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observations have revealed the presence and topology of magnetic fields on the surfaces of some main sequence massive stars. these stars possess a convective core that supports strong dynamo action. this core is linked to the dynamics of the rest of the star through overshooting convection and magnetic fields and may i... | super-equipartition convective dynamo action in the cores of b-type stars |
we examine how 3d mhd simulations can deliver clues on the mechanisms at the origin of angular momentum loss saturation of rapidly rotating solar-like stars. based on a study of six targets, whose magnetic field has been observed by zeeman doppler imaging (zdi), we find that the saturation could be explained by a extre... | spin evolution and saturation: new insights through 3d mhd simulations of young solar analogs |
the saturation and nonlinear evolution of the spatial spectrum of the weibel instability, which is caused by an anisotropy of the particle velocity distribution and generates quasi-magnetostatic turbulence during various transient processes, are important for a wide class of phenomena in the nonequilibrium cosmic and l... | saturated magnetic field of the weibel tm-instability and dynamics of its spatial spectrum in a plasma with the anisotropic kappa or maxwellian distribution of electrons |
our understanding of large-scale magnetic fields in stellar radiative zones remains fragmented and incomplete. such fields, which must be produced by some form of dynamo mechanism, are thought to dominate angular-momentum transport, making them crucial to stellar evolution more generally. a major difficulty is the effe... | large-scale dynamo with stable stratification: the magnetic shear-current effect |
the role played by magnetic fields in high-mass star formation is not yet fully clear. theoretical simulations have shown that magnetic fields appear to suppress fragmentation in the star forming cloud, to enhance accretion via disc and to provide feedback in the form of outflows and jets. however, models require speci... | methanol masers reveal the magnetic field of a high mass protostar |
star formation in giant molecular clouds (gmcs) is of fundamental importance to our understanding of star formation in our universe since it is in these massive, transient objects where almost all stars are formed. to understand the process of star formation in gmcs one must understand how star formation feedback from ... | the dynamics of stellar wind-driven bubbles and their effect on star formation in giant molecular clouds |
simulations of the terrestrial paleo-magnetosphere for early stages of the solar system are of particular importance for studying the evolution and mass loss of the earth's atmosphere. within this presentation, we will present simulations of the paleo-magnetosphere of the earth for the late hadean, i.e. for ~4.1 billio... | on the earth's paleo-magnetosphere for the late hadean eon |
magnetars are neutron stars with ultra strong magnetic fields, $b\sim 10^{14\text{-}15} \text{g}$, and their high surface luminosity, $l_{s}\sim 10^{35} \text{erg} \text{s}^{-1}$, is a direct evidence of their magnetic activity. for a young magnetar, with internal temperatures $t\gtrsim10^{9} \text{k}$, particles in th... | magneto-thermal evolution of neutron star cores in the "strong-coupling regime" |
understanding the magnetic field strength and morphology of astrophysical regions is of great importance in understanding their dynamics. there exist a number of methods astronomers can employ to trace magnetic field structures, and each have their own limitations. a promising technique to trace the magnetic field morp... | tracing cosmic magnetic fields using molecules |
observations of agn feedback have been revolutionized in recent years by the direct detection of galaxy-scale outflows driven by supermassive black holes. these agndriven galactic winds are now observed in several observational windows, including emission and absorption in the uv, optical, x-ray, radio, and far ir. the... | the physics, observational signatures, and consequences of agn-driven galactic winds |
for a few million years after the gravitational collapse that led to their formation; young stellar systems remain surrounded by a circumstellar disk from which planets form. alma and vlt/sphere have provided spectacular images of the planet-forming disks on a scale of a few 10 au (garufi et al. 2017) and; even more re... | a sub-au study of ci tau with gravity: the key to connect stars, disks and planets |
the dissipation of the kinetic energy of large-scale and wave-like tidal flows within the convective envelope of low-mass stars is one of the key physical mechanisms that shape the orbital and rotational dynamics of short-period exoplanetary systems. in the case of stable binary systems, they lead to the orbit circular... | do magnetic fields modify tidal dissipation in the convective envelope of low-mass stars along their evolution? |
