Skymaps of observables of three-dimensional MHD astrosphere models

Abstract

Three-dimensional models of astrospheres have recently become of interest. However, comparisons between these models and observations are non-trivial because of the two-dimensional nature of observations. By projecting selected physical values of three-dimensional models of astrospheres onto the surface of a sphere that is centred on a virtual all-sky observer, these models can be compared to observational data in different observables: the column density, bremsstrahlung flux, rotation measure, H$\alpha$ flux, and synchrotron or cyclotron flux. Projections were calculated by rotating and moving the astrosphere model to the desired position and orientation and by then computing the value of a given patch on the sphere by a modified line-of-sight integration. Contributions to the selected observable made by all model cells that are connected to the patch by the line of sight in question were taken into account. When the model produces a bow shock, a distinct parabolic structure produced by the outer astrosheath can be seen in every observable of the projection, the exact shape depending on the orientations of the line of sight and the stellar motion. Of all four examined astrosphere models, only that of $\lambda$ Cephei shows fluxes that are higher than current observational thresholds. This is due to the strong stellar wind and interstellar inflow of the $\lambda$ Cephei model.

References in corpus (30)

• The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance
• The Spitzer Space Telescope Mission
• LOFAR: The LOw-Frequency ARray
• NLTE line formation of Fe in late-type stars II: 1D spectroscopic stellar parameters
• Pulkovo Compilation of Radial Velocities for 35495 Hipparcos Stars in a Common System
• A new radiative cooling curve based on an up to date plasma emission code
• The Second Data Release of the INT Photometric H-Alpha Survey of the Northern Galactic Plane (IPHAS DR2)
• Properties of Galactic early-type O-supergiants: A combined FUV-UV and optical analysis
• Evidence for an Additional Heat Source in the Warm Ionized Medium of Galaxies
• The Space Weather of Proxima Centauri b
• Accurate determination of the free-free Gaunt factor; I - non-relativistic Gaunt factors
• Powerful Winds from Low-Mass Stars: V374 Peg
• Faraday tomography of the local interstellar medium with LOFAR: Galactic foregrounds towards IC342
• The X-ray Background and AGNs
• Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields
• 3D Simulations of Betelgeuse's Bow Shock
• Bow shock nebulae of hot massive stars in a magnetized medium
• The return of the bow shock
• Can the magnetic field in the Orion arm inhibit the growth of instabilities in the bow shock of Betelgeuse?
• Infrared Photometric Properties of 709 Candidate Stellar Bowshock Nebulae
• The CRONOS Code for Astrophysical Magnetohydrodynamics
• Parameterization of the level-resolved radiative recombination rate coefficients for the SPEX code
• Non-thermal emission from stellar bow shocks
• Modelling interstellar structures around Vela X-1
• Shock structures of astrospheres
• Cosmic rays in astrospheres
• Globally Distributed Energetic Neutral Atom Maps for the "Croissant" Heliosphere
• Possible Association of Two Stellar Bowshocks with Unidentified Fermi Sources
• True versus apparent shapes of bow shocks
• Comic ray flux anisotropies caused by astrospheres

Cited by in corpus (5)

• Simulating observable structures due to a perturbed interstellar medium in front of astrospheric bow shocks in 3D MHD
• Rectangular core-collapse supernova remnants: application to Puppis A
• Mixing of materials in magnetised core-collapse supernova remnants
• Modelling O-star astrospheres with different relative speeds between the ISM and the star: 2D and 3D MHD model comparison
• Modeling the astrosphere of LHS~1140