Five and a half roads to from a millisecond pulsar - ESO · Chile March 6-11, 2011 43 Thomas...
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Five and a half roads to from a millisecond pulsar
Thomas TaurisAIfA, University of Bonn Max-Planck-Institut für Radioastronomie, Bonn
Evolution of Compact Binaries, ESO Chile, March 6-11, 2011
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Chile March 6-11, 2011 2 Thomas Tauris, Bonn
• Millisecond pulsars - an introduction
• Mass transfer in X-ray binaries• Stability• Modes of mass transfer / loss
• Formation of millisecond pulsars1) LMXB Porb > Pbif
2) LMXB Porb < Pbif
3) IMXB Common Envelope4) IMXB Early case B5) IMXB Case A
• Summary
- PSR J1614-2230
For a review: Tauris & van den Heuvel (2006)
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Pulsars are key probes of fundamental physics
Nuclear physics
Particle physics
Condense matter physics
Atom physics
Plasma physics
Relativity
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Chile March 6-11, 2011 4 Thomas Tauris, Bonn
Equations-of-state forhigh density nuclear matter
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Detection of low frequency gravitational waves using pulsars
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Tests of theories of gravity
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Chile March 6-11, 2011 7 Thomas Tauris, Bonn
1669 radio pulsars
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Chile March 6-11, 2011 Thomas Tauris, Bonn
Characteristics of a binary millisecond pulsar (BMSP):
• Rapid spin: Pspin < 50 ms• Small period derivative: dP/dt < 10-18 s s-1
Ingridients needed for spin-up:
• Increase of spin ang. mom.• Decrease of period derivative
Solution:
• Accretion of mass
PPR
IcB
NS
NS 62
3
8
3
21
4
B cv B B
t
Geppert & Urpin (1994); Konar & Bhattacharya (1997) Magnetic-dipole model
* * * * A
dN J I M GM r
dt
Lamb, Pethick & Pines (1973)Ghosh & Lamb (1979, 1992)
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Formation of a BMSP
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Thomas Tauris, Bonn
LMXB cartoon
LMXB
white dwarfmillisecond pulsar
supernova
common envelope
helium star
ZAMS
Roche-lobe overflow
neutron star
+ spiral-in
15.0 1.6
3.99 1.6
1.3 1.6
1.6 0.303
1200 days 0.0 Myr
ageP orb
1538 days 13.87 Myr
0.83 days 13.87 Myr
13.1 1.6
4.86
1.10 days 14.95 Myr
80.75 days 15 Myr
1.3 1.59558 days 2.39 Gyr
4.11 days 2.29 Gyr
eccentricity: 0.93
eccentricity: 0.0
eccentricity: 0.0
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LMXB cartoon
Accretion ?super-Eddington ?
jet ?
B-field, spin ?
Stability ?response of donor star ?
response of Roche-lobe ?
dynamically stable ?
Mode of mass loss ?specific orbital angular momentum ?
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22
2
ln
ln
ln
ln
M
R
M
R LLdonor
Stability criteria for mass transfer
exponents of radius to mass: MR
adiabatic or thermal response of the donor star to mass loss
initial stability criteria: donorL
2
22
22
2 M
MR
t
RR donorM
2
2
2 M
MR
t
RR LLM
LL
nuclear burning tidal spin-orbit couplingsgravitational wave radiation
LRR 2 yields mass loss rate!
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Stability criteria for mass transfer II - Isotropic re-emission model
Orbital evolution: )0(ln
ln 2
q
M
Mq
q
a
NS
000,||
||max
2
2
M
MM Edd
orbit widens (a>0)
orbit shrinks (a<0)
heavy donor
light donor
unstable ?
(Tauris & Savonije 1999, 2001)
Chile March 6-11, 2011 16 Thomas Tauris, Bonn
1 171.28
4q
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The Orbital Angular Momentum Balance Equation
orbital angular momentum2221 1 eaM
MMJorb
orb
ml
orb
ls
orb
mb
orb
gwr
orb
orb
J
J
J
J
J
J
J
J
J
J
|| prJorb
logarithmic differentiation
(e=0, tidal circularization)
M
MM
M
M
M
M
J
J
a
a
orb
orb 21
2
2
1
1 222
2
2
22
1
)1(
M
M
q
J
J
orb
ml
Chile March 6-11, 2011 17 Thomas Tauris, Bonn
0 0 0 0
2 2(1 )3 2
(1 )2( 1)
11 1
1 1ls
a q q q
a q q q
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Chile March 6-11, 2011 18 Thomas Tauris, Bonn
LMXB bifircation period
1bifP day
Porb < Pbif:→ LMXB shorten their orbital period
Donor star still on main sequenceRLO driven by loss of Jorb (gwr, mb)
”Black widow” millisecond pulsars:
.10 0.1orb compP hrs M M
Evaporation → single millisecond pulsars
Tutukov et al. (1985)Pylyser & Savonije (1988, 1989)Ma & Li (2009)
Lazaridis, Verbiest, Tauris, et al. (2011)
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LMXB → BMSPs with He-WD
Formation of BMSPs with He-WD:
1
0.18 0.46
orb
WD
P day
M M
Unique relation between Porb and MWD
Savonije (1987)Joss, Rappaport & Lewis (1987)Rappaport et al. (1995)Tauris & Savonije (1999)
Porb > Pbif:→ LMXB widen their orbital period
Donor star is a (sub)giantRLO driven by nuclear expansion
/
5
1 / 4.50
0.1201.2 10
orb daysWDPM
M
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Orbital period – white dwarf mass correlation
• On the red giant branch (hydrogen shell burning) the growth of the degenerate core mass
is directly related to the luminosity of the star
• Temperature is almost constant on the Hyashi track L R2
• Hence there is a relation between Mcore and R
• The donor star fills its Roche-lobe during the mass transfer R is correlated with Porb
correlation between (Porb , MWD )
2 44 effL R T
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Detailed evolution of LMXBsTauris & Savonije (1999)- formation of MSPs
super-Eddington
sub-Eddington
Dt = 200 Myr
1.30 oM1.60 oM
0.29 o.M 2.05 oM
P = 3 days
P = 39 days
..
