ABSTRACT Stars form from the gravitational collapse of turbulent, magnetized molecular cloud cores. Our non-ideal MHD simulations reveal that intrinsically anisotropic magnetic resistance to gravity during core naturally generates dense gravomagneto sheetlets within inner protostellar envelopes – disrupted versions classical sheet-like pseudo-discs. They are embedded in a magnetically dominant background, where less materials flow along local field lines and accumulate sheetlets. The...

Abstract The streaming instability (SI) is one of the most promising pathways to formation planetesimals from pebbles. Understanding how this operates under realistic conditions expected in protoplanetary disks (PPDs) therefore crucial assess efficiency planet formation. Contemporary models PPDs show that magnetic fields are key driving gas accretion through large-scale, laminar stresses. However, effect such on SI has not been examined detail. To end, we study stability dusty, magneftized a...

ABSTRACT Rings and gaps are routinely observed in the dust continuum emission of protoplanetary discs (PPDs). How they form evolve remains debated. Previous studies have demonstrated possibility spontaneous gas rings formation wind-launching discs. Here, we show that such substructures unstable to Rossby wave instability (RWI) through numerical simulations. Specifically, shorter wavelength azimuthal modes develop earlier, longer ones dominate later, forming elongated (arc-like) anticyclonic...

Abstract The streaming instability (SI) is one of the most promising candidates for triggering planetesimal formation by producing dense dust clumps that undergo gravitational collapse. Understanding how SI operates in realistic protoplanetary disks (PPDs) therefore crucial to assess efficiency formation. Modern models PPDs show large-scale magnetic torques or winds can drive laminar gas accretion near disk midplane. In a previous study, we identified new linear dust-gas instability,...

The majority of stars are in binary/multiple systems. How such systems form turbulent, magnetized cores molecular clouds the presence non-ideal MHD effects remains relatively under-explored. Through ATHENA++-based AMR simulations with ambipolar diffusion, we show that collapsing protostellar envelope is dominated by dense gravo-magneto-sheetlets, a turbulence-warped version classic pseudodisk produced anisotropic magnetic resistance to gravitational collapse, agreement previous single-star...

Rings and gaps are routinely observed in the dust continuum emission of protoplanetary discs (PPDs). How they form evolve remains debated. Previous studies have demonstrated possibility spontaneous gas rings formation wind-launching disks. Here, we show that such substructures unstable to Rossby Wave Instability (RWI) through numerical simulations. Specifically, shorter wavelength azimuthal modes develop earlier, longer ones dominate later, forming elongated (arc-like) anti-cyclonic vortices...

ABSTRACT The majority of stars are in binary/multiple systems. How such systems form turbulent, magnetized cores molecular clouds the presence non-ideal magnetohydrodynamic (MHD) effects remains relatively underexplored. Through athena++-based MHD adaptive mesh refinement simulations with ambipolar diffusion, we show that collapsing protostellar envelope is dominated by dense gravo-magneto-sheetlets, a turbulence-warped version classic pseudodisc produced anisotropic magnetic resistance to...

Fast, collimated jets are ubiquitous features of young stellar objects (YSOs). They generally thought to be powered by disk accretion, but the details debated. Through 2D (axisymmetric) MHD simulations, we find that a fast ($>100$~km/s) bipolar jet is continuously driven along north and south poles circumstellar initially magnetized large-scale open poloidal field contains thermally ionized inner magnetically active zone surrounded dead zone. The primarily magneto-centrifugally release...

Abstract Fast, collimated jets are ubiquitous features of young stellar objects. They generally thought to be powered by disk accretion, but the details debated. Through 2D (axisymmetric) MHD simulations, we find that a fast (>100 km s −1 ) bipolar jet is continuously driven along north and south poles circumstellar initially magnetized large-scale open poloidal field contains thermally ionized inner magnetically active zone surrounded dead zone. The primarily magnetocentrifugally release...

Stars form from the gravitational collapse of turbulent, magnetized molecular cloud cores. Our non-ideal MHD simulations reveal that intrinsically anisotropic magnetic resistance to gravity during core naturally generates dense gravo-magneto-sheetlets within inner protostellar envelopes -- disrupted versions classical sheet-like pseudodisks. They are embedded in a magnetically dominant background, where less materials flow along local field lines and accumulate sheetlets. The sheetlets,...

The streaming instability (SI) is one of the most promising candidates for triggering planetesimal formation by producing dense dust clumps that undergo gravitational collapse. Understanding how SI operates in realistic protoplanetary disks (PPDs) therefore crucial to assess efficiency formation. Modern models PPDs show large-scale magnetic torques or winds can drive laminar gas accretion near disk midplane. In a previous study, we identified new linear dust-gas instability, azimuthal drift...