Pulsars and neutron stars/History of the theoretical understanding of pulsars

Introduction
In this section we first describe advances in the understanding of the interior of neutron stars, then the magnetosphere and emission and finally the pulsar population.

Glitches and the neutron star interior
Even before the discovery of the first pulsar, the existence of neutron stars had been predicted (Baade & Zwicky 1934). It was therefore clear that neutron stars are "made up of neutrons", but it wasn't until the discovery of the first glitch in the vela pulsar that it became possible to directly probe the interior of a neutron star. Baym, Pethick & Pines (1969) showed that matter in the interior of a typical neutron star is a mixture of three degenerate interacting quantum liquids — neutrons, protons and electrons with the neutrons dominating. They suggested that this mixture would be bounded on the inside by a superdense core and on the outside by a solid mantle. They suggested that there would be superfluid states in the interior. They (Baym et al. 1969) then noted that if the glitch in the Vela pulsar was caused by a "star quake" then the event demonstrates that the interior of the pulsar is a superfluid. Their model was able to explain the sudden change in spin-frequency and also the characteristic relaxation of a glitch after the event.

Pines & Alpar (1984) provided a review related to superfluidity in the Vela, Crab and PSR B0525+21 and discussed the possibility of superfluidity in the millisecond pulsar population.


 * Alpar et al. 1984 - vortex creep
 * Alpar, Langer & Sauls (1984) - superfluid core and glitches
 * Pines & Alpar (1985) - superfluidity in neutron stars
 * Alp Alpar, Cheng & Pines (1989) - vortex creep
 * Jones 1991 - neutron-drip superfluid
 * Link, Epstein & van Riper - pulsar glitches
 * Alpar et al. (1994) crust cracking in the Crab
 * Alpar & Baykal 1994 - glitches
 * Bennett, Epstein & Lattimer (1999) - neutron star structure
 * Lyne, Shemar, Smith (2000) - glitch statistics
 * Larson & Link (2001) - glitch simulations
 * Link & Cutler (2002) - vortex unpinning
 * Lattimer & Prakash (2007) - prognosis for equation of state constraints
 * Melatos, Peralta & Wyithe (2008) - Avalanche Dynamics of Radio Pulsar Glitches
 * Warszawski & Melatos (2008) - A cellular automaton model of pulsar glitches
 * Haskell, Pizzochero & Sidery (2012) – pulsar glitches
 * Melatos & Link (2014) - pulsar timing noise from superfluid turbulence
 * Haskell & Antonopoulou (2014) - glitch recoveries in pulsars and magnetars
 * Kantor & Gusakov (2014) - anti-glitches
 * Keer & Jones (2015) - starquakes
 * Melatos & Warszawski (2009) – superfluid vortex unpinning.
 * Mandal et al. (2009) – consideration of glitch in the millisecond pulsar PSR B1821-24.

Pines (1974) showed how observations of pulsars wobbling (free-precession) can be used to study the structure and properties of the associated neutron star.

The pulsar emission and geometry

 * Pacini, 1968
 * Goldstein 1968
 * Radhakrishnan & Cooke
 * Ginzburg et al. 1969
 * Davies 1969
 * Ruderman 1969
 * Ostriker & Gunn 1969
 * Ostriker & Gunn 1969
 * Sutherland et al. 1970
 * Ruderman 1970
 * Goldreich 1970
 * Pacini 1970
 * Sturrock 1970
 * Gil (1985 - sub-microsecond fluctuations in emission
 * Cheng, Ho & Ruderman (1986) - outer gaps
 * Rankin 1990 - geometry
 * Radhakrishan, Rankin (1990) - circular polarisation
 * Romani (1990) - unified model of magnetic fields
 * Thompson, Duncan 1983 - dynamos
 * Chen & Ruderman (1993) - pulsar death lines
 * [http://adsabs.harvard.edu/abs/1995MNRAS.275..255T Thompson, Duncan (1995) - SGRs as magnetized neutron stars
 * Romani & Yadigaroglu 1995 - gamma-ray pulsars - emission zones and viewing geometries
 * Gil, Krawczyk 1996 - pulsar beams - conal not patchy
 * Lyne & Manchester (1988) - the shape of pulsar beams
 * Romani (1996) - gamma-ray pulsars - outermagnetospheres
 * Lyutikov, Blandford, Machabeli (1999) - pulsar radio emission
 * Dyks et al. (2005) - pulsar shadow as double notches
 * Romani & Watters (2010)
 * Kalapotharakos et al. (2012) – pulsar magnetosphere
 * Contopoulos, Kalapotharkos, Kazanas (2014) - a new standard pulsar magnetosphere
 * Machabeli & Chkheidze (2014) - radio emission from the Crab
 * Wang et al. (2014) - fan beam model
 * Szary, Melikidze & Gil (2015) - radio emission from magnetars
 * Vigano et al. (2015) - outer gap model
 * Marelli et al., (2015) - radio-quiet and radio-loud pulsars

