Short and Long Radio Bursts Binary mergers as ``naked inner engines to short and long GRBs Maurice HPM van Putten Le Studium Chair d Astrophysique Le Studium IAS Université d Orléans van Putten - PSR Workshop 008
Outline Radio-bursts and GRBs from rotating black holes Comparison with HETE-II and Swift data Long duration bursts from mergers with Kerr BHs Comparison with BATSE light curves Conclusions and Outlook van Putten - PSR Workshop 008
Stellar mass transient: 5 ms extragalactic radio burst if not instrumental! (Gilles Theureau, 008, priv. comm.) van Putten - PSR Workshop 008 3 Lorimer et al., 007, Science, 38, 585
Stellar mass transients: GRBs 967 Discovery by Vela (US) /Konus (USSR) 99 BATSE Catalogue 997 Redshifts by Beppo-Sax 997 Afterglows by Beppo-Sax 005 Afterglows to short bursts by HETE-II 003 Long GRBs with SN: HETE II GRB03039/SN003dh (confirmed GRB98045/SN998bw) 006 Long GRB without SN: Swift event GRB06064) Present: IPN, HETE II, Swift, GLAST/Fermi van Putten - PSR Workshop 008 4
Black Holes with Spin Spin- energy and frame dragging van Putten - PSR Workshop 008 5
Orbital motion in flat and curved spacetime Orbits of any size Newton ISCO ISCO Schwarzschild Kerr van Putten - PSR Workshop 008 6
Magnetic Flares ( Corona Ejections ) as X-ray sources X-ray line-emission by fluorescence B R van Putten - PSR Workshop 008 7 Fabian, 005, at KerrFest
flux R Iron line-emissions B 4keV energy Doppler line-splitting, Newtonian Splitting + beaming + gravitational redshift MCG-6-30-5 Tanaka et al. 995 van Putten - PSR Workshop 008 8 After Fabian 005 KerrFest
Tanaka et al. 995 Iwasawa etal. 996 R B R Kerr Schwarzschild B Compact ISCO by frame-dragging Kα line emission in MCG-6-30-5 (Seyfert I in a low state) observed by ASCA van Putten - PSR Workshop 008 9
Active Nuclei from spinning black holes Spin Energy f s (Van Putten 999,008) E spin = Ω cos( λ / ) 54 = (sinλ = a / M ) E 4 0 cos( / 4) spin λ 7 H If s M M sun erg Bekenstein- Hawking Entropy S H = 4πM cos ( λ / ) Bekenstein 973; Bardeen et al. 973; Hawking, 973, Strominger & Vafa 996 Kerr BHs can radiate Penrose (969) conform the Rayleigh criterion a M > M p a H van Putten - PSR Workshop 008 0
Angular momentum coupling to Riemann curvature force J = ±ea ϕ F c = *R abcd J a u b u d Papapetrou 956 Blanchet, OSUC Mass Motion 008 Unfortunately, in practical situations it is so weak that nobody has ever found any significant application for it. Thorne, Price & McDonald (986) p56 Line integral E = J Riemann ds =ωj r van Putten, Il. Nuov. Cim. 005 cm /cm van Putten - PSR Workshop 008
Relativistic capillary effect UHECR Linear accelerator Stable against pair-cascade, nearly charge-free A [ V] r A ~ VH Outflow by relativistic capillary effect Van Putten 008 bounded by Alfven surfaces (``Blandford-Znajek limit ) Approx zero potential drop [ V] θh 0 =VH van Putten - PSR Workshop 008
-0 Myr Transiet source during spin-down of SMBH E B M T B B 5 (torus magnetosph ere) E (disk) M AGN = = 9 B M = 5 9 T 7 k.04 0 0 5 9 0 G M T M 7 7 9 Solar yr,, 5 Van Putten & Gupta (008), submitted Van Putten & Levinson (003) AGN T 7 ~ 0.- (-0 million years), based on 3 FR II Radio Galaxies O Dea C.P. et al. (008) van Putten - PSR Workshop 008 3