.
Chile March 6-11, 2011 22Thomas Tauris, Bonn
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Chile March 6-11, 2011 Thomas Tauris, Bonn
At first sight the theoretical relation looks really crappy when compared withobservations……….
Orbital period – white dwarf mass correlation
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Chile March 6-11, 2011 Thomas Tauris, Bonn
The search for low-mass neutron stars Bonn March, 2011
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Chile March 6-11, 2011 Thomas Tauris, Bonn
The search for low-mass neutron stars Bonn March, 2011
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Chile March 6-11, 2011 Thomas Tauris, Bonn
At first sight the theoretical relation looks really crappy when compared withobservations……….
But for each individual binary one must take into account:1) Unknown orbital inclination angle2) The mass of the pulsar (not always 1.35 Msun -- LMXBs allow for accretion!)
Orbital period – white dwarf mass correlation
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Chile March 6-11, 2011 Thomas Tauris, Bonn
The search for low-mass neutron stars Bonn March, 2011
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Chile March 6-11, 2011 Thomas Tauris, Bonn
The search for low-mass neutron stars Bonn March, 2011
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Chile March 6-11, 2011 Thomas Tauris, Bonn
The search for low-mass neutron stars Bonn March, 2011
Some uncertainties and broad scatter is expectedin the correlation, e.g. from- core convective overshooting- mixing length- chemical composition of the donor star
No problem!!
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IMXB case C (B) RLO → BMSPs with CO/ONeMg-WDvia Common Envelope and spiral-in phase
Dynamically unstable mass transfer if:
• deep convective envelope of donor star
(rapid expasion in response to mass loss)
• Mdonor > Maccretor
(orbit shrinks in response to mass loss)
Run-away process !
common envelope
drag force dissipation of orb. ang. mom.
+ deposition of Eorb in the envelope
Outcome:
• huge reduction of orbital separationrejection of stellar envelope
merging of NS + core
(Thorne-Zytkow object / black hole)
(NS orbiting a naked helium star)
Explain tight BMSPs, Porb < 3 days!
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Tauris, van den Heuvel & Savonije (2000)
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IMXB Early case B RLO → BMSPs with CO-WD (He-WD)
Alternative to CE-phase:- thermal timescale mass transfer- isotropic re-emission model
Cyg X-2:King & Ritter (1999)Podsiadlowski & Rappaport (2000)
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IMXB case A RLO → BMSPs with CO/He-WDPodsiadlowski, Rappaport & Pfahl (2002)Tauris, Langer & Kramer (2011a,b), Tauris & Langer (2011)
Was this pulsar born massive?
Nature of progenitor binary ?
Pulsar mass: 1.97±0.04 Mo
WD mass: 0.500±0.006 Mo
Orbital period: 8.69 days
Projected apsr: 11.29 light s
Eccentricity: 1.30±0.04 × 10-6
Inclination angle: 89.17±0.02 deg.
DM distance: 1.2 kpc
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IMXB case A
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IMXB case A: thermal + nuclear timescale mass transfer
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IMXB case A: thermal + nuclear timescale mass transfer
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WD chemical abundances
phase ABHydrogen shell burning
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Chile March 6-11, 2011 42 Thomas Tauris, Bonn
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Chile March 6-11, 2011 43 Thomas Tauris, Bonn
PSR J1614-2230 Tauris, Langer & Kramer (2011)Pulsar mass: 1.97±0.04 Mo 1.99 Mo
WD mass: 0.500±0.006 Mo 0.501 Mo
Orbital period: 8.69 days 8.67 days
Dynamical instabilities L-S interactions…
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Podsiadlowski, Rappaport & Pfahl (2002)
Chile March 6-11, 2011 44 Thomas Tauris, Bonn
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Chile March 6-11, 2011 45 Thomas Tauris, Bonn
PSR J1614-2230
Spin of the recycled pulsar?
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Chile March 6-11, 2011 46 Thomas Tauris, Bonn
PSR J1614-2230: 0.11 M
PSR J1802+2224: 0.01 M (CE)
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LMXB case B
LMXB case A
IMXB early case B
IMXB case C (CE)
case A
HMXB
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Chile March 6-11, 2011 49 Thomas Tauris, Bonn
AIC – accretion induced collapse of a white dwarf
• Theory / simulations (√)
• Attractive for GC MSPs √• Population synthesis ?• Exact outcome Pspin , B (?)
• No observational evidence †(although probably candidates…)
J. Hurley et al. (2010):”AIC route cannot be ignored”
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Chile March 6-11, 2011 50 Thomas Tauris, Bonn
Formation of millisecond pulsars
1) LMXB Porb > Pbif (case B)
2) LMXB Porb < Pbif (case A)
3) IMXB Common Envelope (case C)
4) IMXB Early case B5) IMXB Case A (PSR J1614-2230: neutron star was born massive)
5½) AIC
Great diversity in MSP zoo since discovery in 1982Challenges remain intact!