GW from GRBs Gravitational Radiation from Gamma-Ray Bursts
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1 GW from GRBs Gravitational Radiation from Gamma-Ray Bursts Tsvi Piran Racah Inst. of Jerusalem, Israel Dafne Guetta,, Ehud Nakar, Reem Sari
2 Once or twice a day we see a burst of low energy gamma-rays from the outer space lasting for a few seconds. The energy released during a burst (~10 51 erg within a few seconds) is only a few orders of magnitude below the energy released by the rest of the Universe at the same time! GRBs are the (electromagnetically) brightest objects in the Universe. Only ~8 orders of magnitude less then the theoretically maximal * luminosity (c 5 /G)~10 59 erg/sec. * Up to relativistic corrections. 2 Mc GM / c 3
3 bad GRBs are good for many thing: Determining the high redshift history of the universe? Destroy Life on Earth (mass extinction)?? Creat Life on Earth (trigger planet formation)? Measuring quantum gravity effects?
4 GRBs are good for many thing: Determining the high redshift history of the universe? Destroy Life on Earth (mass extinction)?? Creat Life on Earth (trigger planet formation)? Measuring quantum gravity effects? Accompany sources of Gravitational Radiation (Kochanek & Piran, 1993).
5 Observations The Fireball Model OUTLINE Gravitational Radiation from GRBs Sources Rates Digression to Lorentz Invariance Violation (time permitting) Conclusions and prospects
6 THE DISCOVERY GRBs were discovered accidentally by Klebesadal Strong and Olson in 1967 using the Vela satellites (defense satellites sent to monitor the outer space treaty). The discovery was reported for the first time only in There was an invited prediction Colgate (1967) predicted GRBs from (galactic) supernovae.
7 Properties Duration s Two populations (long and short) ~ keV photons (non n thermal spectrum) (very high energy tail, up to GeV, 500GeV?) Rapid variability (less than 10ms)
8 The Internal-External Fireball Model γ-rays Afterglow Inner Engine Relativistic Outflow Internal Shocks External Shock 10 6 cm cm cm
9 ATERGLOW The bursts are followed by multiwavelength afterglow: X-ray, radio, Optical BeppoSAX
10 Duration ~30 sec accretion time scale. Variability 0.1 sec fluctuation time scale. Short lived accretion disk
11 Routes to a short BH-Disk-Jet NS/BH-NS merger BH-WD merger NS/BH-He core merger Collapsar - LONG - SHORT Long Davies et al, 94 Woosley et al, 99
12 Long Duration GRBs: Massive Stars & Sne GRB host galaxies are star- forming galaxies High column density/extincted extincted bursts In regions of very high star formation (Fruchter( Fruchter). Association with type Ibc SNe But SNe are not seen in some GRBs?
13 Rates of Long Bursts The observed rates of long BAT GRBs is 1 per day on BATSE (20-300KeV, 0.25 photons/cm2/sec, 1/3 sky coverage) An observed burst per galaxy in years years/galaxy with a beaming correction of ~50 This rate is a factor of >1000 below the rate of SNe. Does not follow the SFR requires more distant bursts! UVOT XRT
14 ~ 1/3 of BATSE long bursts. ~1/10 of Swift long bursts. Lower total energy and weaker afterflows. Short Bursts
15 Are Short GRB Extragalactic HyperGiantFlares from SGRs? NO! Nakar, GalYam, TP, Fox, 05?
16 Host of GRB Keck/LGSAO/Narrow Camera K band Evidence for an old population Red elliptical z=0.258 L=1.6 L* SFR<0.03 M yr-1 GRB Kulkarni & Cameron GRB From Nakar, Gal Yam & Fox 05
17
18 Rates of Short GRBs Rate from the observed redshifts Too few known Dominated by unknown selection effects Rate from the flux distribution Ambiguity Rate from Fluxes + Check with the redshift distribution
19 Rates from Fluxes N(>F) Number of bursts with flux >F { n(z) Rate as a function of z φ(l) Luminosity function
20 Rates from Flux N ( > F ) =! 0 Z max ( L, F, p) dz n( z)! 0 " dl #( L) Number of bursts with flux >F Rate as a function of z Luminosity function Maximal redshift for detection of a burst with a luminosity L given the detector s s sensitivity p.
21 Guetta Tsvi Piran & TAU TP March 05a,b 07
22 ? X? X X?? X X XX A comparison with Swift short bursts (Guetta & Piran,, 06) Does not follow the SFR Need more nearby bursts
23 From Nakar, Gal Yam & Fox 05
24 Time lag p(τ) probability for a time lag τ TP 92, Ando 2004
25 Within the context of NS mergers expect p(τ) 1/ 1/τ (TP 92)
26 Intermediate Short Long Selection effects? Guetta & Piran 05
27
28 Typical Delays:
29 Two populations???
30 Luminosity function and Rates ~10 /Gpc 3 /yr 80 mergers /Myr/ Galaxy* *Assuming a beaming factor of 30 Comparable to the estimated rate of mergers (e.g( Kalogera 04) L*~ erg/sec
31 Luminosity function and Rates Weakly constrained by current detectors L*~ erg/sec ~10 4 /Gpc 3 /yr mergers /Myr/ Galaxy Nakar, Gal-Yam, Fox 05, See also Tanvir 05
32 80 Myr/Galaxy 20 (0.5) events/yr within 200Mpc 10 5 Myr/Galaxy 20 (1) events/yr within 40Mpc 1 out of 30 in coincidence with a (short) GRB!
33 Gravitational Radiation from jet acceleration? Regardless of the nature of the inner engine the fireball model predicts gravitational radiation from the acceleration of ~10 51 ergs to relativistic velocity (Piran, 00). γ-rays Acceleration to Γ>>1 within δt Acceleration to Γ>>1 γ-rays 33
34 No Coincidence between this Gravitational Radiation and the GRB Gravitational waves γ-rays Acceleration to Γ>>1 Afterglow Afterglow γ-rays Acceleration to Γ>>1 Gravitational waves 34
35 Summary Long GRBs are associated with powerful SNe (hypernovae)) and produce GW. Rate LGRB <1000 Rate SNe unimportant for GW detection. Short bursts NS-NS or NS-BH mergers. Rate SGRB > 20 events/year up to 200 Mpc Rate SGRB Note uncertainty in the beaming factor (30). A much higher rate is possible but is highly uncertain. GRB coincidences enhance the significance of GW detection but only 1 in 30 events. The canonical GRB mechanism itself is not a likely source of detectable GW emission.
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