in the age of the kepler space telescope and other exoplanet finding missions, a variety of exotic planets have been discovered. some of these planets have been found to be in binary star systems --- systems which have historically been overlooked in planet formation models. this is due to the single star scenario bein... | the formation, evolution, and survivability of discs around young binary stars |
the first multi-messenger observation of a binary neutron star merger has already lead to first constraints on the nuclear matter equation of state. to make the most out of the observational data, however, the theoretical modeling of the merger process needs to be improved further. among other ingredients, the evolutio... | numerical inside view of hypermassive remnant models for gw170817 |
conservation of magnetic flux is associated with regions of the powerful magnetic fields (b ∽ 1013 g) near neutron stars' surface. the vector potential generated by moving electric charge q is uniformly distributed within a neutron star's surface (radius r). the evolution of the magnetic field of isolated neutron stars... | magnetic dipole interaction with multipole magnetic field lines of neutron stars |
the evolution of protoplanetary disks is believed to be driven largely by viscosity. the ionization of the disk that gives rise to viscosity is caused by x-rays from the central star or by energetic particles released by shock waves travelling into the circumstellar medium. we have performed test-particle numerical sim... | local protoplanetary disk ionisation by t tauri star energetic particles |
filaments are ubiquitous in the interstellar medium, yet their formation, internal structure, magnetic properties, and longevity have not been analysed in detail. in this thesis i report the results from a comprehensive numerical study that investigates the characteristics, formation, dynamics, and global evolution of ... | magnetohydrodynamics of wind-cloud interactions: filament formation in the interstellar medium |
although the origin of molecular cloud turbulence remains debated, one possibility is that stellar feedback injects enough energy to drive observed motions on parsec scales. to investigate this possibility, we use magnetohydrodynamic simulations where we vary the stellar mass-loss rates and magnetic field strength. we ... | quantifying the impact of stellar feedback on molecular clouds |
we present results for magnetohydrodynamical simulations of evolving neutron stars in the first moments of its lifetime. we study the poloidal field instability and how the magnetic field components change with time. we find that although our final field does not reach a stable equilibrium, it settles to a twisted toru... | simulating magnetic field evolution in isolated neutron stars |
the activity of stars governs the environment of (exo) planetary systems with implications for habitability. star-planet interactions are primarily mediated via variable stellar radiation, particle fluxes and magnetized stellar winds. the nature of planetary magnetospheres and properties of stellar winds, in particular... | impact of evolving stellar activity on (exo)planetary environments |
collisions between giant molecular clouds (gmcs) have been proposed as a mechanism to compress gas to trigger the birth of massive star clusters and associations and thus be potentially relevant to the formation of most stars in galaxies. the spatial distributions of dense gas cores within protoclusters generated by su... | cores and filaments in mhd simulations of massive protoclusters |
red supergiants (rsg) and asymptotic giant branch (agb) stars produce strong stellar winds, which are not well understood. these winds have a key role in the enrichment of the interstellar medium with chemical elements, which are the building blocks for the next generation of stars. the magnetic field in such stars cou... | the role of convection and magnetic field in the mass loss of evolved cool stars |
this thesis focuses on bridging the gap between solar and stellar physics through the study of flares. solar flares are the most powerful explosions in the solar system and many stellar flares have been observed to be orders of magnitudes larger. however, is not yet known if these phenomena are formed through the same ... | solar and stellar flares and their connection |
i will present new results on magnetar-like transient events in neutron stars having low dipolar fields or generally catalogued as normal radio pulsars or central compact objects. i will then present simulations of magnetic field evolution that might explain the apparently puzzling behaviour of these objects. strong su... | magnetar-like emission in different neutron star classes |
bow shock formation, magnetic reconnection and plasmoid ejection are thought to be present in most planetary environments. the aim of this work is to show that the presence of this kind of structures in the vicinity of planets is not restrictive to magnetized bodies. the presence of a interplanetary magnetic field carr... | numerical simulation of the interaction between planetary exospheres and the stellar wind |
