Constraining the Equation of State with Moment of Inertia Measurements

By J. Lattimer, Bernard F. Schutz. 2004

336 citations recorded by the source corpus.

We estimate that the moment of inertia of star A in the recently discovered double pulsar system PSR J0737-3039 may be determined after a few years of observation to ~10% accuracy. This would enable accurate estimates of the radius of the star and the pressure of matter in the vicinity of 1-2 times the nuclear saturation density, which would in turn provide strong constraints on the equation of state of neutron stars and the physics of their interiors.

Subfields: Astronomy and Astrophysics, Oceanography, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/216a2b8c1ef3ff3810908c49c3522ef1160ffd87

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Oceanography

In Statistical and Nonlinear Physics

Citations in the corpus

The diversity of transients from magnetar birth in core collapse supernovae (2015, background): “The rotational energy of a NS of gravitational mass Mns is given by Erot = IΩ2/2 ' 2.5 × 1052(Mns/1.4M )3/2P−2ms erg, (1) where P = 2π/Ω = Pms ms is the rotational period and I ' 1.3 × 1045(Mns/1.4M )3/2 g cm2 is the NS moment of inertia (Lattimer & Schutz 2005).”
Maximum mass, moment of inertia and compactness of relativistic stars (2016, methodology): “(A2) Assuming ∆M = 0 = ∆ã1 = ∆ã4, as in Lattimer & Schutz (2005), the error in the moment of inertia is ∆I = [( ∂I ∂ã0 )2 (∆ã0) 2 + ( ∂I ∂R )2 (∆R)2 ]1/2 .”
THE EQUATION OF STATE FROM OBSERVED MASSES AND RADII OF NEUTRON STARS (2010, background): “These include neutron star seismology (Samuelsson & Andersson 2007; Steiner & Watts 2009), pulse profiles in X-ray pulsars (Leahy et al. 2009; Morsink & Leahy 2009), and momentof inertia measurements in relativistic binaries (Lattimer & Schutz 2005).”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “A decade later, Bejger and Haensel [62] and then Lattimer and Schutz [67] studied the relation between C and ĪC2 = I/(MR2) (motivated by the fact that I ∝ MR2 for Newtonian polytropes).”
Born–Infeld inspired modifications of gravity (2017, background): “In particular, a correlation between the scaled moment of inertia I/MR2 and the compactness M/R has been observed [57, 239].”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “Assuming a final neutron star mass and radius of M = 1.67M and R = 12 km respectively, we obtain a moment of inertia of about I ≈ 2×1045 g cm2 from the fit formula of (Lattimer & Schutz 2005), I ≈ 0.237MgravR2 1 + 4.2 ( Mgrav kmM R ) + 90 ( Mgrav km M R )4 .”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “…mass Mgrav and assuming a neutron star radius of R = 12 km, we compute the corresponding final final neutron star spin period using the fit formula of Lattimer & Schutz (2005) for the moment of inertia of cold neutron stars, I = 0.237MgravR2 1 + 4.2 ( Mgrav kmM R ) + 90 ( Mgrav km M R )4 .”
RELATIVISTIC MEASUREMENTS FROM TIMING THE BINARY PULSAR PSR B1913+16 (2016, background): “At this point, the spin-orbit term would be calculable, leading to an exciting measurement of the pulsar’s moment of inertia, which has important implications for neutron star equations of state (Lattimer & Schutz 2005).”
The Magnetar Model for Type I Superluminous Supernovae. I. Bayesian Analysis of the Full Multicolor Light-curve Sample with MOSFiT (2017, neutral): “In this case, the rotational energy of the magnetar (for plausible neutron star equations of state; see Lattimer & Schutz 2005) is w= = ´ - ⎜ ⎟ ⎛ ⎝⎜ ⎞ ⎠⎟ ⎛ ⎝ ⎞ ⎠ ( )E I M M P1 2 2.6 10 1.4 1 ms erg, 3mag 2 52 NS 3 2 2 and it spins down on a timescale of = ´ ^ - ⎜ ⎟ ⎜ ⎟ ⎛ ⎝⎜ ⎞ ⎠⎟ ⎛ ⎝ ⎞ ⎠ ⎛ ⎝ ⎞…”
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, methodology): “Such a measurement would provide further constraints on the EoS, particularly at ∼ 2×ρsat (Lattimer & Schutz 2005), but sufficiently precise observations are expected to be some years away (Lattimer & Prakash 2016).”