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Neutron Star Mass Distribution in Binaries
A Tribute to [email protected]
Chang-Hwan Lee @
1
Sabbatical Year@Stony Brook (2013.8~2014.8)
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The Future
The Life
The Science
Gerry’s Three Questions
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4
20 years with Gerry since 1992
1st paper : Kaon condensation in `nuclear star` matter
Lee, Brown, Rho (PLB 335, 266, 1994)
… …
14th paper: Discovery of Black Hole Mass-Period Correlation in
Soft X-ray Transients and its implication for GRB and
Hypernova mechanisms
Lee, Brown, Wijers (ApJ 575, 996, 2002)
… …
34th paper: Kerr parameters for stellar mass black holes and their
consequences for GRBs and hypernovae
Moreno Mendez, Brown, Lee, Walter (ApJ 727:29, 2011)
1996~2000@Stony Brook
34 papers with Gerry
IAS@1998
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Prakash (2013)
All well measured NS masses in
NS-NS binaries are < 1.5 Msun
5
Gerry’s favorite
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1.97 & 2.01 Msun NS were observed in NS-WD binaries
Why all well-measured NS masses in NS-NS binaries are less than
1.5 Msun?
NS mass may/should depend on the evolution process
High-mass neutron stars in NS-White Dwarf binaries
1.97 solar mass NS : Nature 467 (2010) 1081
2.01 solar mass NS : Science 340 (2013) 6131
Our open questions
6
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In 2007
we discussed that NS masses in NS-NS binaries may be the result
of evolution, not an indication of maximum NS mass.
Gerry accepted the possibility that the maximum mass of NS can
be significantly higher than 1.5 solar mass.
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Contents
Part I : What we discovered in BH binaries
Part II : What if we apply the same evolution process
to neutron star binaries ?
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Part I. What we discovered in BH binaries
Collection of Gerry’s
contributions to Astrophysics
until 2002
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Black Hole Binaries (Soft X-ray Transients)
MB
H (M
sun)
Orbital period (days)
Main Sequence companion Evolved companion
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Q3) Evolution of Donor Star
Q1) Evolution of BH/NS Progenitor
Current Observation
Progenitors
Q2) What happens at birth ?
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Q) How can we understand
the population of SXTs ?
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Tidal interaction just before BH formation
rapidly
spinning BH
Fe
Synchronization of
BH-Progenitor Spin & Binary Orbital Period
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Reconstructed BH Binaries at Birth
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Pre-explosion orbital period (days)
Rapidly spinning black holes at birth
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Pre-explosion orbital period (days)
Rapidly spinning black holes at birth
4U 1543-47
GRO J1655-40
Shafee et al. (2006)
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Evolution after BH formation
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GRS 1915+105
Low-spin black holes at birth
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Spin-up due to conservative
accretion
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McClintock et al. (2006)
Pre-explosion orbital period (days)
GRS 1915+105
a* > 0.98
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Gerry’s last paper
by Enrique Moreno Mendez, Brown, Lee, Walter (ApJ 727:29)
submitted 2009 May 11, accepted 2010 Nov 8, published 2011 Jan
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What if we apply the same evolution process to neutron
star binaries ?
Supercritical accretion in NS binaries
Possibilities of `NS + high-mass NS/BH` binaries
Part II
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Supercritical Accretion onto first-born NS
Eddington Accretion Rate : photon pressure balances the gravitation
attraction
If this limit holds, neutron star cannot be formed from the beginning
(e.g. SN1987A; 108
Eddington Limit).
Neutrinos can take the pressure out of the system
allowing the supercritical accretion when accretion rate
is bigger than 104 Eddington limit !
(T > 1 MeV : Thermal neutrinos dominates !)
Q) What is the implications of supercritical accretion, if it works ?
[Lee,Park,Brown, ApJ 670,741(2007)]
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Fresh NS mass from Fe core collapse
In close binaries (evolution without H envelope)
low Fe core mass NS mass = 1.3 - 1.5 Msun
This value is independent of NS equation of state.
Q) What is the fate of primary (first-born) NS in binaries ?
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Final fate of first-born NS
Evolution of
Companion
1st-born NS
NS + accretion
He
Accretion
Fe2nd
NS/WD
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NS
NSA
BLife time
He
H
H
He
Case 1
A
B
No accretion : nearly equal mass NS-NS binary!
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H red giantHe red giant
NS
NSA
B
Life time
He
+0.2 Msun
First born NS should accrete only < 0.2 M⊙ !
H
Case 2
A
B
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H red giant He red giant
WD
NS
90% 10%
A
B
Life time
H He He
+0.7 Msun +0.2 Msun
Supercritical Accretion: First born NS can accrete up to 0.9 M⊙ !
Case 3
A
B
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Possibilities of `NS + high-mass NS/BH` binaries
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Final mass of first-born NS with supercritical accretion
Fin
al m
ass
of 1
st-b
orn
NS
Original mass of 2nd star
NS + NS
without accretion
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seen
Q) maximum NS mass ?
seen
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Can we see BH-NS binaries as pulsars even if they exist ?
Pulsar life time : 1/B
Fresh pulsar : B∼1012 G
NS-NS
if first-born NS is recycled by accretion
longer pulsar life time (B∼108 G) larger beaming angle
bigger chances to be observed
BH-NS
no recycled pulsar
much smaller chances to be observed
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GW sources with NS
NS-NS
– already seen
NS-BH
– no evidence yet
– can contribute to GW if exist
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Consequences of supercritical accretion, if it works
different class of NS binaries may exist
high mass NS/BH ( > 2 solar mass) + typical NS
could be hidden GW sources
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2006
Fly with Eagles
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?
Gerry’s contribution to my HR diagram ?
?
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I really enjoyed working
with Gerry
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