Transcript Slides
@yongpyung.08.02.22 Gamma-Ray Burst Progenitors Chang-Hwan Lee @ 1 Motivations Contents • Introduction to GRB • Long-soft GRB progenitors • HMBH Black Hole Binaries Hypernovae Short-hard GRB progenitors NS/low-mass BH binaries Gravitational waves 2 GRB Gamma-Ray Burst Duration: milli sec - min 1970s : Vela Satellite 1990s: CGRO, BeppoSAX 3 2000s: HETE-II, Swift GRB Cosmological Origin of GRBs 4 GRB Two groups of GRBs Long-duration Gamma-ray Bursts: => HMBH Binaries Short Hard Gamma-ray Bursts: Duration time < 2 sec => NS-NS, NS-BH Binaries 5 L-GRB Contents • Introduction to GRB • Long-soft GRB Progenitors HMBH Black Hole Binaries ApJ 575 (2002) 996 ApJ 671 (2007) L41 Hypernovae • Short-hard GRB Progenitors NS/low-mass BH binaries Gravitational waves HMBH (High-mass black hole) 5-10 solar mass 6 L-GRB LONG-DURATION GRBS BATSE Sample short long Afterglow => Host Galaxy Association => Distance Estimation 0.01 1 7 1000 7 L-GRB GRB/Supernova Association Afterglow GRB980425 SN1998bw 8 L-GRB Kelly et al., arXiv:0712.0430 Type Ic No H, No He consistent with L-GRB afterglow observation 9 L-GRB Candidates for Type Ic SN / L-GRB No H, No He line • WR stars: very massive single progenitor ( > 35 Msun) - loss of hydrogen envelope due to strong wind - slow final rotation • Massive progenitors in binaries ( > 20 Msun) - loss of hydrogen envelope due to common envelope evolution - fast final rotation 10 L-GRB What caused GRB/Supernova (Type Ic) ? Most-likely Rapidly rotating Black Holes Callapsar: Asymmetric Explosion of a Massive Star Most-likely Rapid-Rotation 11 Hyper accretion Formation of black hole Giant Star black hole 12 at birth A Generic GRB Fireball UV/opt/IR/radio gamma-ray gammaray X-ray UV/optical IR mm radio central photosphere internal engine shocks external shocks (reverse & forward) 13 GRB GRBs produced by forward & backward shocks 14 L-GRB How to to form form rapidly rapidly spinning spinning black black holes holes?to trigger How GRBs/Hypernovae ? Most likely in binaries Companion star can keep the BH progenitor rotating Formation of rapidly rotating stellar mass BHs Are there evidences in observation? YES ! 15 Soft X-ray transients (Observed BH Binaries) HMBH Binary Discovery of X-ray BH Binaries X-rays Mass accretion from a companion star to a compact object 16 HMBH Binary X-ray & Optical Telescopes Oscillating Brightness (GRO J1655-40) 17 HMBH Binary m=2Msun ; MBH=6Msun N O Nova Sco 94 Mg Si S Ti Fe [Xi/H] 0.45 1.00 0.90 0.90 0.75 0.90 0.10 error 0.50 0.30 0.40 0.30 0.20 0.40 0.20 [Xi/H]: logarithmic abundances relative to solar Israelial et al. 1999, Nature It’s impossible for normal stars! Where did they come from? 18 HMBH Binary Abundances in the secondary of Nova Sco 94 N [Xi/H] O Mg 0.45 1.00 0.90 Si S Ti Fe 0.90 0.75 0.90 0.10 They 0.50 had to come from black hole progenitor 0.30 0.40 0.30 0.20 0.40 0.20 when it exploded. error Hypernova to explain the observations. 19 HMBH Binary Another evidence ? C.M. System velocity (-106 km/s) : Abrupt Mass Loss by Explosion Mg,Si,S,… 20 HMBH Binary Hypernova Explosions from Rotating BH High Black Hole Mass ( > 5 Msun) --- Maximum Neutron Star Mass < 2 Msun Evidences of BH Spin in BH Binaries What is the key to trigger the explosion ? 21 [ Lee et al. ApJ (2002) ] at BH birth Tidal interaction before BH formation rapidly spinning BH Fe Synchronization of BH-Progenitor Spin & Binary Orbital Period 22 at BH birth Kerr parameter Preexplosion orbital period (days) 23 BH Spin Observation LINE PROFILE at BH birth Fabian Miniutti Doppler effect + Gravitational Redshifts Indication of BH spin 24 at BH birth Innermost stable circular orbit Fabian & Miniutti Schwarzschild BH Kerr BH Line Intensity 25 at BH birth Rapidly spinning black holes at birth Shafee et al. (2006) 4U 1543-47 GRO J1655-40 Sources for GRB & Hypernovae at birth Lee et al. ApJ (2002) Preexplosion orbital period (days) 26 at BH birth Reconstructed BH Binaries at Birth BH Spin – 10000/sec HN/GRB 27 at birth AVAILABLE BH SPIN ENERGIES ? EB 0 Blandford-Znajek 28 Soft X-ray transients (Observed BH Binaries) at birth Kerr parameters & Available Energy L-GRBs 29 L-GRB Conclusions Long-soft GRBs Progenitors • Spin of Stellar Mass BH in BH binaries Spin of stellar-mass BHs : - tidal (BH progenitor spin-orbit) synchronization is consistent with the current BH spin observation Rapidly-Spinning BH can power both GRB & Hypernovae L-GRBs and Hypernovae : - Short orbital period ( P<0.5 day) HMBH binaries are the relics of L-GRBs and Hypernovae 30 SH-GRB Contents • Introduction to GRB • Long-soft GRB Progenitors HMBH Black Hole Binaries Hypernovae • Short-hard GRB Progenitors NS/low-mass BH binaries Gravitational waves low-mas Black Hole 2-3 solar mass 31 SH-GRB hard BATSE SHORT-HARD GRBS Sample Origin NS-NS, NS-BH merger No Early Optical Afterglow, yet short long soft 0.01 1 UFFO Any coincidence with GW detection@LIGO ? Any information on the 3 inner structure of NS ? 