energy and momentum coupling between spatially separate but magnetically linked plasmas is a key aspect of space physics. previous active plasma experiments (e.g., apex north star [pfaff et al., 2004]) showed the presence of parallel electric fields that are assumed to facilitate the cross-field "skidding" of the combi... | kinetic-scale energy and momentum transport experiment (kinet-x): expectations for ion and electron heating |
plasma ions heating (especially minor heavy ions preferential heating) in fast solar wind and solar corona is an open question in space physics. however, alfvén waves have been always considered as a candidate of energy source for corona heating. in this paper, by using a two-dimensional (2-d) hybrid simulation model i... | parametric instabilities and particles heating of circularly polarized alfvén waves with an incoherent spectrum: two-dimensional hybrid simulations |
plasma is the most abundant form of visible matter in the universe. plasmas make up approximately 99 percent of stellar objects observed including billions of stars and nebulae. high-energy-density (hed) physics is a rapidly growing area of physics that encompasses several disciplines including plasma-, condensed-matte... | investigations of plasma evolution in laser ablation z-pinch experiments using time-resolved optical spectroscopy |
massive stars are amongst the rarest but also most intriguing stars. their extreme, magnetised stellar winds induce, by wind-ism interaction, famous multi-wavelengths circumstellar gas nebulae of various morphologies, spanning from large-scale wind bubbles to stellar wind bow shocks, rings and bipolar shapes. we presen... | magnetised gas nebulae of evolved massive stars |
the merger of two carbon-oxygen white dwarfs has long been theorized to lead to a massive carbon-oxygen or oxygen-neon white dwarf, accretion-induced collapse to a neutron star, or a type ia supernova. determining which mergers lead to a particular outcome requires hydrodynamic simulations of the merging process. i giv... | the physics and end-products of merging co wd binaries |
we present the results of numerical magnetohydrodynamic (mhd) simulations of the isothermal stage of the collapse of magnetic rotating protostellar clouds of solar mass at various initial values of rotational and magnetic energies and with various degrees of nonuniformity. the simulations are carried out using the two-... | evolution of angular momentum during the collapse of magnetic rotating protostellar clouds |
we know that when two neutron stars the dense, compact cores of evolved stars collide, they produce signals that span the electromagnetic spectrum. but could these binaries also flare before they merge, as well?a broad range of signalsartists impression of the collision and merger of two neutron stars. [nsf/ligo/sonoma... | signs of collisions to come |
in order to explain the higher spin down rate of the intermittent pulsar psr b1931+24 in the radio-on state than that in the radio-off state, and to simulate the rotation evolution of the crab pulsar, the wind braking model in the annular acceleration gap considering both core and annular region with different accelera... | wind braking model of pulsars in the case of annular acceleration gap |
an important phenomenon in a pulsing agb (asymptotic giant branch) star is the variability of its circumstellar envelope. the study of stimulated radiation called sio maser (microwave amplification by stimulated emission of radiation) in the inner edge of the envelope shows fluctuations in polarization during the stell... | maser polarization simulation in the circumstellar envelope of an evolving star |
the removal of the ism of disk galaxies through ram pressure stripping (rps) has been extensively studied in numerous simulations. these models show that this process has a significant impact on galaxy evolution (the truncation of the ism will lead to a decrease in the star formation and the galaxy will become redder).... | mhd simulations of ram pressure stripping of a disk galaxy |
stable magnetic fields have been observed in intermediate-mass stars in the main-sequence (ap/bp stars) and in degenerate stars (white dwarfs and neutron stars). despite the important role that the magnetic field plays in the stellar evolution, its origin, internal structure and the way it can survive timescales as lon... | stellar magnetic equilibria with the pencil code |
stellar feedback occurring at small-scales can significantly impact the evolution of galaxies at much larger scales. for example, an appropriate feedback mechanism, including thermal and radiative components, can help regulate star formation, particularly in low-mass galaxies. while feedback models are generally preval... | magnetic field seeding through supernova feedback |
