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EXTRA CREDIT
Find as many mistakes as you can and correct them!
Cite your source for the lyrics and astronomical data.
Show any math/conversions explicitly.
Due: Last day of classes, May 1
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Room Change
Monday April 20, 2009BioChem room 111
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Outline
X-ray binaries – nuclear physics at the extremes
1. Observations2. X-ray Burst Model3. Nuclear Physics – the rp process4. Open Questions
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X-rays
Wilhelm Konrad Roentgen,First Nobel Price 1901 fordiscovery of X-rays 1895
First X-ray image from 1890(Goodspeed & Jennings, Philadelphia)
Ms Roentgen’s hand, 1895
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0.5-5 keV (T=E/k=6-60 x 106 K)
Cosmic X-rays: discovered end of 1960’s:
Again Nobel Price in Physics 2002for Riccardo Giacconi
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D.A. Smith, M. Muno, A.M. Levine,R. Remillard, H. Bradt 2002(RXTE All Sky Monitor)
H. Schatz
X-rays in the sky
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First X-ray pulsar: Cen X-3 (Giacconi et al. 1971) with UHURU
First X-ray burst: 3U 1820-30 (Grindlay et al. 1976) with ANS
Today:~50
Today:~70 burst sources out of 160 LMXB’s
Total ~230 X-ray binaries knownTotal ~230 X-ray binaries known
T~ 5s
10 s
H. Schatz
Discovery of X-ray bursts and pulsars
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Typical X-ray bursts:
• 1036-1038 erg/s• duration 10 s – 100s• recurrence: hours-days• regular or irregular
Frequent and very brightphenomenon !
(stars 1033-1035 erg/s)
H. Schatz
Burst characteristics
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Neutron StarDonor Star(“normal” star)
Accretion Disk
The Model
Neutron stars:1.4 Mo, 10 km radius(average density: ~ 1014 g/cm3)
Typical systems:• accretion rate 10-8/10-10 Mo/yr (0.5-50 kg/s/cm2)• orbital periods 0.01-100 days• orbital separations 0.001-1 AU’s• surface density ~ 106 g/cm3
H. Schatz
The model
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Unstable, explosive burning in bursts (release over short time)
Burst energythermonuclear
Persistent fluxgravitational energy
H. Schatz
Observation of thermonuclear energy
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Energy generation: thermonuclear energy
Ratio gravitation/thermonuclear ~ 30 – 40(called α)
4H 4He
5 4He + 84 H 104Pd
6.7 MeV/u
0.6 MeV/u
6.9 MeV/u
Energy generation: gravitational energy
E =G M mu
R= 200 MeV/u
(“triple alpha”)
(“rp process”)
H. Schatz
Energy sources
(“CNO cycles”)
34He 12C
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10-2 10-1 100
accretion rate (L_edd)
0.16
0.17
0.18
0.19
0.2
0.21
0.22
0.23
0.24
tem
pera
ture
(GK
)
H. Schatz
Initial Conditions
Accreting material loses energy via X-ray emissionGravitational energy
Surface temperature related to accretion rateKinetic energy
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0 1 10temperature (GK)
10-15
10-14
10-13
10-12
10-11
10-10
10-9
rea
ctio
n ra
te (c
m2 s-1m
ole
-1)
Burst trigger rate is “triple alpha reaction” 3 4He 12C
Ignition: dεnucdT
dεcooldT> εnuc
εcool ~ T4
Ignition < 0.4 GK:unstable runaway
• heat added increases T• higher T increases εnuc• larger εnuc increase T more
Triple alpha reaction rate
Nuclear energy generation rate
Cooling rate
H. Schatz
Burst ignition at “low” accretion rates
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0 1 10temperature (GK)
10-15
10-14
10-13
10-12
10-11
10-10
10-9
rea
ctio
n ra
te (c
m2 s-1m
ole
-1)
Stable Burning: dεnucdT
dεcooldT< εnuc
εcool ~ T4
Stable Burning > 0.5 GK:
• heat added efficiently cooled• T doesn’t change dramatically
• NO X-Ray Bursting!!
Triple alpha reaction rate
Nuclear energy generation rate
Cooling rate
H. Schatz
Stable burning at “high” accretion rates
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27Si
neutron number13
Protonnumber
14(p,γ) (α,p)
(α,γ)
(,β+)
H. Schatz
Visualizing reaction networks
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3 4 5 6 7 8
9 10
111213
14
C (6)N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)
3 4 5 6 7 8
9 10
111213
14
C (6)N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)
“Cold” CN(O)-Cycle
Hot CN(O)-Cycle
),(14 γσε pNv >∝<Energy production rate:
T9 < 0.08
T9 ~ 0.08-0.1
const)/(1 11)(15)(14=+∝ −−
++ ββλλε
OO
“beta limited CNO cycle”
Note: condition for hot CNO cycledepend also on density and Yp:
βγ λλ >,pon 13N:
βλσρ >><⇔ vNY Ap
Ne-Na cycle !
