Chandra observations of CTA 1 PWN show jet/torus morphology, constrain pulsar velocity to ≲200 km/s, and model low magnetic field with PeV electron cutoff in a young low-efficiency nebula.
On the physics of cold MHD winds from oblique rotators
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
abstract
I show that the self-consistent solution of the problem of MHD plasma flow in magnetosphere of an oblique rotator with an initially split-monopole magnetic field is reduced to the solution of the similar problem for the axisymmetric rotator. All properties of the MHD cold plasma flows from the axisymmetric rotators with the initially split-monopole magnetic field are valid for the oblique rotators as well. Rotational losses of the oblique rotator do not depend on the inclination angle and there is no temporal evolution of this angle. Self-consistent analytical and numerical solutions for the axisymmetric plasma flows obtained earlier show that the rotators can be divided on fast rotators ($\sigma_0/U_0^2 > 1$) and slow rotators ($\sigma_0/U_0^2 < 1$), where $\sigma_0$ is the ratio of the Poynting flux to the matter energy flux in the flow at the equator on the surface of the star, $U_0 = \gamma_0v_0/c$, $v_0$ and $\gamma_0$ are the initial velocity and Lorentz-factor of the plasma. The self-consistent approximate analytical solution for the plasma flow from the oblique rotator is obtained under the condition $\sigma_0/U_0^2 \ll 1$. Implications of these results for radio pulsars are discussed. In particular, I argue that all radio pulsars are apparently the slow rotators ejecting the Poynting dominated relativistic wind.
citation-role summary
background 2
citation-polarity summary
years
2026 4verdicts
UNVERDICTED 4roles
background 2polarities
background 2representative citing papers
2D radiative PIC simulations show multi-sheet reconnection in relativistic pair plasma evolving into Kolmogorov-like turbulence that provides secondary particle acceleration while keeping the high-energy spectrum steep.
A general Grad-Shafranov equation is obtained via differential forms, together with a scalar-field Lagrangian that yields the equation on-shell.
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.
citing papers explorer
-
Chandra X-ray Observations of the Pulsar Wind Nebula within CTA 1
Chandra observations of CTA 1 PWN show jet/torus morphology, constrain pulsar velocity to ≲200 km/s, and model low magnetic field with PeV electron cutoff in a young low-efficiency nebula.
-
Radiative PIC simulations of relativistic pair plasma: multiple interacting current sheets and turbulent evolution
2D radiative PIC simulations show multi-sheet reconnection in relativistic pair plasma evolving into Kolmogorov-like turbulence that provides secondary particle acceleration while keeping the high-energy spectrum steep.
-
General Grad-Shafranov Equation
A general Grad-Shafranov equation is obtained via differential forms, together with a scalar-field Lagrangian that yields the equation on-shell.
-
How many VHE gamma-ray binaries with young pulsars can be observed?
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.