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Department of Physics and Astronomy. Formation of Double Neutron Stars: Kicks and Tilts. Vicky Kalogera. with Bart Willems Mike Henninger. In this talk …. Pulsars and Recycling Double Neutron Star Formation The Double Pulsar PSR J0737-3039 Evolution constraints

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slide1
Department of Physics and Astronomy

Formation of Double Neutron Stars:

Kicks and Tilts

Vicky Kalogera

with

Bart Willems

Mike Henninger

slide2
In this talk …
  • Pulsars and Recycling
  • Double Neutron Star Formation
  • The Double Pulsar PSR J0737-3039
    • Evolution constraints
    • Kinematics constraints
    • Expected kicks and spin tilts
  • PSR B1913+16 and B1534+12
pulsars
Highly magnetized rapidly rotating neutron stars whose magnetic field axis is inclined with respect to their rotation axis lighthouse effect

Spin period of a few seconds

Spin-down time scale of a few 10-100Myr

Pulsars

http://imagine.gsfc.nasa.gov/docs/science/know_l1/pulsars.html

millisecond pulsars
Magnetic field: ~ 109-1010 G

Spin period: < 100ms

Spin-down time scale: ~ 100Gyr

Old neutron stars which are recycled (spun-up) by mass accretion and the associated transport of angular momentum from a close binary companion

Millisecond Pulsars

http://chandra.harvard.edu/resources/illustrations/blackholes2.html

slide5
NS-NS Formation Channel

from Tauris & van den Heuvel 2003

How do Double

Neutron Stars

form ?

current properties

constrain NS #2

formation process:

  • NS kick
  • NS progenitor
slide6
NS-NS Formation Channel

animation credit:

John Rowe

psr j0737 3039 properties
Component A 23 ms pulsar

fastest known DNS pulsar spin

Orbital period 2.4 hours

closest known DNS orbit

Eccentricity 0.09

least eccentric of all known DNS binaries

Periastron advance 16.9° per year

fastest of all known DNS binaries

PSR J0737-3039 Properties

Burgay et al. 2003

psr j0737 3039 properties1
Coalescence time 85 Myr

shortest of all known DNS binaries

Drastic increase by a factor of 6-7

in estimates for gravitational wave detections

by ground-based interferometers

PSR J0737-3039 Properties

Kalogera et al. 2004

psr j0737 3039 properties2
Component B 2.8s pulsar

FIRST known DOUBLE PULSAR system!

Inclination close to 90° eclipses

unique probe into magnetospheric physics

PSR J0737-3039 Properties

Lyne et al. 2004

Remarkable progenitor constraints

next … Willems & VK 2004

Willems, VK, Henninger 2004

derivation of progenitor constraints
Post-SN orbital separation (A) and eccentricity (e) evolve due to Gravitational Radiation

equations for dA/dt and de/dt need to be integrated backwards in time what is the age of PSR J0737-3039?

2) Pre- and post-SN orbital parameters are related by conservation laws of orbital energy and orbital angular momentum

3) Constraints arise from requiring physically acceptable solutions M0-A0 diagram

Derivation of Progenitor Constraints
orbital evolution backwards in time
Orbital Evolution Backwards in Time

Gravitational Radiation: dA/dt & de/dt

Orbital separation

Orbital eccentricity

A = 1.54 R⊙

e = 0.119

the pre sn orbital separation
The Pre-SN Orbital Separation

Evolution of A(1-e) ≤ A0≤ A(1+e) back in time

the pre sn orbital separation1
The Pre-SN Orbital Separation

Evolution of A(1-e) ≤ A0≤ A(1+e) back in time

the pre sn orbital separation2
The Pre-SN Orbital Separation

Evolution of A(1-e) ≤ A0≤ A(1+e) back in time

the pre sn orbital separation3
The Pre-SN Orbital Separation

Evolution of A(1-e) ≤ A0≤ A(1+e) back in time

detached vs semi detached pre sn binary
If left alone, a helium star of mass M0 will reach a maximum radius R0,max(M0)

For a given companion mass, the size of the helium star's critical Roche lobe is determined by the orbital separation and the helium star mass RL(M0,A0)

R0,max(M0) > RL(M0,A0): detached A0 > A0,crit(M0)