14O T1/2=71s
15O T1/2=122s
22Mg T1/2=3.9s
23Mg T1/2=11.3s
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3 4 5 6 7 8
9 10
111213
14
C (6)N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)Very Hot CN(O)-Cycle
still “beta limited”
T9 ~ 0.3
18Ne T1/2=1.7s
3α flow
3 4 5 6 7 8
9 10
111213
14
C (6)N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)Breakout
processing beyond CNO cycleafter breakout via:
3α flow
T9 > 0.36 15O(α,γ)19Ne18Ne(α,p)21NaT9 > 0.62
How do we calc?
15O T1/2=122s
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0.0 0.5 1.0 1.5100
101
102
103
104
105
Temperature (GK)
Den
sity
(g/c
m3 )
Current 15O(a,γ) Ratewith X10 variation
Multizone Nova model(Starrfield 2001)
Breakout
NoBreakout
New lower limit for density from B. Davids et al. (PRC67 (2003) 012801)
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No Breakout15O(α,γ) 19Ne Breakout
18Ne(α,p)21NaBreakout
Gorres, Weischer and ThielemannPRC 51 (1995) 392
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0 1 23 4
5 6
7 8
9 10
111213
14
1516
17181920
2122
2324
25262728
2930
3132
33343536
3738394041
424344
45464748
49505152
535455
56
5758
59
H (1)He (2)Li (3)
Be (4) B (5) C (6) N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)Al (13)Si (14) P (15)
S (16)Cl (17)
Ar (18)K (19)
Ca (20)Sc (21)
Ti (22)V (23)
Cr (24)Mn (25)
Fe (26)Co (27)
Ni (28)Cu (29)
Zn (30)Ga (31)
Ge (32)As (33)
Se (34)Br (35)Kr (36)Rb (37)
Sr (38)Y (39)
Zr (40)Nb (41)
Mo (42)Tc (43)
Ru (44)Rh (45)Pd (46)Ag (47)
Cd (48)In (49)
Sn (50)Sb (51)
Te (52)I (53)
Xe (54)
Collaborators:L. Bildsten (UCSB)A. Cumming (UCSC)M. Ouellette (MSU)T. Rauscher (Basel)F.-K. Thielemann (Basel)M. Wiescher (Notre Dame)
(Schatz et al. PRL 86(2001)3471)
H. Schatz
Doubly Magic Nuclei influence nucleosynthesis
40Ca – end of αp-process
56Ni – peak luminosity
100Sn – end of rp-process
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αp & rp competition− Important branching points
past 40Ca, α-induced reactions inhibited− rp-process continues
Most energy generated near 56Ni− Can develop cycles− Heavy α-nuclei are waiting points
100Sn region natural endpoint
H. Schatz
After Breakout
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H. Schatz
Competition between αp- & rp- processes
21Na
26Si
25Al
25Si
24Al
24Si
23Al
22Mg
22Mg is branching point
(p,g) and (a,p) compete
rp-process eats p’s
αp-process eats α’s
Branch points also appear at 26Si, 30S & 34Ar
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H. Schatz
55Co
60Zn
59Cu
59Zn
58Cu
58Zn
57Cu
56Ni
56Ni is doubly magic
59Cu is branch point
Either rp-continues
or (p,α) back to 56Ni
This is the NiCu cycle
Cycle pattern repeats for 60Zn
This is the ZnGa cycle
Development of Cycles
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Slow reactions extend energy generation abundance accumulation
(steady flow approximation λY=const or Y ~ 1/λ)
Critical “waiting points” can be easily identified in abundance movie
H. Schatz
Waiting points
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0 1 23 4
5 6
7 8
9 10
111213
14
1516
17181920
2122
2324
25262728
2930
3132
33343536
3738394041
424344
45464748
49505152
535455
56
5758
59
H (1)He (2)Li (3)
Be (4) B (5) C (6) N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)Al (13)Si (14) P (15)
S (16)Cl (17)
Ar (18)K (19)
Ca (20)Sc (21)
Ti (22)V (23)
Cr (24)Mn (25)
Fe (26)Co (27)
Ni (28)Cu (29)
Zn (30)Ga (31)
Ge (32)As (33)
Se (34)Br (35)Kr (36)Rb (37)
Sr (38)Y (39)
Zr (40)Nb (41)
Mo (42)Tc (43)
Ru (44)Rh (45)Pd (46)Ag (47)
Cd (48)In (49)
Sn (50)Sb (51)
Te (52)I (53)
Xe (54)
The Sn-Sb-Te cycle
104Sb 105Sb 106 107Sb
103Sn 104Sn 105Sn 106Sn
105Te 106Te 107Te 108Te
