Year: 2014
Type: article
Abstract: Adopting our new method for matching general relativistic, ideal magnetohydrodynamics to its force-free limit, we perform the first systematic simulations of force-free pulsar magnetospheres in general relativity. We endow the neutron star with a general relativistic dipole magnetic field, model the interior with ideal magnetohydrodynamics, and adopt force-free electrodynamics in the exterior. Comparing the spin-down luminosity to its corresponding Minkowski value, we find that general relativistic effects give rise to a modest enhancement: the maximum enhancement for $n=1$ polytropes is $\ensuremath{\sim}23%$. Evolving a rapidly rotating $n=0.5$ polytrope we find an even greater enhancement of $\ensuremath{\sim}35%$. Using our simulation data, we derive fitting formulas for the pulsar spin-down luminosity as a function of the neutron star compaction, angular speed, and dipole magnetic moment. We expect stiffer equations of state and more rapidly spinning neutron stars to lead to even larger enhancements in the spin-down luminosity.
Institution: University of Illinois Urbana-Champaign
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
Awards: G1269417628, G2952167421, Theoretical Studies in Gravitation and Astrophysics, Theoretical Studies in Gravitation and Astrophysics, THE INSPIRAL AND COALESCENCE OF COMPACT BINARY STARS IS ONE OF THE MOST CHALLENGING PROBLEMS IN THEORETICAL ASTROPHYSICS. ONLY RECENTLY HAVE ADVANCES, THE INSPIRAL AND COALESCENCE OF COMPACT BINARY STARS IS ONE OF THE MOST CHALLENGING PROBLEMS IN THEORETICAL ASTROPHYSICS. ONLY RECENTLY HAVE ADVANCES, XSEDE: eXtreme Science and Engineering Discovery Environment
OpenAlex ID: W2033855671