Detached vs. Semi-Detached Pre-SN Binary
the progenitor mass of the last born ns
The relations between the pre- and post-SN orbital parameters (conservation laws of orbital energy and orbital angular momentum) have REAL solutions only if M0≤ M0,max( A , e , A0 , Vk )

For a given age (i.e. fixed A and e), the upper limit M0,max(A0) can be determined for every admissible value of the kick velocity Vk

The Progenitor Mass of the Last-Born NS

age dependency

the progenitor mass of the last born ns1
A(1-e) < A0 < A(1+e)

Detached: A0 > A0,crit(M0)

Mass transfer:

A0≤ A0,crit(M0)

M0≤ M0,max(A0,Vk) for age of 100Myr

The Progenitor Mass of the Last-Born NS
the helium star progenitor mass revisited
Lower limit: the helium star must form a NEUTRON STAR rather than a WHITE DWARF

M0≥ 2.1Mo(Habets 1986)

Upper limit: the binary mass ratio cannot be too extreme if runaway mass transfer leading to a merger is to be avoided

M0/MNS≤ 3.5 (Ivanova et al. 2003)

M0≤ 4.7Mo

The Helium Star Progenitor Mass Revisited
a 1 e a 0 a 1 e m 0 2 1m o m 0 4 7m o m 0 m 0 max a 0 v k for age of 0myr
A(1-e) < A0 < A(1+e)

M0≥ 2.1Mo

M0≤ 4.7Mo

M0≤ M0,max(A0,Vk) for age of 0Myr

The Minimum Kick Velocity
a 1 e a 0 a 1 e m 0 2 1m o m 0 4 7m o m 0 m 0 max a 0 v k for age of 100myr
A(1-e) < A0 < A(1+e)

M0≥ 2.1Mo

M0≤ 4.7Mo

M0≤ M0,max(A0,Vk) for age of 100Myr

The Minimum Kick Velocity
the maximum kick velocity
An upper limit on the magnitude of the kick velocity is set by the requirement that the binary must remain bound after the SN explosion

depends on constraints on pre-SN orbital separation and helium star mass

for 1.15Ro≤ A0≤ 1.72Roand 2.1Mo≤ M0≤ 4.7Mo the maximum possible kick velocity is 1660km/s

The Maximum Kick Velocity
conclusions
PSR J0737-3039

Pulsar B's helium star progenitor is most likely transferring mass to the first-born NS

NS progenitor mass: 2 Mo ≤ M0 ≤ 4.7 Mo

Kick magnitude: 60 km/s ≤ Vk≤ 1660 km/s

Conclusions
polar angle between pre sn orbital velocity v 0 and kick velocity v k
polar angle between pre-SN orbital velocity V0 and kick velocity VkThe Kick Direction

0

Kalogera (2000)

NS1

azimuthal angle in plane ^ to V0

given a kick velocity v k real solutions for a finite number of kick directions
Given a kick velocity Vk :

REAL solutions for a finite number of kick directions

The Kick Direction

Vk = 200km/s

Vk = 500km/s

the kick direction
The Kick Direction

Kick is generally directed

opposite to the orbital motion

Regardless of

Vk and age:

q > 115°

slide31
For a given kick velocity Vk :

M0 and A0 constraints translate to polar angle constraints

Isotropic Kicks

Bayes' theorem

Isotropic Kicks

Vk

M1≤ M0≤ M2

A1≤ A0≤ A2

q1≤q≤q2

f1≤ f≤f2

conclusions1
PSR J0737-3039

Pulsar B's helium star progenitor is most likely transferring mass to the first-born NS

NS progenitor mass: 2 Mo ≤ M0 ≤ 4.7 Mo

Kick magnitude: 60 km/s ≤ Vk≤ 1660 km/s

most probable: 150 km/s

Kick direction: 115°≤q≤ 180°

Conclusions
psr j0737 3039 evolutionary kinematic history
PSR J0737-3039

Evolutionary + Kinematic History

systemic velocity of psr j0737 3039
Ransom et al. 2004 :

PSR J0737-3039: Vtransverse≈ 140 km/s

from scintillation observations

But... unknown orientation in the plane of the sky!

and unknown radial velocity …

Systemic Velocity of PSR J0737-3039
beyond the evolutionary constraints
So far all constraints from stellar and binary evolution

However... the DNS center-of-mass may receive a significant kick:

mass loss + supernova kick

but... current velocity ≠ post-SN velocity must trace Galactic motion back in time to birth place

where was the system born? what is its current 3D space velocity?

