Double neutron star evolution from geometric constraints
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1 Double neutron star evolution from geometric constraints Robert Ferdman University of East Anglia Bonn NS Workshop X 14 November 2016
2 A tale of two DNSs PSR J A/B J Spin period (s) / Pulsar/comp. mass (M ) (7) / (7) 1.341(7) / 1.230(7) Orbital/system parameters Orbital period (h) Inclination ( ) Eccentricity Trans. velocity (km/s) ~10 < 68 Compare with other DNS systems, e.g.: PSR B PSR B Eccentricity Trans. velocity (km/s)
3 Geodetic precession Companion star perturbs spacetime around pulsar spin axis precesses about orbital angular momentum k δ K s 1 j Orbital plane J i δ: misalignment angle Plane of the sky line of sight varies over time pulse profile change I = i Observer line of sight RDF et al. (2013)
4 Geodetic precession Companion star perturbs spacetime around pulsar spin axis precesses about orbital angular momentum k δ K s 1 j Orbital plane J i δ: misalignment angle Plane of the sky line of sight varies over time pulse profile change I = i Observer line of sight RDF et al. (2013)
5 Geodetic precession PSR Precession Period (yr) δ( ) B (years) (4) B (6) J A 75 J B (4) J J * (-44, +85)
6 Geodetic precession B PSR Precession Period (yr) B δ( ) B (years) (4) B (6) J A 75 J B (4) J J * (-44, +85) (Stairs, Living Rev. Relativity 6, (2003), 5) (Taylor & Weisberg, 1989, ApJ, 345, 434; Weisberg, Romani, and Taylor, 1989, ApJ, 347, 1030; Kramer, 1998, ApJ, 509, 856)
7 Geodetic precession PSR Precession Period (yr) δ( ) B (years) (4) B (6) J A 75 Fit widths: J B (4) beam region ½ opening angle pulse ½ width misalignment angle J (Rafikov & Lai 2006, ApJ, 641, 438) 496 J * (-44, +85) (Damour & Taylor 1992, PRD, 45, 1840) spin/magnetic axis separation spin/los axis separation orbital inclination precession phase
8 Observations Green Bank Telescope 820 MHz J : ~6 years (~8% P prec ) semi-annual concentrated campaigns 1-2 weeks x ~5-8 hr single-epoch combined profiles J : ~9.5 years + Lovell ~2 years combined 6-month spans
9 PSR J A RDF et al. 2013
10 PSR J A RDF et al. 2013
11 PSR J RDF et al. (2014)
12 Precession and misalignment PSR Precession Period (yr) δ( ) B (years) (4) B (6) J A 75 < 3.2 J B (4) J < 34 J * (-44, +85)
13 Precession and misalignment PSR Precession Period (yr) δ( ) B (years) (4) 95% B (6) J A 75 < 3.2 J B (4) RDF et al. (2014) J < 34 J * (-44, +85)
14 Precession and misalignment PSR Precession 68% 95% Period (yr) δ( ) B (years) (4) B (6) J A 75 < 3.2 J B (4) RDF et al. (2014) J < 34 J * (-44, +85)
15 Precession and misalignment NEW from PALFA! { PSR Lazarus et al. (2016) { Precession Period (yr) δ( ) B (years) (4) B (6) J A 75 < 3.2 J B (4) J < 34 J * (-44, +85) J ? Pulsar mass: 1.65(5) Companion mass: 1.24(5) Eccentricity:
16 PSR B PSR B High eccentricity Large transverse velocity Large spin-orbit misalignment Larger companion mass PSR J PSR J Low eccentricity Low transverse velocity Low spin-orbit misalignment Low companion mass High mass-loss Large pre-natal kick Asymmetric explosion Low mass-loss Low pre-natal kick Symmetric supernova event Type II SN VIOLENT CORE COLLAPSE Electron-capture SN Ultra-stripped Type Ic SN
17 Symmetric supernovae Electron capture: Secondary O-Ne-Mg core overcomes density threshold Electron degeneracy pressure Chandrasekhar mass Collapse! Faster than instability formation timescale Low kicks Critical mass for collapse B mass + binding energy Almost no mass ejected! Ultra-stripped Type Ic: Mass transfer from a He core to compact companion Very fast core collapse, low kick expected Very low ejecta mass Expected range of resulting NS similar to B pulsar and 1756 companion See Tauris et al. (2013), ApJ, 778, L23
18 Double neutron star evolution from geometric constraints Robert Ferdman University of East Anglia Bonn NS Workshop X 14 November 2016
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