The rate of short Gamma Ray Bursts and NS 2 mergers
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1 The rate of short Gamma Ray Bursts and NS 2 mergers Tsvi Piran The Hebrew University! David Wanderman, Paz Biniamini, Omer Bromberg,! Simore Dall Osso, Oleg Korobkin, Martin Obergaulinger
2 Outline Long and short GRBs vs Collapsars and non-collapsars The rate of non- Collapsar short GRBs Implications
3 A Quick Summary About 1/3 of Swift short (<2sec) GRBs are Collapsars The rate of non-collapsar short GRBs (sgrbs) is Gpc -3 yr -1 (depending on the assumed minimal luminosity). A LIGO detection rate of per year (0.1-3 coinciding with a sgrb)* A typical time delay of ~ 3 Gyr after SFR An initial separation of ~ 2 x cm With beaming of ~ 30 and mass ejection of 0.02 M sun - compatible with R-process nucleosynthesis for A>110 elements.
4 Gamma-Ray Bursts
5 Gamma-Ray Bursts
6 Long and Short GRBs Duration s Two populations: long (>2 sec) and short (<2 sec) The short GRBs are typically harder!
7 Eichler, Livio, TP, Schramm, 89 MacFadyen & Woosley, 98 NS mergers Collapsars Indirect Short Long Direct Evidence Evidence
8 GRB b Swift/XRT position intersects a bright elliptical at z = No optical/radio afterglow Kulkarni et al Elliptical host Old stellar population Bloom et al Castro-Tirado et al Gehrels et al Hjorth et al. 2005
9 The Collapsar Model (MacFadyen & Woosley 1998)
10 The Jet drills a hole in the star Model Zhang, Woosley & MacFadyen 2004
11 Jet Simulations (Obergaulinger, TP 11) Opening angle of 15 o degrees at 2000 km into a star of 15 solar masses and solar metallicity. Constant energy injection rate, 5 * erg /s, through the entire run of the model. Lorentz factor at injection 7
12 Jet Simulations (Obergaulinger, TP 11) Opening angle of 15 o degrees at 2000 km into a star of 15 solar masses and solar metallicity. Constant energy injection rate, 5 * erg /s, through the entire run of the model. Lorentz factor at injection 7
13 Jet Simulations (Obergaulinger, TP 11) Opening angle of 15 o degrees at 2000 km into a star of 15 solar masses and solar metallicity. Constant energy injection rate, 5 * erg /s, through the entire run of the model. Lorentz factor at injection 7
14 Jet Simulations - A Failed Jet (Obergaulinger, Piran + 11) Opening angle of 15 o degrees at 2000 km into a star of 15 solar masses and solar metallicity. Constant energy injection rate, 5 * erg/s, for 2 seconds.
15 Jet Simulations - A Failed Jet (Obergaulinger, Piran + 11) Opening angle of 15 o degrees at 2000 km into a star of 15 solar masses and solar metallicity. Constant energy injection rate, 5 * erg/s, for 2 seconds.
16 Jet breakout time (Bromberg Nakar, TP, Sari 11) Text
17 Jet breakout time (Bromberg Nakar, TP, Sari 11) Text The engine must be active until the jet s head breaks out!*
18 T e = T B +T 90 T B T 90 T e
19 A prediction of the Collapsar model Observed duration T 90 = T e -T B Engine time Break out time
20 A prediction of the Collapsar model Observed duration dn(t 90 )/dt T 90 = T e -T B Engine time Break out time T 90
21 A prediction of the Collapsar model Observed duration dn(t 90 )/dt T 90 = T e -T B Engine time Break out time T B T 90
