Hypernovae: : GRB-supernovae as LIGO/VIRGO sources of gravitational radiation

Transcription

1 Hypernovae: : GRB-supernovae as LIGO/VIRGO sources of gravitational radiation Maurice H.P.M. van Putten (MIT-LIGO) in collaboration with Paris 003 Amir Levinson (Tel Aviv) Stephen Eikenberry (U Florida) Tania Regimbau (MIT-LIGO) Eve Ostriker (U Maryland) Hyun Kyu Lee (Hanyang( U) David Coward (U of WA) Ronald Burman (U of WA) LIGO-G R

2 Molecular cloud Star-formation in a molecular cloud

3 Core-collapse in a rotating massive star in a binary Molecular cloud Core-collapse (Woosley-Paczynski-Brown)

4 Active stellar nuclei Active nucleus inside remnant stellar envelope Molecular cloud Core-collapse (Woosley-Paczynski-Brown)

5 Hypernovae: GRB-supernovae from rotating black holes Jet through remnant envelope (McFadyen& Woosley 98)

6 Hypernovae: GRB-supernovae from rotating black holes Torus produces winds & radiation: Ejection of remnant stellar envelope Excitation of X-ray line-emissions E E r w Jet through remnant envelope (McFadyen& Woosley 98) van Putten (003)

7 GRB-SNe in and GRB (z.41) Reeves et al. 0 Er (G. Ghisellini 00) Stanek, K., et al., 003 astro-ph/

8 Outline 1. Quantitative phenomenology of GRB-supernovae. A causal spin-connection in active stellar nuclei 3. Durations of tens of seconds of long bursts 4. Calorimetry on radiation energies 5. Observational opportunities for Adv LIGO/VIRGO 6. Conclusions

9 GRBs with redshifts (33) and opening angles (16) GRB redshift angle instrument GRB SAX/WFC GRB SAX/WFC GRB RXTE/ASM GRB >0.056 SAX/WFC GRB SAX/WFC GRB >0.17 SAX/WFC GRB RXTE/ASM GRB SAX/WFC GRB BAT/PCA GRB SAX/WFC GRB SAX/WFC GRB >0.411 SAX/WFC GRB <0.079 Uly/KO/NE GRB BAT/PCA GRB <0.047 Uly/KO/NE GRB SAX/WFC GRB000131C ASM/Uly GRB SAX/WFC GRB Uly/KO/NE GRB Uly/KO/NE GRB Uly/KO/NE GRB SAX/WFC GRB HE/Uly/SAX GRB SAX/WFC GRB SAX/WFC GRB Uly/MO/SAX GRB HETE GRB HETE GRB HETE GRB HETE GRB HETE GRB HETE <- most nearby! Barthelmy s IPN Greiner s catalogue and Frail et al. (001) <- very nearby!

10 Durations of GRB-SNe True energy in gamma-rays Van Putten 0 Frail et al. 01 T 90 few 10 s E γ erg

11 The true-but-unseen GRB-event rate Unseen event rate 1/fb or 1/fr times observed event rate Geometrical beaming factor in GRB - emissions : 1/ f b 500 (Frail et al. 001) Event loss- rate in flux- limited sample locked to the SFR : observed simulated: observable simulated: total p SFR (z) Van Putten & Regimbau 003, submitted 1/ f r 450 (van Putten & Regimbau, 003,submitted) probability redshift z True GRB event rate / year

12 Phenomenology of GRB-SNe from rotating black holes For a 7 solar mass black hole : Keplerian period of the torus : P 4ms Rotational energy of the black hole : E rot erg γ 0 T 90 / P γ 1 E γ / E rot event per year within D 100Mpc

13 Magnetized nucleus in core-collapse collapse

14 A causal spin-connection to Kerr black holes Goldreich and Julian (1969) (spin-down of pulsars (magnetized neutron stars)) Ruffini & Wilson (1975) (spin-down of black holes, but: weak fields) Blandford & Znajek (1977) (strong fields, but: causality not addressed, Punsly & Coroniti 1990) Van Putten (1999) (idem, with causality by topological equivalence to PSRs) BH PSR PSR - Asymptotic infinity Spin-up Spin-down PSR Ω H Ω H PSR Ω Ω 0 Ω Van Putten & Levinson, ApJ 003; Science 00 Van Putten, Phys Rep, 001; Science 1999