Beyond the Evolutionary Constraints
birth sites of double neutron stars
DNS binaries form from massive primordial binaries vertical scale height of 50-70 pc

Center-of-mass kick imparted at first SN:

~ a few 10 km/s (Brandt & Podsiadlowski 95, Wex et al. 00, Pfahl et al. 02)

the system is probably still close to the Galactic plane when the second NS is formed

We assume that the DNS was born in the Galactic disk

Birth Sites of Double Neutron Stars
proper motion
Proper Motion

Velocity components in R.A. and Decl.

Proper motion of 100mas/yr should be detectable in less than 17 months

for d = 0.6 kpc

Determination of the proper motion will considerably constrain W

Solid: Va Dashed: Vd

motion of the system backwards in time depends on
Motion of the system backwards in time depends on Galactic Motion

the unknown longitude of the ascending node W

(direction of Vtransverse)

AND

the unknown radial velocity Vr

2 unknown parameters

many possible trajectories

derivation of progenitor constraints ii
For each W [0 , 360] and Vr [-1500 , 1500] km/s

Trace the motion back in time to a maximum age of 100Myr

Each crossing of the trajectory with the Galactic plane is considered a possible birth site

The times of the plane crossings yield kinematic age estimates

Post-SN peculiar velocity at birth =

total systemic velocity - local Galactic rotational velocity

Combine with stellar and binary evolution constraints

Derivation of Progenitor Constraints II
kinematic ages
Kinematic Ages

The system may have crossed the disk up to 3 times in the last 100Myr

1st crossing

There is a wide range of W and Vr values for which the system is < 20Myr old

2nd crossing

For ages > 20Myr disk crossings only occur for tight ranges of W and Vr

If the system crossed the Galactic plane twice it is at least 20Myr old

post sn peculiar velocities
Post-SN Peculiar Velocities

1st crossing

1st crossing:

90km/s ≤ Vpec≤ 1550km/s

2nd crossing

2nd crossing:

120km/s ≤ Vpec≤ 800km/s

Vpec generally increases with increasing Vr

isotropic kicks bayes theorem
Isotropic Kicks

+

Bayes' theorem

Kick Velocity Distribution

For a each value of W and Vr

Vk

M1≤ M0≤ M2

A1≤ A0≤ A2

q1≤q≤q2

f1≤ f≤f2

Average over all W assuming a uniform distribution

kick velocity distribution for isotropic kicks
Kick Velocity Distribution for Isotropic Kicks

1st crossing

1st crossing

2nd crossing

2nd crossing

spin orbit misalignment
Mass transfer spinning up pulsar A: expected to align pulsar A's spin axis with the pre-SN orbital angular momentum axis

Kick: the post-SN orbit is inclined w/r to the pre-SN orbit

Pulsar A's spin axis misaligned w/r to post-SN orbital angular momentum axis

The misalignment angle l depends only on q not on f

Distribution functions for the misalignment angle are derived in a similar way as the kick velocity distributions

Spin-Orbit Misalignment
spin tilt distribution for isotropic kicks
Spin Tilt Distribution for Isotropic Kicks

1st crossing

1st crossing

2nd crossing

2nd crossing

non isotropic kicks
Recent observations of the Crab and Vela pulsars suggest a possible alignment between the projected proper motion and spin axis

(Lai et al. 2001, Romani 2004)

Spin-kick alignment?

Non-Isotropic Kicks

Crab Pulsar Chandra X-ray image

http://chandra.harvard.edu/photo/2002/0052/index.html

non isotropic kicks1
Non-Isotropic Kicks

x = angle between pre-SN orbital angular momentum and kick velocity

Planar kicks: x≈ 90°

Polar kicks: x ≈ 0° or x ≈ 180°

kick velocity distribution for polar kicks
Kick Velocity Distribution for Polar Kicks