the traditional paradigm for magnetic field lines changing connections ignores magnetic field line chaos and requires an extremely large current density, $j_{max}\propto r_m$, flowing in thin sheets of thickness $1/r_m$, where $r_m$ is the magnetic reynolds number. the time required for a general natural evolution to t... | judgment of paradigms for magnetic reconnection in coronal loops |
ranging from dense plasmas above nuclear saturation in their interiors to strongly magnetized pair-plasmas in their magnetospheres, neutron stars feature some of the most extreme plasmas in the universe. the delicate interplay between strong gravity, nuclear and plasma physics makes the collision of two neutron stars a... | simulating extreme plasmas in neutron star mergers and beyond |
black-hole binary (bhb) mergers are expected to be powerful sources of gravitational radiation at stellar and galactic scales. a typical astrophysical environment for these mergers will involve magnetized plasmas accreting onto each hole; the strong-field gravitational dynamics of the merger may churn this plasma in wa... | robust grmhd evolutions of merging black-hole binaries in magnetized plasma |
feedback processes from massive stars plays a critical role in their formation, destroy the molecular clouds in which they are born and shape the evolution of galaxies. in this talk i will discuss our recent 3d amr simulations that are the first to include the coupled feedback effects of protostellar outflows combined ... | the coupled effects of protostellar outflows, radiation feedback, magnetic fields and turbulence on the formation of massive stars and orion-like clusters |
we review theoretical models for the formation of dense cores in molecular clouds and their subsequent collapse. fragmentation of molecular clouds is affected by many ambient conditions including magnetic fields and background turbulence. we review the outcome of a wide range of simulations and focus in on the origin o... | molecular cloud fragmentation and core collapse |
a primary goal of the open-source spectre project is to simulate the disruption of neutron stars in compact-object binary systems. as a step towards this goal, we present the evolution of a relativistic magnetized accretion disk in a fixed gravitational field. the evolution uses a hybrid scheme of a discontinuous galer... | evolution of a magnetized accretion disk using spectre |
grb 170817a provided clear evidence of an intrinsic connection between short gamma-ray bursts (sgrbs) and binary neutron star (bns) mergers. the mechanism by which the latter are able to feed the former, however, remains poorly understood, and many theoretical and phenomenological models, combining observational data w... | simulating short gamma-ray burst jets with genuine surrounding environments |
the intrinsic magnetic field of a terrestrial planet is considered to be an important factor for the evolution of terrestrial atmospheres. this is in particular relevant for early stages of the solar system, in which the solar wind as well as the euv flux from the young sun were significantly stronger than at present-d... | on the paleo-magnetospheres of earth and mars |
this proposal is the continuation of a previous 3-year project that focused on modeling the nonthermal emission from magnetars and pulsars and testing the models against new observations, in particular by nustar. the proposed project develops in two directions: (1) first-principle simulations of the magnetospheric elec... | activity of strongly magnetized neutron stars |
we present new fully general relativistic magnetohydrodynamic (grmhd) simulations of the merger of high-mass binary neutron star (bns) systems. we considered bnss that produce an hypermassive neutron star that promptly collapses to a spinning black hole (bh) surrounded by a magnetized accretion disk. we investigated wh... | high-mass magnetized binary neutron star mergers and short gamma-ray bursts |
observations of lunar regolith composition have revealed the need for a source that differs in the abundance of light volatile elements (like h, he, c, n, and some noble gases) from the solar wind. mass supply from earth's atmosphere has been previously proposed as one possibility if the earth incurred phases of vanish... | investigating the influence of an unmagnetized versus magnetized earth on the relative solar wind and earth atmosphere contributions to lunar soil |
magnetized stellar plasma winds play a critical role in defining and shaping planetary magnetospheres. the dynamics of star planet interactions are different for planets with and without intrinsic large-scale magnetic fields. magnetohydrodynamic models provide the physical basis for understanding such interactions on t... | solar-stellar winds and the dynamics of star-planet interactions in mars-like planets |
the age-dependent activity of a star dictates the extent of its planetary impact. we study the interaction of the stellar wind produced by solar-like stars with the magnetosphere of earth-like planets using three dimensional (3d) magnetohydrodynamic (mhd) simulations. the numerical simulations reveal important features... | the activity evolution of solar-like stars with age and its planetary impact |