2 32 1000 GRB Short-Hard Gamma-ray Burst : Colliding NS binaries Very Important for Gravitational Waves, too Science 308 (2005) 939 33 GRB Laser Interferometer Gravitational Wave Observatory LIGO I : in operation (since 2004) LIGO II: in progress (2014 ?) 34 Motivations NS (radio pulsar) which coalesce within Hubble time (2003) (2004) (1990) (2004) (1975) (1990) (2000) Not important Globular Cluster : no binary evolution35 White Dwarf companion UFFO Wanted by UFFO Existence of early optical afterglow of GRBs , especially Short-hard GRBs ? If exist, what UFFO can tell us about the physics of GRBs? Can UFFO tell something about the inner structure of NS ? 36 Thank You ! 37 Extra Slides 38 SH-GRB Contents • Introduction to GRB • Long-soft GRB Progenitors HMBH Black Hole Binaries Hypernovae • Short-hard GRB Progenitors Physics Reports 462 (2008) 1 Brown, CHL, Rho NS/low-mass BH binaries Gravitational waves low-mas Black Hole 2-3 solar mass 39 maximum MNS Inner structure of NS can be revealed by UFFO? Why Strange Quarks in Neutron Stars ? proton, neutron: u, d quarks By introducing strange quark, we have one more degrees of freedom, energy of the system can be reduced! In what form ? Kaon, Hyperons … … Kaon is the lighest particle with strange quark ! 40 maximum MNS Chemical Potential Kaon Condensation in Dense Matter 41 maximum MNS “Neutron/Strange/Quark” Star 42 Astrophysical Implications maximum MNS Neutron Star Neutrino s Reduce Pressure Soft EoS 43 Formation of low mass Black Hole Mass of stable NS Black Holes maximum MNS NS without kaon BH with kaon condensation Neutron Stars 44 NS observation Masses of Radio Pulsars NS-NS NS-WD Large uncertainty due to WD mass determination 45 1.5 NS observation Short summary on NS observations All well-controlled observations are consistent with lower maximum NS mass (soft equation of state). Those observations with higher NS mass cannot rule out the soft equation of state, yet. 46 Hyper accretion Formation of black hole/neutron star Giant Star black hole or neutron star 47 Hyper accretion NS/BH formation from Giant Stars Mass of Iron Core < 1.5 Msun : NS > 1.5 Msun : BH There are a lot more Black Holes (unseen) than we thought !! 48 Hyper accretion H red giant A Life time B He red giant NS 90% 10% NS A He H He B DT > 10% +0.7 Msun +0.2 Msun Hypercritical Accretion: First born NS should accrete 0.9 M⊙ ! 49 y-axis: final mass of first-born NS in NS-NS Binaries, if they can stay as NS GW & SHB NS-BH NS-BH should be more dominant than NS-NS NS-NS 50 Lee et al., ApJ 670, 741 (2007) Hyper accretion Why we don’t see BH-NS Binary ? Pulsar life time : 1/B Fresh pulsar : B=1012 G • NS-NS: First-born NS is recycled by accretion B=108 G (large chances to be observed) • BH-NS: No recycled pulsar Second fresh pulsar doesn’t live long ! 51 GW & SHB Short-Hard Gamma-ray Bursts (SHBs) Observed NS-NS binaries are inconsistent with SHBs Invisible old ( > 6 Gyr) NS binaries are responsible for short-hard gamma-ray bursts (SHBs) Nakar, Physics Reports invisible old NS binaries are consistent with our NS-BH Binaries Lee et al., ApJ (2007) 52 GW & SHB Hypercritical Accretion NS + LMBH Binaries as GW source • unseen “NS+LMBH” are 6 times more dominant than seen “NS+NS” system. • “NS+LMBH” system may increase LIGO detection rate by factor of about 10. 53 NS/LMBH • NS/Low-mass BH binaries Maximum mass of NS : - soft equations of state predict lower NS masses Observations : - most NS masses in binaries are still consistent with soft equations of state (prefer lower NS mass). - some indications for higher NS masses Hypercritical accretion : - NS/LMBH should be much more dominant than NS/NS due to hypercritical accreiton Gravitational waves & Short-Hard GRBs : - Advanced LIGO should see 10 times more mergers than predicted by NS/NS binaries - invisible NS/LMBH binaries are consistent with SHBs 54