Misalignment angle x≤ 30°

1st crossing

1st crossing

2nd crossing

2nd crossing

spin tilt distribution for polar kicks
Spin Tilt Distribution for Polar Kicks

Misalignment angle x≤ 30°

1st crossing

1st crossing

2nd crossing

2nd crossing

conclusions2
PSR J0737-3039

Pulsar B's helium star progenitor is most likely transferring mass to the first-born NS

NS progenitor mass: 2 Mo ≤ M0 ≤ 4.7 Mo

Kick magnitude: 60 km/s ≤ Vk≤ 1660 km/s

most probable: 150 km/s

Kick direction: 115°≤q≤ 180° and 25°≤x≤ 155°

Kicks are directed opposite to orbital motion and cannot be too closely aligned with the pre-SN orbital angular momentum

Tilt angles below 30°-50° are favored for Vr< 500 km/s

Conclusions
psr b1534 12 properties
Wolszczan 1991; Stairs et al. 2002; Konacki et al. 2003; Arzoumanian et al. 1999

Spin period 37.90 ms

Orbital period 10.1 hours

Eccentricity 0.274

Periastron advance 1.76° per year

Proper motion ma = 1.34 mas/yr

md = -25.05 mas/yr

Spin-down age 210 Myr

PSR B1534+12 Properties

Kinematic history depends on only 1 unknown quantity: radial velocity Vr

progenitor constraints
Progenitor Constraints

Red: detached Blue: mass transfer

3rd crossing

1st crossing

2nd crossing

Detached as well as semi-detached solutions

kick constraints
Kick Constraints

1st crossing

2nd crossing

3rd crossing

Red: detached Blue: mass transfer

kick velocity distribution for isotropic kicks1
Kick Velocity Distribution for Isotropic Kicks

1st crossing

1st crossing

2nd crossing

2nd crossing

3rd crossing

3rd crossing

spin tilt distribution for isotropic kicks1
Spin Tilt Distribution for Isotropic Kicks

1st crossing

1st crossing

2nd crossing

2nd crossing

3rd crossing

3rd crossing

psr b1913 16 properties
Hulse & Taylor 1975; Taylor et al. 1976, 1979; Taylor & Weisberg 1982, 1989; Damour & Taylor 1991; Arzoumanian et al. 1999

Spin period 59.03 ms

Orbital period 7.75 hours

Eccentricity 0.617

Periastron advance 4.23° per year

Proper motion ma = -3.27 mas/yr

md = -1.04 mas/yr

Spin-down age 80 Myr

PSR B1913+16 Properties

Kinematic history depends on only 1 unknown quantity: radial velocity Vr

+ ...

psr b1913 16 properties1
Hulse & Taylor 1975; Taylor et al. 1976, 1979; Taylor & Weisberg 1982, 1989; Damour & Taylor 1991; Arzoumanian et al. 1999

Spin period 59.03 ms

Orbital period 7.75 hours

Eccentricity 0.617

Periastron advance 4.23° per year

Proper motion ma = -3.27 mas/yr

md = -1.04 mas/yr

Spin-down age 80 Myr

PSR B1913+16 Properties

Kinematic history depends on only 1 unknown quantity: radial velocity Vr

+ ...

Measured spin tilt around 18° or 162°

progenitor constraints1
Progenitor Constraints

Red: detached Blue: mass transfer

1st crossing

2nd crossing

l = 162°

l = 18°

l = 162°

l = 18°

Detached as well as semi-detached solutions

kick constraints1
Kick Constraints

1st crossing

2nd crossing

l = 18°

l = 162°

l = 18°

l = 162°

Red: detached Blue: mass transfer

kick velocity distribution for isotropic kicks2
Kick Velocity Distribution for Isotropic Kicks

1st crossing

1st crossing

2nd crossing

2nd crossing

conclusions3
PSR J0737-3039

Pulsar B's helium star progenitor is most likely transferring mass to the first-born NS

NS Progenitor mass: 2Mo≤ M0≤ 4.7 Mo

Kick magnitude: 60 km/s ≤ Vk≤ 1660 km/s

most probable: 150 km/s

Kick direction: 115°≤q≤ 180° and 25°≤x≤ 155°

Tilt angles below 30°-50° are favored for Vr< 500 km/s

PSR J0737-3039, PSR B1534+12 and PSR 1913+16

Kicks are directed opposite to orbital motion and cannot be too closely aligned with the pre-SN orbital angular momentum

Conclusions
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