Results 21 to 30 of about 36,797 (212)
, 2015 The winds of massive stars create large (>10 pc) bubbles around their progenitors. As these bubbles expand they encounter the interstellar coherent magnetic field which, depending on its strength, can influence the shape of the bubble.
Marcowith, Alexandre +2 more
core +3 more sources
FAST Polarization Mapping of the Supernova Remnant VRO 42.05.01
The Astrophysical Journal, 2023 We have obtained the polarization data cube of the supernova remnant (SNR) VRO 42.05.01 at 1240 MHz using the Five-hundred-meter Aperture Spherical Radio Telescope (FAST).
Li Xiao +4 more
doaj +1 more source
Magnetic Fields in Interstellar Masers [PDF]
Symposium - International Astronomical Union, 1990 Zeeman splitting in the spectra of molecular masers that arise in the envelopes of newly formed stars (called interstellar masers) offers a method of estimating the magnetic field in these dense regions (106–1011 cm−3). The magnetic field strengths in regions of OH and H2O masers scale as the square root of the density when compared to the density and ...
openaire +1 more source
Obtaining the Strength of the Magnetic Field from E- and B-Modes of Dust Polarization
The Astrophysical Journal, 2023 We perform numerical simulations of supersonic magnetohydrodynamic (MHD) turbulence and calculate Fourier power spectra of E - and B -modes arising from dust polarization. We pay close attention to the ratio of E -mode to B -mode spectra (a.k.a.
Jungyeon Cho
doaj +1 more source
Biermann Mechanism in Primordial Supernova Remnant and Seed Fields
, 2006 We have studied the generation of magnetic fields by the Biermann mechanism in the pair-instability supernovae explosions of the first stars. The Biermann mechanism produces magnetic fields in the shocked region between the bubble and interstellar medium
Abel +29 more
core +1 more source
Interstellar turbulent magnetic field generation by plasma instabilities [PDF]
Astrophysics and Space Science, 2013 The maximum magnetic field strength generated by Weibel-type plasma instabilities is estimated for typical conditions in the interstellar medium. The relevant kinetic dispersion relations are evaluated by conducting a parameter study both for Maxwellian and for suprathermal particle distributions showing that micro Gauss magnetic fields can be ...
Tautz, R. C., Triptow, J.
openaire +2 more sources
The Astrophysical JournalWe report the detection of the ordered alignment between the magnetic field and kpc-scale bubbles in the nearby spiral galaxy, NGC 628. Applying the Velocity Gradient Technique on CO spectroscopic data from the ALMA-PHANGS, the magnetic field of NGC 628 ...
Mengke Zhao +11 more
doaj +1 more source
The Orientation of the Local Interstellar Magnetic Field [PDF]
Science, 2007 The orientation of the local interstellar magnetic field introduces asymmetries in the heliosphere that affect the location of heliospheric radio emissions and the streaming direction of ions from the termination shock of the solar wind. We combined observations of radio emissions and energetic particle streaming with extensive three-dimensional ...
Opher, M., Stone, E. C., Gombosi, T. I.
openaire +4 more sources
Energy Landscapes in Chemical Reactions and Transport
ChemPhysChem, Volume 26, Issue 6, March 15, 2025.Kinetics/dynamics of chemical reactivity and transport of chemical species in a solid are both determined by the energy landscape in which they take place. Discussing common grounds but also distinct differences may help in advancing the understanding in both fields.
Karl‐Michael Weitzel
wiley +1 more source
MHD flows at astropauses and in astrotails [PDF]
, 2014 The geometrical shapes and the physical properties of stellar wind -- interstellar medium interaction regions form an important stage for studying stellar winds and their embedded magnetic fields as well as cosmic ray modulation. Our goal is to provide a
Karlicky, Marian +3 more
core +2 more sources