15 Topology of inner and outer torus magnetospheres (vacuum case) separatrix Van Putten & Levinson, ApJ 003

16 New magnetic stability criterion Sum of magnetic and tidal interaction tilt Magnetic dominated U µ B > 0 U µ B < 0 b R Tidal dominated / < 1/1 E B E k [1/15 for buckling instabilit y] Van Putten & Levinson, ApJ 003

17 Durations of long bursts S S T H rot spin M M M R M M S T E T / 40s 4 Van Putten & Levinson, ApJ 003 Most of the spin-energy is dissipated unseen in the event horizon of the black hole T T spin 90

18 Long durations / ] [ 0.03 / 0.1 / 0.03) / ( 0.1) / ( 10 ] [ / parameter Large Ω Ω observed M M theory P T H T H T γ µ η µ η γ γ

19 Critical point analysis in baryon-rich rich torus wind MeV-torus cools by neutrino emission (electron-positron capture on nuclei) T 10 L 1/ 6 5 M T 0.1M S 1/ 6 M A [on torussurface] 16πp 1/ M 1/ 3 l T 1/ L Bp Bp M S ρ bc c s M 1/ M / 3 ξ H T 1/ c / 3 r M 0.1M r L c S S c 1 gcm - s -1 M g s -1 Van Putten & Levinson ApJ 003

20 Torus winds create open magnetic flux-tubes Baryon-poor inner tube Baryon-rich Outer tube MeV

21 The active stellar nucleus: a black hole in suspended accretion BH Magnetic wall PSR PSR - Van Putten & Levinson, submitted; Science 00 Van Putten, Phys Rep, 001; Science 1999

22 Equilibrium charge distribution Rapidly rotating black hole ρtopology Q>0 Q<0

23 Energy in baryon-poor outflows θj Outflow in open flux - tube along E T Ω A / 4 j 90 H ϕ rotation axis A ϕ BM H Poloidal curvature of flux -surfaces θ H θ H M H / R ( η / ) /3 θh Van Putten & Levinson ApJ 003

24 Small GRB-energies Small parameter γ 1 E E γ rot γ 1 [ theory] ( η / 0.1) 8/3 ( ε / 0.15) γ 1 [ observed]

25 Durations and GRB-energies Rotational energy of black hole γ 0 Horizon dissipation Black hole output γ 0 γ 1 tens of seconds Torus input Baryon poor outflows GRBs

26 Linearized stability analysis for the torus Free surface waves on inner and outer boundaries mutually interact (Papaloizou-Pringle 1984) m buckling mode

27 Waves in a differentially rotating and incompressible toroidal fluid (A) Following Papaloizou - Pringle (1984), consider the linearized stability analysis for an unperturbed torus (between Kepler and Rayleigh's criterion) : Ω( r) Ω e r h Ω a q a r M r r ( q [ 3,] ) h P ρ (B) Velocity potentialfor incompressible, irrotational perturbations (van Putten 00) ϕ e imθ iω ' t Σ n a n ( r) z n, ϕ 0 of azimuthal mode number m and corotation frequency ω' (C) Linearized Euler equations of motion (Goldreich et al.1986) iσu Ωv r ( h Φ) iσv Bu ik( h Φ) iσw zh where B ( q) Ω (variable), k m / r, σ ω' m( Ω Ω subject to zero enthalpy boundary conditions h 0. a ),

28 0. ) ( ) ( et al.1986) (Goldreich 0 ) ( at Boundary conditions (C) 4 / /, with ), ( (van Putten 00) Leading - order expansion in (B) ' ) ( EOM : of Decoupling (A) Φ ± ± ± r e r e p p r r r kh B i k r h m q q p r r a z O a r q z a z a qr a r m r ϕ σ σ ϕ σ λ ϕ A free boundary value problem

29 Multipole mass-moments moments in tori a Ω( r) Ωa r q ( ) q [ 3,] U q c 3 as b / a ~ 0 Papaloizou - Pringle (1984) Goldreich et al. (1986) S Slenderness -> Van Putten, 00

30 Gravitational radiation-reaction reaction force (m) Burke - Thorne Thus, πσ I xx The potential and so with Φ Φ iσ β BT ± [ ] 3 3 r η r η Φ 5 t ± 1 5 Φ x potential i in the BT x iβ ( r ± / a) 1 πaσ( ωa) 10 j I ij, EOM becomes iω 5 etc Φ Iδ [( r BT ± ~ 10 ij / a) 4, 3 ϕ I Φ r ij BT ( r Σ π ) ( r ± r r η η ( x iy) / a) 3 ϕ r x i I x ( r xx j dxdy, )]

