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07.02.27@apctp

Chang-Hwan Lee @

Spin of Stellar Mass Black Holes:Hypernova and BH Spin Correlation in Soft X-ray BH Binaries

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Compact Stars

• White Dwarf [M < 1.4 Msun; R=1000 km]

• Neutron Star [M < 3 Msun; R < 15 km]

• Black Holes

Density of Neutron Star

1 cm3

All buildings in Busan

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Theoretical Black Holes ?

Sun : r = 3 km

Earch : r = 9 mm

Total Nonsense !?

Einstein’s General Relativity

Light cannot escape !

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Observed (visible) Black Holes

Center of galaxies [106-109 Msun]

Black Hole Binaries (Soft X-ray Transients )

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Discovery of blackhole binaries

Discovery of X-ray Binaries

Mass accretion from a companion star to a compact object

X-rays

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Sources of Strong X-ray in the Universe

• Neutron Stars [M < 3 MSun; R <15 km]

• Black Holes

• … …

X-ray emission by accretion

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Now we believe that black holes exist !

X-ray Observations (2002 Nobel Prize)

•First Observation 1962

•First X-ray Satellite Uhuru (Dec. 1970)

•..

•Current Missions Chandra (NASA) XMM-Newton (Europe)

•Future Xeus (ESA), ……

Chandra (NASA)

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BH at the Center of a galaxy (M87)

Jet=100000 light year

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Number of X-ray Sources

1,000 50,000

1970s 1990s

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What is a black hole in real observation ?

• Souce of strong X-ray emission

• X-ray emission region is very small

• No stable star exists with given mass & size

We call it a Black Hole !

Beyond Neutron Star5-10 Msun

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Black Hole Binaries in our Galaxy

XTE J1118+480

Galactic Disk

Soft X-ray Transients

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Oscillating Brightness (GRO J1655-40)

X-ray & Optical Telescopes

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Nova Sco 94

N O Mg Si S Ti Fe

[Xi/H] 0.45

1.00

0.90 0.90

0.75

0.90

0.10

error 0.50

0.30

0.40 0.30

0.20

0.40

0.20

[Xi/H]: logarithmic abundances relative to solar

Israelial et al. 1999, Nature

m=2Msun ; MBH=6Msun

It’s impossible for normal stars!

Where did they come from?

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Abundances in the secondary of Nova Sco

Hypernova to explain the observations.

N O Mg Si S Ti Fe

[Xi/H] 0.45

1.00

0.90 0.90

0.75

0.90

0.10

error 0.50

0.30

0.40 0.30

0.20

0.40

0.20

They had to come from black hole progenitor when it exploded.

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System velocity (-106 km/s) :

Abrupt Mass Loss by Explosion

Another evidence ?

C.M.

Mg,Si,S,…

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Hypernova Explosions from Rotating BH

Spinning BH (QPOs)

High Black Hole Mass ( > 5 Msun)

--- Maximum Neutron Star Mass < 2 Msun

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Related Issues to be clarified

• Neutrinos from hypernova

• Nucleosynthesis from hypernova

• Evidences of asymmetric explosions

• Connection to GRBs

• … …

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Hypernovae in BH X-ray Binaries

We have seen it twice.

So, does it happen everywhere ?

Nova Sco, V4641 Sgr

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Q) How can we understand the population of SXTs ?

Orbital period (days)

MBH

(Msu

n)

10

15

5

1 10

Evolved companion

MS companion

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before BH

after BH

Goal : At the time BH Formation

Evolution of Donor Star

Evolution of BH Progenitor

Current Observation

Progenitors

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High Mass Black Hole progenitor (20-40 Msolar)

Bigger star evolves fast !

High Mass Black Hole is formed when the separation is large (Case C; meet at supergiant stage)

NS/LMBH is formed when the separation is relatively small (Case A, B; meet at/before red giant stage)

before BH

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Fe core mass

Neutron Star

In Close Binaries

before BH

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A

Case C

HMBHNS/

LMBHCase B

before BH

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HMBH Formation in Case C NS LMBH HMB

H

Current 1915+105 (108 Rsun)

Phase II

before BH

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Formation of Stellar Mass Black Holes

Assumption

Case C Mass Transfer (in supergiant stage of BH progenitor)

If BH formation through Case B (in giant stage) is possible, contrary to the observation, we should see about 10 times more BHs in our Galaxy.

before BH

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Rapidly Rotating Black Holes

Assumption: Synchronization of BH-Progenitor Spin & Binary Orbital Period

Rapidly rotating BH with large Kerr parameter (even close to 1)

