Results 11 to 20 of about 221 (127)

Dust in and Around the Heliosphere and Astrospheres. [PDF]

Space Sci Rev, 2022
AbstractInterstellar dust particles were discovered in situ, in the solar system, with theUlyssesmission’s dust detector in 1992. Ever since, more interstellar dust particles have been measured inside the solar system by various missions, providing insight into not only the composition of such far-away visitors, but also in their dynamics and ...
Sterken VJ, Baalmann LR, Draine BT, Godenko E, Herbst K, Hsu HW, Hunziker S, Izmodenov V, Lallement R, Slavin JD.   +9 more
europepmc   +5 more sources

3D MHD astrospheres [PDF]

Monthly Notices of the Royal Astronomical Society, 2021
A significative fraction of all massive stars in the MilkyWay move supersonically through their local interstellar medium (ISM), producing bow shock nebulae by wind-ISM interaction. The stability of these observed astrospheres around cool massive stars challenges precedent 2D (magneto-)hydrodynamical (MHD) simulations of their surroundings.
Meyer, Dominique M.-A. (Dr. rer. nat.), Mignone, Andrea, Petrov, Mykola, Scherer, Klaus, Velazquez, Pablo F., Boumis, Panos   +5 more
core   +5 more sources

Examining simulated MHD shock structures of astrospheres

, 2022
In dieser Arbeit werden verschiedene Untersuchungen an magnetohydrodynamischen Modellen von Astrosphären (ASn) präsentiert. Die Schockstrukturen der ASn um vier Sterne, den schnell-laufenden O-Stern \(\lambda\) Cephei, die Sonne, unseren nächsten Nachbarn Proxima Centauri, und den M-Stern LHS 1140, wurden untersucht. Eine Methode zur Projektion von ASn,
Baalmann, Lennart Robin (M. Sc.)
core   +4 more sources

Skymaps of observables of three-dimensional magnetohydrodynamic astrosphere models [PDF]

Astronomy & Astrophysics, 2020
Context. 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. Aims. By projecting selected physical values of three-dimensional models of astrospheres onto the surface of a sphere that is centred on a ...
L. R. Baalmann, K. Scherer, H. Fichtner, J. Kleimann, D. J. Bomans, K. Weis   +5 more
core   +4 more sources

The global structure of astrospheres: Effect of Knudsen number

Publications of the Astronomical Society of Australia
Abstract The interaction between stellar winds and the partially ionized local interstellar medium (LISM) is quite common in astrophysics. However, the main difficulty in describing the neutral components lies in the fact that the mean free path of an interstellar atom, l, can be comparable to the characteristic size of an astrosphere, L (i.e.
Sergey Korolkov, Vladislav Izmodenov
openaire   +3 more sources

Numerical modelling of Astrospheres [PDF]

, 2020
MSc (Astrophysical Sciences), North-West University,Potchefstroom ...
Light, J.
openaire   +2 more sources

Imaging Magnetically Driven Astrospheres: A Forward Modeling Approach

The Astrophysical Journal Letters
An astrosphere is a vast, tailed, bubble-like volume around a star, formed through the interaction between the stellar magnetic field, the stellar wind, and the interstellar medium (ISM).
Ziqi Wu, Tom Van Doorsselaere, Jiansen He, Hugues Sana, Nicholas Jannsen, Tianhang Chen, Weining Wang, Zheng Sun   +7 more
doaj   +3 more sources

Exploration of the heliosphere and astrospheres with HST

AIP Conference Proceedings, 2012
We present some recent results concerning the analysis of Hubble Space Telescope observations of Lyman-α absorption from the heliosphere and astrospheres. We present heliospheric absorption predictions from the first extended-tail 3-D MHD model of the global heliosphere, with kinetic neutrals.
Brian E. Wood, Vladislav V. Izmodenov, Dmitry Alexashov   +2 more
openaire   +2 more sources

The numerical simulation of astrospheric evolution in different interstellar environments [PDF]

, 2023
The interaction between the interstellar medium (ISM) and a stellar wind leads to the formation of an astrosphere. In this study, the evolution of astrospheres is simulated with a two-dimensional spherical hydrodynamic (HD) and magnetohydrodynamic (MHD) model, and a three-dimensional cartesian MHD model.
Marais, Andrea
openaire   +2 more sources

Effects of stellar eruptions throughout astrospheres

, 2016
Stars like the Sun evolve from young, fast-rotating and very active stars to older, slowly rotating main-sequence stars like our own Sun. The changes in stellar magnetic fields and stellar activity of such solar analogs with stellar evolution and the change in their rotation period are described in Ch. 2 of Vol. III.
Ofer Cohen
openaire   +2 more sources