102In 103In 104In 105In
(γ,a)
Sb
β+
(p, )γ
Known ground stateα emitter
Endpoint: Limiting factor I – SnSbTe Cycle
Collaborators:L. Bildsten (UCSB)A. Cumming (UCSC)M. Ouellette (MSU)T. Rauscher (Basel)F.-K. Thielemann (Basel)M. Wiescher (Notre Dame)
(Schatz et al. PRL 86(2001)3471)
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Experiments in the rp-process
Henrique Bertulani
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Key nuclear physics parameters:• Proton separation energies (masses)• β-decay half-lives• proton capture rates
Key nuclear physics parameters:• Proton separation energies (masses)• β-decay half-lives• proton capture rates
Data needs for rp process
p-bound
Schatz et al. Phys. Rep. 294(1998)167
Exp.limit
41424344
45464748
49505152
535455
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5758
5960
6162636465666768697071727374
75767778
79808
(30)(31)
Ge (32)As (33)
Se (34)Br (35)Kr (36)Rb (37)
Sr (38) Y (39)
Zr (40)Nb (41)
Mo (42)Tc (43)
Ru (44)Rh (45)Pd (46)Ag (47)
Cd (48)In (49)
Sn (50)Sb (51)
Te (52) I (53)
Xe (54)
N=Z line
?
?
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Experimental data ?
Mass known < 10 keVMass known > 10 keVOnly half-life known
seen
Most half-lives known Masses still need work(need < 10 keV accuracy)mass models not the issue(extrapolation, coulomb shift)
Reaction rates ?
Most half-lives known Masses still need work(need < 10 keV accuracy)mass models not the issue(extrapolation, coulomb shift)
Reaction rates ?
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0 50 100 150 200 250 300time (s)
0e+00
5e+16
1e+17
lum
inos
ity (e
rg/g
/s)
BrownAudi unboundAudi bound
H. Schatz
Influence of masses on X-ray burst models
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Problem: Reaction rates
0 12
3 45 6
7 8
9 10
111213
14
1516
17181920
2122
2324
25262728
2930
3132
33343536
3738394041
424344
45464748
49505152
535455
56
5758
n (0)H (1)
He (2)Li (3)
Be (4) B (5) C (6) N (7)
O (8) F (9)
Ne (10)Na (11)
Mg (12)Al (13)Si (14) P (15)
S (16)Cl (17)
Ar (18) K (19)
Ca (20)Sc (21)
Ti (22) V (23)
Cr (24)Mn (25)
Fe (26)Co (27)
Ni (28)Cu (29)
Zn (30)Ga (31)
Ge (32)As (33)
Se (34)Br (35)Kr (36)Rb (37)
Sr (38)Y (39)
Zr (40)Nb (41)
Mo (42)Tc (43)
Ru (44)Rh (45)Pd (46)Ag (47)
Cd (48)In (49)
Sn (50)Sb (51)
Te (52)I (53)
Xe (54)
some experimental information available(most rates are still uncertain)
Theoretical reaction rate predictions:
Hauser-Feshbach: not applicable near drip line
Shell model: available up to A~63 but largeuncertainties (often x1000 - x10000) (Herndl et al. 1995, Fisker et al. 2001)
Are important when:• they draw on equilibrium• they are slow – low T(ignition, cooling, upper layers)
• several reactions compete
Need radioactive beams
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H. Schatz
Comparison to Observations
Galloway et al ApJS 179 (2007) 360
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H. Schatz
Repeated Observations of GS 1828 24
Galloway et al ApJ 601 (2004) 466
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H. Schatz
Average XRB Light Curve
Galloway et al ApJ 601 (2004) 466
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H. Schatz
Model Comparisons
Heger et al ApJL 671 (2007) 141
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H. Schatz
Summary
• rp-process is important to understand• X-ray bursts• crusts of accreting neutron stars/ transients• neutron stars !
• lots of open question – much work to do• modelling• nuclear physics (predict instabilities ?) • observations
• need radioactive beam experiments• much within reach at existing facilities• with RIA and FAIR precision tests possible