PROPAGATION AND STABILITY OF SUPERLUMINAL WAVES IN PULSAR WINDS

Journal Article · Mon Jul 01 00:00:00 EDT 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/771/1/53· OSTI ID:22140180

Mochol, Iwona

Nonlinear electromagnetic waves with superluminal phase velocity can propagate in the winds around isolated pulsars, and around some pulsars in binary systems. Using a short-wavelength approximation, we find and analyze an integrable system of equations that govern their evolution in spherical geometry. A confined mode is identified that stagnates to finite pressure at large radius and can form a precursor to the termination shock. Using a simplified criterion, we find this mode is stable for most isolated pulsars, but may be unstable if the external pressure is high, such as in the pulsar wind nebulae in starburst galaxies and in W44. Pulsar winds in eccentric binary systems, such as PSR 1259-63, may go through phases with stable and unstable electromagnetic precursors, as well as phases in which the density is too high for these modes to propagate.

• OSTI ID: 22140180
• Journal Information: Astrophysical Journal, Vol. 771, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
APPROXIMATIONS
DENSITY
ELECTROMAGNETIC RADIATION
EQUATIONS
EVOLUTION
GALAXIES
INSTABILITY
NEBULAE
NONLINEAR PROBLEMS
PHASE VELOCITY
PLASMA
PRECURSOR
PULSARS
STABILITY
STARS
STELLAR WINDS
SUPERNOVA REMNANTS
WAVE PROPAGATION
WAVELENGTHS