22 ? Short Long T 90
23 ? dlog(n)/dt 90 Short Long T 90
24 A second look (Bromberg Nakar, TP & Sari, 2011) dn/dt 90 T 90
25 A second look (Bromberg Nakar, TP & Sari, 2011) dn/dt 90 T 90 A direct observational proof of the Collapsar model.
26 Short (Non-Collapsars) GRBs are harder Short GRBs are harder
27 Short (Non-Collapsars) GRBs are harder Short GRBs are harder
28 Short (Non-Collapsars) GRBs are harder Short GRBs are harder
29 Short (Non-Collapsars) GRBs are harder Short GRBs are harder BASTE shows a longer plateau for soft Bursts
30 Short (Non-Collapsars) GRBs are harder Short GRBs are harder BASTE shows a longer plateau for soft Bursts
31 Short (Non-Collapsars) Collapsars
32 Short (Non-Collapsars) Collapsars
33 Short (Non-Collapsars) GRBs Collapsars
34 Short (Non-Collapsars) GRBs Collapsars
35
36
37
38 Swift Short (Non- Collapsars) GRBs Collapsars
39 Swift Short (Non- Collapsars) GRBs Collapsars
40 Swift Short (Non- Collapsars) GRBs Collapsars Short Swift GRBs with T 90 >0.7sec are not short!
41 SGRB Fraction Bromberg et al, 2012 in perparation
42 The Rate of non-collapsars Wanderman & TP, 14 Our Sample BATSE short (<2 sec bursts) [peak flux] Fermi short (<2 sec bursts) [peak flux] Swift short with redshift and high probability of being non-collapsars
43 The Rate
44 The Luminosity Function Log[Φ(L)] Log(L)
45 MAXIMUM LIKELIHOOD
46 FITTING THE DATA
47 Best Fit Parameters
48 The intrinsic redshift distribution The rate was higher in the past
49 The time delay
50 Collapsars and non-collapsars
51 The local sgrb rate
52 The rate of sgrbs Guetta & TP 2006; Wanderman & TP 2014 R sgrb =4±2 Gpc -3 yr -1 Typical spiral-in phase of 2.5 Gyr. Consistent with R merger = 200 Gpc -3 yr -1 for a reasonable beaming factor of 30. Consistent with rate estimaes based on galactic neutron star binaries.
53 The NS 2 Sample 2.9 Gyr <-> 2x10 11 cm
54 Eccentricity Biniamini, Korobkin & TP, 14
55 Eccentricity Biniamini, Korobkin & TP, 14
56 J (the double pulsar) TP & Shaviv 05, Dall Osso, TP Shaviv 14 J0737 was not born in a regular SN Progenitors mass ~1.5 M sun Ejected mass ~ M sun
57 Eccentricity Biniamini, Korobkin & TP, 14
58 Eccentricity Biniamini, Korobkin & TP, 14
59 Eccentricity Biniamini, Korobkin & TP, 14
60 ALIGO Detection Rate With this rate we expect 0.1-3* joint ALIGO/(300 Mpc) sgrb per year (provided that there is a GRB satellite at the time). With a beaming factor of ~ 30 -> ALIGO events per year. * x covering factor of the GRB detector.
61 r-process nucleosynthesis Eichler, Livio, TP & Schtamm, 89; TP, Korobkin & Rossowg, x 10 4 sgrbs pointing towards us within the Milky way. With a beaming factor of 30 -> sufficient to produce the observed heavy r-process
62 Early nucleosynthesis - a challenge A population of fast mergers? time-> From Cowan and Thielemann
63 One cannot give a talk in Astronomy these days without a reference to the Solar System and life. sgrbs are too weak and too rate to pose danger to life due to events in the Galaxy. TP & Jimmenez, 14
64 Mergers and the early Solar system
65 Mergers and the early Solar system The early Solar System had 244 Pu (τ= 117 Myr) Wasserburg et al, (2006). No evidence for 244 Pu deposition in deep-sea crust and sediment accumulated over the last ~25 Myr (M. Paul et al., 2001; A. Wallner et al., in preparation). => 244 Pu is NOT from the Inter Stellar Medium! => Actinides production near the early Solar System just prior to formation. Gerry Wasserburg Irregular production from rare episodes. => E.g. a merger within <50 pc=150 lyr from the solar system just prior to its formation?
66 Summary About 1/3 of Swift short (<2sec) GRBs are Collapsars The rate of non-collapsar short GRBs (sgrbs) is Gpc -3 yr -1 (depending on the assumed minimal luminosity). A LIGO detection rate of per year (0.1-3 coinciding with a sgrb* A typical time delay of ~ 3 Gyr after SFR Corresponding to an initial separation of ~ 2 x cm With beaming of ~ 30 and mass ejection of 0.02 M sun - compatible with R-process nucleosynthesis for A>110 elements.
67 The END
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