns
Thus :r acc = 2GM
v + v 2 2w ns
bow shockmatter collects in wake
racc
Stellar wind model cont.
• Process much less efficient than Roche lobe overflow, but mass loss rates high enough to explain observed luminosities.
• 10 solar masses per year is required to produce X-ray luminosities of 10 J/s.
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Magnetic neutron starsFor neutron star with strong mag field, disk
disrupted in inner parts.
This is where most radiation is produced.Compact object spinning => X-ray pulsator
Material is channeled along field lines and falls onto star at magnetic poles
‘Spin-up pulsars’
• Primary accretes material with angular momentum => primary spins-up (rather than spin-down as observed in pulsars)
• Rate of spin-up consistent with neutron star primary (white dwarf would be slower)
• Cen X-3 ‘classical’ X-ray pulsator
Types of X-ray BinariesGroup I Group IILuminous (early, Optically faint (blue)massive opt countpart) opt counterpart(high-mass systems) (low-mass systems)hard X-ray spectra soft X-ray spectra(T>100 million K) (T~30-80 million K)often pulsating non-pulsatingX-ray eclipses no X-ray eclipsesGalactic plane Gal. Centre + bulgePopulation I older, population II