Gravitational Waves from Newborn Magnetars - IN2P3moriond.in2p3.fr/J07/trans/friday/stella.pdfGravitational Waves from Newborn Magnetars Luigi Stella ... whole Virgo Cluster, ... Persistent

Gravitational Waves from Newborn MagnetarsLuigi Stella – INAF – Rome

- Magnetars are neutron stars that are powered by the decay of theirvery high magnetic field

- Fast rotating (i.e. newborn) magnetars can be powerful GW sources,because of the star deformation induced by the magnetic field

- Two classes of high energy sources contain magnetars- If their field is B~1015 Gauss, GWs can be detected with Advanced

LIGO class instruments only from the Galaxy, where the birth rate is ~1 magnetar/1000 yr

There is now astrophysical evidence that magnetars have B>1016 Gauss:

GWs from newborn magnetars can be detectable from the whole Virgo Cluster, where their birth rate is >1 magnetar/yr

Newborn Magnetars are interesting GW sources for Advanced LIGO class instruments

Neutron Stars

- Radio Pulsars (rotation power) B ~ 108-1013 Gauss P(spin) ~ 1.5 ms – 8 s

- Accreting neutron stars (accretion power) B ~ 108-1013 Gauss P(spin) ~ 1.5 ms – 2000 s

Superstrong B-fields ?: a bit of history

- B~ 1014-1015 G from magnetic flux conservation in progenitor star(Woltjer 1964)

Radio Pulsars: B ~ 108-1013 G Accreting X-ray pulsars: B ~ 108-1013 G

- Superstrong B-fields to cause outflows in stellar collapse ?

- Strong toroidal field as a residual of differential rotation at birth ?

- Superstrong B-fields from dynamo action in proto-neutron star (+ magnetic energy dissipation !) Modern idea of Magnetar (Duncan & Thompson 1992 -> ) (developed also in connection with GRBs)

Two classes of high energy sources contain magnetars

Soft Gamma Repeaters Anomalous X-ray Pulsars SGRs (1987) AXPs (1995)

• No. of sources 5+1 8+1

• Spin Period 5-8 s 6-12 s

• Period Derivative ~10-11 s/s ~10-11-5x10-13 s/s

• Recurrent Bursts ~1038-1041 erg/s ~1037-1038 erg/s

• Giant Flares yes no

• Persistent emission ~1035 erg/s ~1034-1035 erg/s

• Association to SNRs ? in some cases

• Radio pulsations no in 1 case

Two classes of high energy sources contain magnetars

Soft Gamma Repeaters Anomalous X-ray Pulsars SGRs (1987) AXPs (1995)

• No. of sources 5+1 8+1

• Spin Period 5-8 s 6-12 s

• Period Derivative ~10-11 s/s ~10-11-5x10-13 s/s

• Recurrent Bursts ~1038-1041 erg/s ~1037-1038 erg/s

• Giant Flares yes no

• Persistent emission ~1035 erg/s ~1034-1035 erg/s

• Association to SNRs ? in some cases

• Radio pulsations no in 1 case

SGR Bursts

- Concentrated in time (“outbursts”)- Relatively simple profiles (faster rise than decay)- Broad distribution of wait times (~7 decades) : similar to that of

earthquakes; no waiting-time correlations- Energy distribution dN/dE ~ E-5/3 : similar to earthquakes- Most bursts release ~1038-1041 ergs

Two classes of high energy sources contain magnetars

Soft Gamma Repeaters Anomalous X-ray Pulsars SGRs (1987) AXPs (1995)

• No. of sources 5+1 8+1

• Spin Period 5-8 s 6-12 s

• Period Derivative ~10-11 s/s ~10-11-5x10-13 s/s

• Recurrent Bursts ~1038-1041 erg/s ~1037-1038 erg/s

• Giant Flares yes no

• Persistent emission ~1035 erg/s ~1034-1035 erg/s

• Association to SNRs ? in some cases

• Radio pulsations no in 1 case

Giant Flares

- 1979 March 5 from SGR 0526−66: energy released ~1044 ergs- 1998 August 27 from SGR1900+14: energy released ~1044 ergs- Main peak ~0.2 s; variability down to ms, hard BB-like spectrum (kT~ 100 keV)- 2-3 min long ringing tail: (nearly) exponential decay pulsations at 5-8 s (spin period) TB temperature of ~30-50 keV.- In Magnetar model: GFs due to large scale rearrangements of core B-field

Two classes of high energy sources contain magnetars

Soft Gamma Repeaters Anomalous X-ray Pulsars SGRs (1987) AXPs (1995)

• No. of sources 5+1 8+1

• Spin Period 5-8 s 6-12 s

• Period Derivative ~10-11 s/s ~10-11-5x10-13 s/s

• Recurrent Bursts ~1038-1041 erg/s ~1037-1038 erg/s

• Giant Flares yes no

• Persistent emission ~1035 erg/s ~1034-1035 erg/s

• Association to SNRs ? in some cases

• Radio pulsations no in 1 case

Magnetars: Neutron Stars powered by magnetic energy

- “Magnetars” (MAGNEtic sTARS): neutron stars with very high magnetic fields (B>1014G) Why magnetic energy ? (Magnetic energy propagating through fractures in the crust)

Persistent luminosity 10-100 times higher than spin down power -> rotational energy ruled out Recurrent flares reach 1041 erg/s ~ 1000 LEdd , giant flares 1044 erg/s ~ 106 LEdd -> accretion energy ruled out

Fast spin (few ms) and differential rotation generate

internal toroidal field B > 1015 G

Rotational energy losses are orders of magnitudes smaller (1032-33erg/s) than observed Lx!!

