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GRBs and their contribution to the stochastic background radiation in gravitational waves

GRBs and their contribution to the stochastic background radiation in gravitational waves. Maurice H.P.M. van Putten (MIT-LIGO) LIGO-G030145-00-Z. LSC March 2003. GRB 011211 (z=2.41). Reeves et al. ‘02. GRB-durations and energies. GRB-SNe association. Kouvelioutou et al. ‘93.

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GRBs and their contribution to the stochastic background radiation in gravitational waves

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  1. GRBs and their contribution to the stochastic background radiation in gravitational waves Maurice H.P.M. van Putten (MIT-LIGO) LIGO-G030145-00-Z LSC March 2003

  2. GRB 011211 (z=2.41) Reeves et al. ‘02 GRB-durations and energies GRB-SNe association Kouvelioutou et al. ‘93 Van Putten ‘02 Frail et al. ‘01 Regimbau & Van Putten 2003, in preparation

  3. Formation of counter-oriented current rings in core-collapse Van Putten & Levinson, ApJ, 2003

  4. Topology of flux-surfaces of a uniformly magnetized torus (vacuum case) separatrix Van Putten & Levinson, ApJ 2003

  5. tilt Magnetic stability Potential energy (magnetic+tidal) B-dominant G-dominant Van Putten-Levinson stability criterion: Van Putten & Levinson, ApJ 2003

  6. PSR + PSR - BH Asymptotic infinity Spin-up Spin-down PSR PSR Topological Equivalence to Pulsars Black hole luminosity from horizon Maxwell stresses: Perturbative limit: Ruffini & Wilson (PRD 1975) Non-perturbative: Blandford & Znajek (MNRAS 1977) but: causality unresolved (Punsly & Coroniti ApJ 1989) Causality by topological equivalence to PSRs: van Putten (Science 1999): (a) Most of the black hole luminosity is incident onto the inner face of the torus (b) Most of the black hole-spin energy is dissipated in the horizon Van Putten & Levinson, 2003; Science 2002 Van Putten, Phys Rep, 2001; Science 1999

  7. Long durations Van Putten & Levinson ApJ 2003

  8. Creation of open magnetic flux-tubes Baryon-poor inner tube Baryon-rich Outer tube 2MeV

  9. Energy in baryon-poor outflows qj qH Van Putten ApJ 2003 Van Putten & Levinson APJ 2003

  10. Small GRB-energies Van Putten ApJ 2003 Van Putten & Levinson APJ 2003

  11. T90 and GRB-energies Rotational energy of black hole Horizon dissipation Black hole output Torus input Baryon poor outflows tens of seconds GRBs

  12. Stability diagram of multipole mass-moments U S Slenderness -> Van Putten, 2002

  13. Gravitational Radiation in suspended accretion Balance in angular momentum and energy transport for a torus around a black hole with a quadrupole mass moment with the constitutive ansatz for dissipation by turbulent MHD stresses, into thermal emissions and MeV-neutrino emissions Van Putten, 2001

  14. Energy emissions from the torus Asymptotic results for small slenderness In practical terms… Gravitational radiation by catalytic conversion of spin-energy

  15. Calorimetry Rotational energy of black hole Horizon dissipation Black hole output Torus input Baryon poor outflows Gravitational radiation Torus winds Thermal and neutrino emissions GRBs SN irradiation of envelope Torus mass loss SN remnant X-ray emission lines

  16. Emission lines in GRB 011211 (Reeves et al., 2002) Van Putten, ApJ, 2003

  17. Observational opportunities in astronomy • Calorimetry on SNRs of GRB-remnants: constrain wind energies and frequency in gws • Morphology of GRB-remants: black hole in a binary with optical companion surrounded by SNR RX J050736-6847.8 Chu, Kim, Points et al., ApJ, 2000

  18. Stochastic background radiation Coward, van Putten & Burman (2002) Van Putten (2003), in preparation Van Putten (2003), in preparation

  19. Observational opportunities for LIGO • Radiation from GRB-SNe, point sources: • Associated with SNe, test t0[gw-burst]=t0[SN] • Radiation from GRB-SNe, stochastic background radiation: Van Putten (2003), in preparation

  20. A line-detection algorithm Van Putten & van Putten, in prep

  21. Conclusions • Model: GRB-SNe from rotating black holes in dimensionless gamma parameters as a function of normalized angular velocity eta, slenderness delta and mass mu of the surrounding torus • Long durations (largegamma0~1e4) stem from lifetime black hole-spin, subject to the Van Putten-Levinson stability criterion for the torus. • GRB-energies (smallgamma1~1e-3) derive from a BPJ produced by the black hole, regulated by poloidal curvature in torus magnetosphere • Gravitational radiation during the GRB-SNe event of energies of a few times 0.1MSolar (gamma2~0.1) at an expected nominal frequency around 470Hz • Expect spectral closure density of about 1e-8 @100-300Hz Observational opportunities for HF in Advanced LIGO with 3 detectors GRB remnants: black hole-binaries in SNRs Gravitational radiation in GRB-SNe (1/yr within D=100Mpc) LIGO GRB-sensitivity range presently: 1Mpc@500Hz Multiple lines in stochastic background radiation (1 yr obs LIGO-II)

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