More Like this

1. Fluctuation Dynamo in a Collisionless, Weakly Magnetized Plasma

   https://doi.org/10.3847/2041-8213/aad638  

   St-Onge, Denis A. ; Kunz, Matthew W. ( August 2018 , The Astrophysical Journal)
2. Design of 30-T pulsed magnetic field generator for magnetized high-energy-density plasma experiments

   https://doi.org/10.1103/PhysRevAccelBeams.22.080401  

   Shapovalov, R. V. ; Brent, G. ; Moshier, R. ; Shoup, M. ; Spielman, R. B. ; Gourdain, P.-A. ( August 2019 , Physical Review Accelerators and Beams)
3. Coherent Electromagnetic Emission from Relativistic Magnetized Shocks

   https://doi.org/10.1103/PhysRevLett.127.035101  

   Sironi, Lorenzo ; Plotnikov, Illya ; Nättilä, Joonas ; Beloborodov, Andrei M. ( July 2021 , Physical Review Letters)

   null (Ed.)
4. Heat pump via charge incompressibility in a collisional magnetized multi-ion plasma

   https://doi.org/10.1103/PhysRevE.102.013212  

   Mlodik, M. E. ; Kolmes, E. J. ; Ochs, I. E. ; Fisch, N. J. ( July 2020 , Physical Review E)

   null (Ed.)
5. Can magnetized turbulence set the mass scale of stars?

   https://doi.org/10.1093/mnras/staa1883  

   Guszejnov, Dávid ; Grudić, Michael Y ; Hopkins, Philip F ; Offner, Stella S ; Faucher-Giguère, Claude-André ( August 2020 , Monthly Notices of the Royal Astronomical Society)

   null (Ed.)

   ABSTRACT Understanding the evolution of self-gravitating, isothermal, magnetized gas is crucial for star formation, as these physical processes have been postulated to set the initial mass function (IMF). We present a suite of isothermal magnetohydrodynamic (MHD) simulations using the gizmo code that follow the formation of individual stars in giant molecular clouds (GMCs), spanning a range of Mach numbers found in observed GMCs ($\mathcal {M} \sim 10\!-\!50$). As in past works, the mean and median stellar masses are sensitive to numerical resolution, because they are sensitive to low-mass stars that contribute a vanishing fraction of the overall stellar mass. The mass-weighted median stellar mass M50 becomes insensitive to resolution once turbulent fragmentation is well resolved. Without imposing Larson-like scaling laws, our simulations find $M_\mathrm{50} \,\, \buildrel\propto \over \sim \,\,M_\mathrm{0} \mathcal {M}^{-3} \alpha _\mathrm{turb}\, \mathrm{SFE}^{1/3}$ for GMC mass M0, sonic Mach number $\mathcal {M}$, virial parameter αturb, and star formation efficiency SFE = M⋆/M0. This fit agrees well with previous IMF results from the ramses, orion2, and sphng codes. Although M50 has no significant dependence on the magnetic field strength at the cloud scale, MHD is necessary to prevent a fragmentation cascade that results in non-convergent stellar masses. For initial conditions and SFE similar to star-forming GMCs in our Galaxy, we predict M50 to be $\gt 20 \, \mathrm{M}_{\odot }$, an order of magnitude larger than observed ($\sim 2 \, \mathrm{M}_\odot$), together with an excess of brown dwarfs. Moreover, M50 is sensitive to initial cloud properties and evolves strongly in time within a given cloud, predicting much larger IMF variations than are observationally allowed. We conclude that physics beyond MHD turbulence and gravity are necessary ingredients for the IMF. 

   more » « less