the pipe nebula is a nearby filamentary shaped molecular cloud in which star formation is concentrated in the western end of the cloud known as b59, while the eastern part has no star formation. the morphology of the projected magnetic fields is well constrained through both extinction and emission dust polarization me... | challenging the dense core identification in a strongly dynamical, magnetized and turbulent region of the pipe nebula. |
the merger of two carbon-oxygen white dwarfs (co wds) can either create a more massive wd, lead to collapse into a neutron star, or explode spectacularly as a thermonuclear, or type ia, supernova (sn ia). it has traditionally been believed that sne ia result only from mergers at or above the chandrasekhar mass (mch), a... | illuminating mergers of carbon-oxygen white dwarfs and their possible link to thermonuclear supernovae |
we present recent improvements in general relativistic hydrodynamics simulations with the open source numerical relativity code spectre. major updates include support for tabulated equations of states, implementation of higher-order and positivity-preserving adaptive order finite difference schemes in our discontinuous... | progress in grmhd simulations with spectre |
recent advances in numerical techniques and computational power have allowed us to simulate the pulsar magnetosphere from first principles using particle-in-cell techniques. these ab-initio simulations seem to indicate that pair creation through photon-photon collision at the light cylinder is required to sustain the p... | numerical experiments on magnetospheres of weak pulsars |
although a triangular vortex lattice is stable in a bulk type-ii superconductor, exotic vortex configurations are expected to appear in a small superconducting plate. theoretical calculations on vortex structures in a star-shaped superconducting plate have been given in our preceding work. in this work, we extended our... | simulations of vortices in a star-shaped plate with an artificial pin |
magnetohydrodynamic turbulence is central to laboratory and astrophysical plasmas, and is invoked for interpreting many observed scalings. verifying predicted scaling law behaviour requires extreme-resolution direct numerical simulations (dns), with needed computing resources excluding systematic parameter surveys. we ... | bxc: a swift generator for 3d magnetohydrodynamic turbulence |
buoyantly driven convection under the strong influence of rotation is a ubiquitous feature of geophysical and astrophysical fluid flows. it is known to be a principal ingredient in the generation of observable large-scale shear flows and magnetic fields within planetary and stellar interiors. the constraint of geostrop... | rotationally constrained convection in extreme parameter regimes |
m dwarf habitable zones move inward with time over the star's extended pre-main sequence phase such that rocky planets that are currently orbiting in an m dwarf's habitable zone may have once orbited interior to it. before the habitable zone contracts to envelop the planet, the planet will likely be in a runaway greenh... | carbon dioxide outgassing constrains the habitability of rocky planets after their host m dwarf's pre-main sequence phase |
magnetic fields play an essential role in the star formation process. however, due to challenges in directly observing magnetic fields, the morphology and evolution of magnetic fields within young cores are not well constrained. in order to discriminate between different star formation models, we have analyzed magnetoh... | using synthetic observations to constrain the properties of magnetic fields in protostellar cores |
cosmic rays (crs) play an important role in galaxy formation and evolution: in the interstellar medium, their energy density is roughly in equipartition with magnetic and thermal energy densities of the gas, and their production may contribute to feedback regulating star formation. crs primarily exchange energy and mom... | realistic thermodynamics for cosmic-ray-driven galactic winds |
in strongly-magnetized neutron star crusts (b <= 1014 g), electrons are quantized into a moderate number of landau levels. this can dramatically change the thermodynamic (specific heat capacity, magnetization, differential magnetic susceptibility) and transport properties (electrical and thermal conductivity) of the... | numerical simulations of hall magnetohydrodynamics in neutron star crusts with landau-quantized electrons |
we examine the long-term evolution of accretion tori around the black hole remnants of compact object mergers involving at least one neutron star, to better understand the role of secular outflows in the creation of kilonovae and the synthesis of r-process elements. we modify the flash code to evolve magnetohydrodynami... | long term 3d-mhd simulations of neutron star merger accretion tori with realistic microphysics |