The population of neutron stars and pulsars

 * Falnnery & van den Heuvel 1975
 * Radhakrishnan (1984) - the origins of pulsar velocities
 * van den Heuvel & Taam (1984) - evolutionary histories
 * Narayan & Ostriker 1990 - pulsar populations
 * Bhattacharya, van den Heuvel (1991) - formation and evolution of binary and msps
 * van den Heuvel (1992) - pulsar planets
 * [http://adsabs.harvard.edu/abs/1995MNRAS.275L..16L Lorimer, Lyne, Anderson (1995) - the pulsar velocity-magnetic field correlation
 * Lorimer et al. (1995) - the birth rate of msps
 * van Kerkwijk, van Paradijs, Zuiderwijk (1995) - masses of neutron stars
 * Kaspi et al. (1996) - neutron-star birth kicks
 * Cadez, Galicic, Calvani (1997) - free precession
 * Hansen & Phinney (1997) - pulsar kick velocity distribution
 * Spuit & Phinney (1998) - birth kicks as the origin of pulsar rotation
 * Lorimer et al. (1993) - birthrate and initial spin periods
 * Lyne & Lorimer 1994 - pulsar velocities
 * Cheng, Ho & Ruderman (1986) - rapidly spinning pulsars
 * Thorsett & Chakrabarty (1999) - neutron star masses
 * Brazier & Johnston (1999) - implications of radio-quiet neutron stars
 * Chakrabarty et al. (2003) - maximum spin frequency of neutron stars
 * Lattimer & Prakash (2004) - the physics of neutron stars
 * Lipunov et al. (2005) - population of pulsar-blcak hole binaries
 * Hobbs et al. (2005) presented a statistical study of a large number of pulsar proper motions]
 * Cordes et al. (2006) - theory of parabolic arcs
 * Ng & romani (2007) birth kick distributions
 * Zhang et al. (2011) – pulsar masses
 * Tauris & can den Heuvel (2014) - formation of the triple system
 * Bates et al., (2014) - PSRPOPPy
 * Kerr et al., (2015) - limits of planet formation around young pulsars
 * Wielebinski, Vaughan & Large (1969) first suggested that pulsars are galactic objects associated with the galactic disk or spiral arms.
 * The theoretical understanding of the properties of X-ray pulsars was summarised in White, Swank & Holt (1983).
 * Blair & Candy (1985) - X-ray pulsar population and birthrate.
 * Lyne, Manhcester & Taylor (1985) discussed the galactic population of pulsars in detail.
 * Narayan 1987 considered the birthrate and initial spin period of isolated radio pulsars.
 * Theory of planet formation: Rasio, Shapiro & Teukolsky 1992
 * Gonthier et al. (2005) simulated the Gould Belt and showed that pulsars should exist there.

Extra:


 * Ruderman & Sutherland (1975)
 * Backer, Rankin & Campbell (1976)
 * Manchester & Lyne (1977)
 * Arons & Scharlemann (1979)
 * Arons (1981)
 * Curtis (1982)
 * Harding (1983)
 * Friedman (1983)
 * Shapiro, Teukolsky & Wasserman (1983)
 * Rankin (1983)
 * Rankin (1983)
 * Arons (1984)