Persistent X-ray emission of AXPs

Erot=IΩΩ=4π2PP-3 . . .

The B-field of Magnetars

Very strong internal B-fields in a newborn differentially rotating fast-spinning neutron star

For initial spin periods of Pi~1–2 ms, differential rotation can store ~1052(Pi/1 ms)2 ergs,that can be converted into a magnetic field of up to 3x1017 (Pi/1ms)-1 G.(efficient dynamo might be limited to ~3x1016 G) (Duncan & Thompson1992)

BdBt

Bd ~ 1014-15 G outer dipole field (spin-down, pulsations) inferred from spin-down rate (and confirmed through the energetics of the “ringing tail” of Giant Flares from SGRs)

Bt > 1015 G inner toroidal field (energy reservoir): lower limit from: L(persistent) x age ~ 1047 ergs

Fast spin (few ms) and differential rotation generate

internal toroidal field B > 1015 G

SGR 1806-20: Giant Flare of 2004 Dec 27

(Mereghetti et al. 2005)

(Palmer et al. 2005 Hurley et al. 2005)

Moon reverberation seen !

Shape of a highy magnetic star

Star with a constant inner B-field cannot be spherical(Chandrasekhar & Fermi 1953)

Poloidal inner B-field : Oblate star

Toroidal Innar B-field : Prolate star

Magnetically induced distortion and gravitational wave emission

-An old idea, considered mainly in relation to young fast radio pulsars such as the Crab (e.g. review by Cutler & Thorne2002)-Renewed interest in highly magnetic (~1014-1015 G) newly formed neutron star in our Galaxy.

Problem: expected recurrence times are long (> 100 yr at the best) (e.g. review by Bonazzola & Marck 1994)- Detailed studies of gravitational wave emission properties (Gourgoulhon & Bonazzola 1996, Konno 2001, and early evolution (Cutler 2002) Palomba 2001 )

- Toroidal inner field: prolate shape with ellipticity -6.4x10-4 (Bt/1016.3 G)2

-Symmetry axis of deformed star, in general, not (exactly) coaligned with the spin axis:

Viscous damping of free precession leads to an orthogonal rotator within ~1 day from birth

spin spin

Bt

Bt

The 2004 Dec 27 Event and the Internal B-field of Magnetars- Energy of ~ 5x 1046 ergs released in initial 0.6 s long spike (Terasawa et al. 2005; Hurley et al. 2005)

- 1 such event in ~30 yr of monitoring of 5 SGRs -> Recurrence time ~ 150 yr/magnetar

- Events this powerful would be detectable within tens of Mpc: If no events seen -> Recurrence time 4-20 times longer (Lazzati et al. 2005; Popov & Stern 2005)

Did we observe a very unlikely event ? Or are there unknown selection effects at work ?

The 2004 Dec 27 event would have been seen no matter what ! Evaluate the chances of long recurrence times, given the observation of the 2004 Dec 27 event:

-> Prob. that recurrence time is > 600 yr : 10-3

- ~70 events like the 2004 Dec 27 event expected in ~104 yr (SGR lifetime) -> Total energy release (independent of beaming) ~4x1048 ergs

If internal field is the energy source, then B > 1015.7 G

Including total neutrino energy release: B > 1015.9 G New limit on Bt

Gravitational Wave Emission from a Newborn Magnetar with Bt > 1016 G

- GW emission concentrated in the first few weeks of the magnetar life Spin down timescale:

- e.m. torques due to Bd, GW torques due to Bt-induced distortion

- GW strain for the Virgo Cluster distance (20 Mpc)

- Characteristics amplitude with

A VERY PROMISING VALUE !

Bt

Optimal Signal to Noise ratio with advanced LIGOPo = 1.2 msPo = 2.0 msPo = 2.5 ms

initial spin periods (for Virgo Cluster distance, 20 Mpc)

- Detection threshold of ~12 (for 1018 templates)

Most promising region is Bt > 1016.5 G and Bd < 1014 G

- Within reach, but required no. of templates is very large: hierarchical search techniques required (Dall’Osso & Re 2007)

Slowly evolving periodic GW signal at ~1 kHz,whose frequency halves over weeks, would unambiguously reveal the early days of fast-spinning magnetar

Expected magnetar birth rate in the ~2000 galaxies of Virgo: > 1 yr-1 ! We do not know which fraction is born with sufficiently high Bt, the 2004 Dec 27 event indicates that values > 1016 G might be common

Potentially Very Interesting GW Event Rate in Advanced LIGO-class instruments

The present and near future (2-3 years)

- 2 transient magnetars discovered: magnetars might be morenumerous than currently believed and their birth rate higher

- Frequency of occurrence of very high energy SGR Giant Flares tobe determined

- Dedicated (hierarchical) signal search techniques to be developed

Summary

There is now astrophysical evidence that magnetars have B>1016 Gauss:

- GWs from newborn magnetars can be detectable from the whole Virgo Cluster, where their birth rate is >1 magnetar/yr

- Newborn Magnetars are interesting GW sources for Advanced LIGO-class instruments

Refs:Stella, Dall’Osso, Israel & Vecchio, 2005 ApJ 634 L165Dall’Osso & Stella astro-ph/ 0702075Dall’’Osso & Re 2007, PRD, submitted

A special thank also to Moriond 2005 !