most studies of the 3d density structure of prestellar cores have used isotropic evolution models, which are projected into 2d for direct comparison with observation data. in this study, we introduced the anisotropic inverse abel transform method for reconstructing the 3d volume density profile of prestellar cores. we ... | reconstructing the volume density profile of prestellar cores with the anisotropic inverse abel transform method |
the hubble tension between early universe and local measurements of h0 can be resolved by a brief episode of dark energy contributing about 10% of cosmic energy density at redshift z ~ 3500. new n-body simulations have shown that this early dark energy scenario predicts earlier structure formation, e.g. 50% more cluste... | julius edgar lilienfeld prize (2020): new challenges in cosmology, galaxy formation, and planets |
this review describes realistic evolution of magnetic field and rotation of the protostars, dynamics of outflows and jets, and the formation and evolution of protoplanetary disks. recent advances in the protostellar collapse simulations cover a huge dynamic range from molecular cloud core density to stellar density in ... | low-mass star formation: from molecular cloud cores to protostars and protoplanetary disks |
the first billion years of the universe are marked by a major transition: the epoch of reionisation. both the reionisation of the intergalactic medium and the regulation of galaxy growth are ruled by feedback mechanisms, but the nature and the interplay of these feedback processes remain undetermined. cosmic rays (crs)... | the impact of cosmic ray feedback on the reionisation of the universe |
simulations of the earth's magnetosphere obstacle, including the shape of the auroral oval and related field lines for early stages of the solar system are of particular importance for studying the evolution and mass loss of the earth's atmosphere. within this presentation, we will present simulations of the terrestria... | simulation of the earth's paleo-magnetosphere for the late hadean eon |
magnetic fields have only recently been included in theoretical simulations of high-mass star formation. the simulations show that magnetic fields can play a crucial role not only in the formation and dynamics of molecular outflows, but also in the evolution of circumstellar disks. therefore, new measurements of magnet... | magnetic field measurements at milliarcsecond resolution around massive young stellar objects |
the first stars in the universe, known as population iii stars, formed just a few hundred million years after the big bang. while researchers expect that most population iii stars led bright, brief lives, those with masses less than 0.8 solar mass would still be shining faintly today. can magnetic fields in the early u... | simulations suggest magnetic fields made the first stars form solo |
durring their formation, most young stars are surrounded by a protoplanetary disc. the angular momentum evolution of these system is quite complex but still poorly understood despite a lot of effort and some recent breakthrough. observations indicate that stars with a disc tend to rotate more slowly even though they ac... | stars and their disc - a short but complex story |
significant advances have been made over the past decade in the characterization of multiple protostar systems, enabled by the karl g. jansky very large array (vla), high-resolution infrared observations with the hubble space telescope, and ground-based facilities. to further understand the mechanism(s) of multiple sta... | astro2020 science white paper: the formation and evolution of multiple star systems |
we present a model for the seeding and evolution of magnetic fields in galaxies by supernovae (sn). sn explosions during galaxy assembly provide seed fields, which are subsequently amplified by compression, shear flows and random motions. our model explains the origin of μg magnetic fields within galactic structures. w... | a supernova scenario for magnetic fields and rotation measures in galaxies |
we have performed numerical magnetohydrodynamic (mhd) simulations of two closed active regions (ar). the input magnetic field values were the coronal magnetic field computed as extrapolation coronal from observations of the photospheric magnetic field. the studied active regions, noaa ar12565 and ar12567, were register... | numerical simulations of the evolution of solar active regions: the complex ar12565 and ar12567 |
recent high-cadence transient surveys and rapid follow-up observations have revealed that some massive stars dynamically lose their own mass within decades before supernovae (sne). such a mass-loss forms confined circumstellar medium (csm); a high density material distribution only in small radius (≲ 1015 cm with the m... | millimeter emission from supernovae in the very early phase: implications for dynamical mass loss of massive stars |
we use three-dimensional numerical magnetohydrodynamic simulations to investigate the quasi-equilibrium states of galactic disks regulated by star formation feedback. we incorporate effects from massive-star feedback via time-varying heating rates and supernova (sn) explosions, comparing momentum-only injection with th... | feedback regulated turbulence, magnetic fields, and star formation rates in galactic disks |