Energetic output in leptonic jet Gamma-rays by dissipation of kinetic energy in ultra-relativistic baryon poor in internal shocks Shemi & Piran 990, Rees & Meszaros 99,... E E p γ = c = c E LT 90 ( E = ωj, J = eaϕ) ( L= Ω A, Goldreich & Julian 969; Blandford & Znajek 977, Thorne et al.987) F ϕ c c, ω, Ω F ~ Ω H E p T / 90 = eke / γ / ( k = cc ) Ep E c E 0.7 γ 3/ p (Eichler &Juntof (Ghirlanda et al. 004) -Hutter 005) ; k E / 40 γ E / γ E p T / 90 E γ V H 3 0 M 7M H Sun B 6 0 G θh 0.5 ev van Putten - PSR Workshop 008 van Putten et al., PRD (004) 4
Correlation to HETE-II and Swift data Pearson coeff: 0.85 Pearson coeff. 0.76 E p T / 90 E γ van Putten - PSR Workshop 008 5 van Putten, 008
Topology of black hole torus formation GRB03039/SN003dh GRB06064 A common inner engine to long GRBs with & without SNe Van Putten Science 999 Van Putten & Ostriker ApJ L 00 van Putten & Levinson ApJ 003 van Putten - PSR Workshop 008 6
Bi-modal distribution in durations from slowly and rapidly rotating BHs ΩH < ΩISCO T90 hyper-accretion (accelerated by shedding of angular momentum in magnetic winds) ΩH > ΩISCO T90 viscous timescale of BH spin-down (by horizon Maxwell stresses) van Putten - PSR Workshop 008 7 Van Putten & Ostriker 00
Suspended accretion state by powerful spin-connection BH PSR PSR + - asymptotic infinity PSR Ω + PSR Ω Ω H Ω=0 Spin-up Spin-down Topological equivalence to pulsar magnetospheres when viewed in poloidal cross-section van Putten, Science (999) van Putten & Ostriker ApJL 00 van Putten & Levinson ApJ 003 van Putten & Levinson, Science (00) van Putten - PSR Workshop 008 8
Equations of BH spin-down in suspended accretion Position of the ISCO (rel. M ) : z Specific energy and angular momentum at ISCO: e= Ω T Z / = + (-a 3 l = M z 3, + a ) 3 3 ((+ a) Ω 3 + ( a) = 3+ Z ), ((3 Z = (3a ( a= M, z= ; a= 0, z= 6) H tan( λ / ) = M 3 Z Ω η = Ω T H = )(3+ Z + Z ) ; 3z + Z )) ( ) z + a tan( λ/) 3 l = - 3 [ ] + (3z ) : Bardeen et al.97 Van Putten 999 Balance of E Balance of J dm dt dj dt = e = e ( ) ηηω ( η) Ω H H Van Putten, 008 van Putten - PSR Workshop 008 9
Model light-curve compared with normalized GRB light curves van Putten - PSR Workshop 008 0
Matched Filtering to BATSE light curves of long GRBs van Putten - PSR Workshop 008 Van Putten & Gupta, 008, under review
Matched Filtering with Kerr and Block-type template van Putten - PSR Workshop 008
Matched Filtering to BATSE light curves of long GRBs van Putten - PSR Workshop 008 3 Van Putten & Gupta, 008, under review Van Putten, in Orleans School of Mass and Motion in GR (008)
Conclusions and Outlook Binary mergers of neutron stars and BHs produce an energetic (``explosive ) events with a bi-modal distribution of durations similar to those of GRBs in the BATSE catalogue from systems with BH angular velocities smaller and larger than that of the ISCO As a ``naked inner engines (would make aspherical radio-loud Ib/c in CC-SNe) are intrinsically radio-loud: energy output in magnetic winds from the accretion disk is about e5 erg for long bursts, and less for short bursts. Binary mergers in low-density host environments Radio emissions from the magnetic winds may be un-absorbed and detectable Outlook Archive searches in radio may reveal long-duration counterparts to the Lorimer at al. 007 event van Putten - PSR Workshop 008 4