SXTs with short orbital periods Possible sources of Hypernovae/GRB

At the time of BH Formation

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Kerr Black Holes

Marginally stable orbit

Marginally bound orbit

Inner disk can extend to RSch for a=1

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Preexplosion orbital period (days)

Kerr parameter (Lee et al. 2002)

At the time of BH Formation

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Line Profile

Doppler effect + Gravitational Redshifts

BH Spin Observation

Indication of BH spin

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Preexplosion orbital period (days)

Kerr parameter

At the time of BH Formation

4U 1543-47GRO J1655-40

Shafee et al. (2006)

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HN/GRB

Reconstructed BH Binaries at Birth

BH Spin – 10000/sec

At the time BH Formation

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Gamma Ray Bursts from Black Hole Systems

• Energy > 1051 ergs

• Rinit = O(100 km)

• M < 30 Msun

• dT = ms – min

• … …

Energy in Hypernovae = Energy in GRBs

BH Binaries -> Long-duration GRBs (> 2 sec)

Most likely BHs !

BH Binary is natural source of rapidly rotating black hole

At the time BH Formation

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Shrink

Expand

after BH

AML: Angular Mom Loss

Nu: Nuclear Burning

Evolved Companion

MS companion

I: Hubble TimeII: Main SequenceIII: Oveflow at t=0

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Current Observatio

n

after BH

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10 Msun

15 Msun

Q) How to Evolve ?

OK?

after BH

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Preexplosion orbital period (days)

Kerr parameter

4U 1543-47GRO J1655-40

GRS 1915+105P=33 daysa* > 0.98

McClintock et al. (2006)

after BH

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Q) How to form BHs in 10-15 Msun ?

problem 1: It’s hard to form BH with masses > 10 Msun from stellar evolution.

problem 2: The current separation is too large.

Problem 3:Observed Kerr parameter is too big.

easiest solution: Accrete extra mass after BH formation

after BH

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?

after BH

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Conservative Mass Transfer

2.817 daysGRS 1915+105

V4641 Sgr

Data: 33.5 days

Consistent within error range

after BH

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10 Msun

15 Msun

V4641 Sgr

1915+105

9.5 Msun + 6.5 Msun

P=3 day

14 Msun + 2 Msun

P=33 days

Beauty of Simple Physical Laws !

after BH

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Spin-up due to accretion

GRS 1915+105a* > 0.98

McClintock et al. (2006)

after BH

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Preexplosion orbital period (days)

Kerr parameter

4U 1543-47GRO J1655-40

GRS 1915+105P=33 daysa* > 0.98

after BH

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Pre-Explosion Properties

V4641 & 1915

At the time BH Formation

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HN/GRB

Reconstructed BH Binaries at Birth

BH Spin – 10000/sec

At the time BH Formation

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Conclusions

• Soft X-ray BH binaries Formation and evolution :

- only “Case C mass transfer” can explain HMBH in binaries.

Spin of stellar-mass BHs :- tidal (BH progenitor spin-orbit) interaction is consistent with the current BH spin observation

Long-time scale GRBs and Hypernovae :- Short orbital period ( P<0.5 day) HMBH binaries are the sources of long-duration GRBs and Hypernovae

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Gamma-Ray Burst

Duration: milli sec - min

1970s : Vela Satellite

1990s: CGRO, Beppo-SAX

2000s: HETE-II, Swift

Motivations

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Motivations

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Galactic ?

Motivations

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Motivations

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Gamma-Ray Bursts are the brightest events in the Universe.

During their peak, they emit more energy than all the stars and galaxies in the Universe combined !

Motivations

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Two groups of GRBs

Short Hard Gamma-ray Bursts:Duration time < 2 secNS-NS, NS-LMBH mergers

Long-duration Gamma-ray Bursts:from spinning HMBH

HMBH (High-mass black hole)

5-10 solar mass

Motivations

52Science 308 (2005) 939

Short-Hard Gamma-ray Burst : Colliding NS binaries

Very Important for Gravitational Waves, too

Motivations

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Long-duration GRBs: Afterglow

Host Galaxy Association

= Distance Estimation

Motivations

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GRB/Supernova Association

Afterglow

GRB980425 SN1998bw

GRB030329/Supernova Association

(z=0.2: closest GRB/Afterglow)

Top 10 Scientific Achievement in 2003 [New York Times]

Nature 423 (2003), 843, 844, 847

Motivations

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What caused GRB/Supernova ?

Most-likely Black Holes

Callapsar: Asymmetric Explosion of a Massive Star Most-likely Rapid-Rotation

Motivations

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How to form rapidly spinning black holes?

Most likely in binaries (Soft X-ray Transients)

Motivations

Companion star can keep the BH progenitor rotating

Formation of rapidly rotating stellar mass BHs