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CALTECH AY 125 - Neutron Stars

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Neutron StarsSlide 2ReferencesManifestations of NSManifestations of Neutron StarsA Young Pulsar in G11.2-0.3PowerPoint PresentationPulsar P-Pdot DiagramSlide 9Slide 10Slide 11Slide 12Nearby X-ray NSMagnetic FieldsSlide 15Slide 16Masses of Neutron StarsNeutron Star MassesSlide 19Radius (Rotation) of NSCoherent Oscillations from LMXBsMaximum Spin RateRadius of NS: constraints from spin periodFormation of NSSlide 25Slide 26Slide 27Slide 28Do most SN produce NS?Enigmatic Source in Cas AWhat is in the center of SN 1987A?Slide 32Slide 33Slide 34Neutron StarsNeutron Stars•Discovery of neutron (1932) •Neutron Star (1934)–Landau (unpublished)–Baade & Zwicky “With all reserve we advance the view that supernovae represent the transitions from ordinary stars into neutron stars, which in their final stages consist of extremely close packed neutrons”•Oppenheimer & Volkoff (1938)•Recognition of the importance of accretion power (Salpeter, …) in early sixtiesReferences•Padmanabhan (Volume 2)•Shapiro Teukolsky •Lattimer & Prakash Science (astroph/0405262)–This is an excellent review •Kaspi et al. (astroph/0402136)–Good phenomenological review•Kaplan 2004 PhD thesis–For local flavourManifestations of NSManifestations of Neutron Stars•Low Mass X-ray Binaries (Rocket Flt, Sco X-1)•Pulsars (IPS Array, CP1919)•High Mass X-ray Binaries (UHURU, Cen X-3?)•Binary Pulsars (Arecibo, 1913+16)•Soft gamma-ray repeater (Satellites, 5 March 1979)•Millisecond Pulsars (Arecibo, 1937+214)•Cluster Pulsars (Jodrell Bank, M28)•Anomalous X-ray Pulsars (Einstein, 1E2259)•Thermally emitting NS (ROSAT, RXJ 1856)•Enigmatic source in Cas A (Chandra)A Young Pulsar in G11.2-0.3Of Crabs, Shells and PlerionsPulsar P-Pdot DiagramNearby X-ray NS•Cooling NS•Middle-aged magnetars (decay of B field)•Accreting from ISM (see Accretion lecture)Magnetic FieldsCyclotron Frequency omega = eB/mcElectron cyclotron: nu = 3 Hz B(micro Gauss) Energy = 10 keV (B/1012) G BQED = 4x1013 GaussMagnetic Fields•Cyclotron lines in accreting pulsars (usually confirmed by harmonics)•Features in nearby X-ray bright NS (confused state of affairs)–Some are interpreted as proton cyclotron–Features are broad in some casesSee review by Kaspi et al. [astroph/0402136]Masses of Neutron StarsNeutron Star MassesRadius (Rotation) of NSCoherent Oscillations from LMXBsMaximum Spin Rate642 Hz: Is this the limiting period?•Neutron stars cannot be spun up (grav radiation -> LIGO)•Limiting period is fundamental to the equation of state of dense matterRadius of NS: constraints from spin periodFormation of NSDo most SN produce NS?Enigmatic Source in Cas AWhat is in the center of SN 1987A?Kaplan’s thesis: what is in the centers of


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