31 Gravitational radiation-reaction reaction force on quadrupole emissions Complex plane of corotation frequency β 10 4 Increase in imaginary value: backreation promotes instability

32 Gravitational radiation in suspended accretion Balance in angular momentum and energy flux τ τ τ rad Ω τ Ω τ Ωτ rad P with the constitutive ansatz for dissipation P A r ( Ω Ω by turbulent MHD stresses, into thermal emissions and MeV-neutrino emissions )

33 Black hole-beauty: emissions from the torus Asymptotic results for small slenderness Egw Ew Ediss γ ~ η γ 3 ~ η γ 4 ~ δη E E E rot rot rot 4e53 erg in gravitational radiation 4e5 erg in torus winds producing SNe 6e5 erg in MeV-neutrinos η δ Ω T / Ω H 10% 1 minor - to - major radius of torus

34 Remnants of beauty Morphology of GRB-supernova remnant: Black hole in a binary with optical companion surrounded by SNR RX J Chu, Kim, Points et al., ApJ, 000 (Candidate GRB-SN remnant)

35 Calorimetry on active stellar nuclei Rotational energy of black hole Horizon dissipation Black hole output γ Torus input γ 4 Baryon poor outflows GWB 4e53erg Gravitational radiation γ 3 Torus winds Thermal and neutrino emissions GRB 3e50erg SN 4e51erg irradiation of envelope Torus mass loss X-ray emission lines SN remnant 1e49erg

36 Observational constraint on gravitational wave-frequency from wind-energy f gw 455Hz 3/ Ew 7M O ( m erg M ) (scaling value of wind energy corresponds to eta0.1)

37 Phase-modulation of observed radiation by Lense-Thirring precession n-torus α 0 Line-of-sight q ia torus h h cosα r 1 4r (1 1 sinα cos sinθ α) cos(ω cosα sin(ω 0 T cos( Ω t) LT T t) t) cosα 0 Van Putten, Lee, Lee & Kim, 003, in preparation cosθ

38 Phase-modulated wave-forms α 0 0, π θ π / 6 /8, π / 4, π /

39 h(f)-diagram in matched filtering Stochastic background radiation in gravitational waves D100Mpc Van Putten, in preparation (003)

40 Stochastic background radiation in gravitational waves Coward, van Putten & Burman 00 Van Putten et al., in preparation (003)

41 Observational opportunities for Adv LIGO Matched filtering S N mf 8 S 1/ h 4 10 (500Hz) 4 Hz -1/ 1 η 0.1 3/ M 7M H Solar 5/ d 140Mpc 1 Correlating two detectors S N cs 1.5 S 1/ h 4 10 (500Hz) 4 Hz -1/ 1 D1 S 1/ h 4 10 (500Hz) 4 Hz -1/ 1 D η 5/3 0.1 M 5 H 7 d 8 B µ 1/ S N averaged over M averaged over M H H 4 14 M 5 8 M S S Van Putten (003), in preparation

42 Lower bound on black hole-mass in GRB Spp we use matched filtering and define no detection : S/N<1 Entertain the possibility of Current Livingston S N mf sensitivity : 3 / a rapidly rotating torus : η M 7M H S Solar 1/ h / (500Hz) 4 Hz -1/ (140Mpc / 800Mpc) < 1 M H < 5M Solar Van Putten, Burst Digest (003), LIGO DCC D

43 Conclusions GRB-SNe from rotating black holes have long durations (gamma01e4), small true GRB-energies (gamma11e-4) and an true event rate of 1 per year in D100Mpc Durations of tens of seconds correspond to the lifetime of rapid spin of the black hole (gamma0[theory]gamma0[observation]). Most of black hole spin-energy is dissipated in the event horizon. GRB-SNe produce 4e53 erg in gravitational radiation via a causal spin-connection between the black hole and a surrounding torus in suspended accretion (gamma0.1) The true GRB-energies represent a small fraction of black hole-spin energy, released through an open tube with finite horizon angle (gamma1[theory]gamma1[observation]) Matched filtering gives (formally) rise to a current LIGO sensitivity range of 1Mpc, and a (formal) upper bound of 5 Solar masses in GRB The sensitivity range of Adv LIGO using matched filtering is 100Mpc Correlation between two detectors may apply to searches for individual events, as well as searches for the contribution of GRB-SNe to the stochastic background radiation in gravitational waves (Omega-B6e-8) Opportunity: gravitational radiation from hypernovae: LIGO/VIRGO detections coincident (in position on the sky) with the expected wide-angle optical emissions from an associated supernova and non-coincident with the associated GRB-emissions