thanks to the observational and simulation works, the importance of the nonideal magnetohydrodynamic (mhd) effects, i.e., hall effect, ohmic resistivity, and ambipolar diffusion, have been well established at various stages of cloud evolution. to get a comparison between the hall effect with other effects, we aim to mo... | the importance of hall effect in the self-similar collapse of a filamentary cloud |
magnetic field plays an important role in star formation and galaxy evolution. previous studies discussed about the origin of magnetic field and its effect to the environment. with the recent advancement of supercomputers, adding the magnetic field to a cosmological hydrodynamic simulations only become feasible. in thi... | magneto-hydrodynamic simulations on galaxy modeling |
black holes embody one of the few, simple, solutions to the einstein field equations that describe our modern understanding of gravitation. in isolation they are small, dark, and elusive. however, when a gas cloud or star wanders too close, they light up our universe in a way no other cosmic object can. the processes o... | magnetohydrodynamic simulations of black hole accretion |
periods of solar wind where the interplanetary magnetic field (imf) is pointing northward are traditionally considered not to be geo-effective, or having little interaction with the earth's magnetosphere and ionosphere. we simulate and present an example of extreme northward imf stellar wind impacting an earth-like, cl... | earth-like exoplanet response to extreme northward imf stellar wind |
the explosion energy of supernovae is believed to be a major energy source to drive and maintain turbulent motions in the interstellar gas. the interaction of supernova remnants with the interstellar medium plays a crucial role in shaping the statistics of interstellar turbulence, and has important effects on physical ... | the impact of supernova remnants on interstellar turbulence and star formation |
the magnetohydrodynamics of stars and planetary cores is usually dominated by the overwhelming importance of rotation compared to other forces. under these conditions the fluid motions are characterized by a strong invariance along the rotation axis. in the presence of a background magnetic field, magnetohydrodynamic o... | propagation and reflection of diffusionless torsional waves in a sphere |
dispersionless and dispersed particle injections associated with substorms have been studied for many years based on observations acquired primarily at geosynchronous orbit. a general picture that has emerged is that particles are energized and rapidly transported/organized behind an "injection boundary" that penetrate... | multi-point observations and modeling of particle injections during substorms |
the orbital evolution of cataclysmic variables with periods above the "period gap" (>3 hrs) is governed by angular momentum loss via the magnetized wind of the unevolved secondary star. the usual prescription to study such systems takes into account only the magnetic field of the secondary and assumes its field is d... | realistic mhd modelling of cataclysmic variable spin-down |
created at the base of the convective envelope by a nonlinear dynamo process, the large scale magnetic field of a star evolves with its rotational history. beyond the photosphere, magnetic processes heat the corona above one million kelvin hence driving a magnetized wind responsible for the braking of main sequence sta... | coronal magnetic field and wind of an aging k-type star |
the galactic magnetic fields are considered as one of the key components regulating star formation, but their actual role on the dense cores formation and evolution remains today an open question.dust polarized continuum emission is particularly well suited to probe the dense and cold medium and study the magnetic fiel... | statistical properties of the polarized emission of planck galactic cold clumps |
the combined feedback of supernova explosions and stellar winds from associations of massive stars has a dramatic impact on their environment: large amounts of energy coming from the ejecta create dense shocks around the associations, compressing the surrounding ism and triggering the formation of molecular clouds and ... | formation of cold clumps and filaments around superbubbles |
solar energetic particle (sep) phenomena represent one of the major components of space weather. often, but not exclusively associated with coronal mass ejections (cmes), they pose a significant scientific as well as practical interest. as these particles originate at such explosive events, they have energies up to sev... | field-aligned transport and acceleration of solar energetic particles |
massive infrared dark clouds (irdcs) are believed to be the precursors to star clusters and massive stars (e.g. bergin & tafalla 2007). the supersonic, turbulent nature of molecular clouds in the presence of magnetic fields poses a great challenge in understanding the structure and dynamics of magnetized molecular ... | structure and dynamics of magnetized dark molecular clouds |
understanding the processes related to the formation and evolution of molecular clouds is essential to our understanding of the interstellar medium (ism) at large and of star formation. high galactic latitude clouds are ideal laboratories for studying the physics of the ism as only turbulence, magnetic fields and the i... | aspects of hi behaviour in the birth of molecular clouds |
magnetic fields play a key role in the processes leading to the formation of stars and planets. analytical models and mhd numerical simulations of the evolution of star-forming cores show that the magnetic field is critical for transporting angular momentum during the protostellar phase and sets the conditions for stro... | magnetic fields in herbig ae/be stars |
this work is dedicated to the numerical simulations of the dynamics of toroidal magnetic flux tubes (mfts) in the accretion disk of a young t tauri star. the equations of mft dynamics take into account the buoyancy and drag forces, the magnetic field of the disk, and the tensions of the internal magnetic field of the m... | formation and dynamics of magnetic flux tubes in the accretion disks of young stars |
magnetic helicity, as one of the few conserved quantities in magneto-hydrodynamics, is often invoked as the principle driving the generation and structuring of magnetic fields in a variety of environments, from dynamo models in stars and planets, to post-disruption reconfigurations of tokamak's plasmas. most particular... | magnetic helicity estimations in models and observations of the solar magnetic field |
it is not fully clear how the magnetic field acts during the first stages of star formation. a possible way to clarify its role is to observe the polarized light coming from masers and thermal dust emission. by measuring linear polarization angles and zeeman splitting of different maser species it is possible to study ... | magnetic fields around massive protostars as traced by masers and dust emission |
the physical mechanisms involved in the evolution of young stellar objects (ysos) are a complex subject still under debate. classical t tauri stars (ctts) are solar-like stars that are not only accreting mass from their circumstellar disks, but are also ejecting part of it in different shapes of outflows. at the moment... | unveiling yso dynamics through observations and simulations. |
turbulence, magnetic fields and gravity driven flows are important for the formation of new stars. although magnetic fields have been proven to be important in the formation of stars, only a few works have been done combining magnetic field and kinematic information. such studies are important to analyze both gravity a... | collapse scenarios in magnetized star-forming regions |
magnetars are neutron stars of extreme magnetization, the most magnetized objects known in the universe. they are among the most topical sources in high energy astrophysics, being discovered in 1979 when their emission of intense flares of nonthermal hard x rays was first detected. pulsed modulation of the signal in a ... | modeling hard x-ray bursts and giant flares from magnetars |
interplanetary coronal mass ejections (icmes) originate from the eruption of complex magnetic structures occurring in our stars atmosphere. they propagate in the interplanetary medium, where they can be probed by spacecraft. icmes are known to generate geomagnetic storms that can disturb our technologies on earth, this... | 3d modelling of titov-demoulin modified flux ropes propagation in the solar wind |
when a supermassive black hole (smbh) feeds on its host galaxy, it launches energetic mechanical outflows and emits radiation. such active galactic nuclei (agn) can launch relativistic jets that blow away and heat up the ambient gas via a process known as agn feedback. this feedback is key to understanding galaxy evolu... | from inside out: bridging the bondi and event horizon scales using 3d grmhd simulations |
the dynamical evolution of short-period low-mass binary stars (m < 1.5 msun, p < 10 days) is strongly influenced by tidal dissipation. despite its fundamental role in binary evolution, constraining the strength of tidal dissipation, typically parameterized by the tidal quality factor q, has remained discrepant by... | prospects of constraining tidal dissipation in low-mass binary stars |
star formation has important implications for the formation of planetary systems and the evolution of galaxies, but due to the complex interplay of gravity, turbulence, magnetic fields, as well as feedback from newly formed stars, star formation is still poorly understood. the evolution of the gas density probability d... | effect of initial conditions on the gas density distribution in a simulated star-forming cloud with stellar feedback |
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