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we calculate the evolution of cloud cores embedded in different envelopes to investigate environmental effects on the mass accretion rate on to protostars. as the initial state, we neglect the magnetic field and cloud rotation, and adopt star-forming cores composed of two parts: a centrally condensed core and an outer ... | environmental effects of star-forming cores on mass accretion rate |
understanding the role galactic-scale winds play in the formation and evolution of galaxies is a fundamental goal of current astrophysical research. galactic winds, driven by energetic feedback processes associated with supernovae, regulate the baryonic content, star formation rates, and stellar masses of galaxies. to ... | resolving the physics of galactic winds using the gpu-accelerated cholla code |
most massive stars are in binaries. binarity can drastically alter their evolution, which can result in the formation of x-ray binaries or binary black hole systems, the dominant sources of gravitational waves. while single star formation is increasingly well understood, the detailed physics of binary/multiple massive ... | how do (massive) binary stars form? |
the unified model for agn stats that seyfert 1 or 2 types are the same type of object harbouring a luminous accretion disk surrounded by a thick torus, but seen under different viewing angles. this model has been successfully tested for many years by several observers, bringing some evolutions to the initial model, but... | extragalactic observations with adaptive optics: polarisation in active galactic nuclei and study of super stellar clusters |
our closest neighbour star, proxima centauri, has been shown to have at least one orbiting planet, proxima cen b. this planet has a minimum mass close to earth's mass and is likely rocky in its composition. unlike the sun, proxima centauri possesses a very strong magnetic field of at least a few hundred gauss, which ma... | induction heating of the interior of proxima cen b |
young stars such as protostars and pre-main-sequence stars evolve via the interaction with the surrounding accretion disks. it is believed that stellar and disk magnetic fields play important roles in shaping the accretion structure and exchanging the angular momentum between the stars and the disks. however, because o... | 3d mhd simulations of an accreting young star |
we present simulations of the merger of binary neutron star systems calculated with full general relativity and incorporating the global magnetic field structure for the stars evolved with resistive magnetohydrodynamics. we also incorporate the effects of neutrino transport and tabular equations of state to describe th... | merger of magnetized binary neutron stars |
during the late 1990's the mars global surveyor mag/er experiment detected crustal remanent magnetization at mars indicating an ancient internal magnetic dynamo. the location of this remanent magnetization and in particular its absence at the large martian impact craters like hellas suggests a cessation of the dynamo d... | the martian paleo-magnetosphere during the early naochian and its implication for the early martian atmosphere |
in the near future, next-generation telescopes, covering most of the electromagnetic spectrum, will provide a view into the very earliest stages of galaxy formation. to accurately interpret these future observations, accurate and high-resolution simulations of the first stars and galaxies are vital. this proposal is ce... | kinetic modeling of radiative turbulence in relativistic astrophysical plasmas: particle acceleration and high-energy flares |
magnetic fields are speculated to play a significant role in early star formation, in particular, in the collapse dynamics at formation to influence the imf, which may be imprinted in the local metal-poor population. these fields may arise by the amplification of primordial fields during the formation of the first star... | magnetizing the universe during the epoch of reionization |
magnetic fields and self-gravity are likely to play important and interconnected roles in the evolution of protostellar disks around newly formed stars. we propose to use a combination of numerical simulations and analytic models to understand how net magnetic fields evolve during a self-gravitating disk phase, and whe... | magnetic fields and self-gravity in early protostellar disks |
i discuss how hydrodynamical simulations enable exploring nonlinear couplings amongst different physical processes in galaxy formation. i focus on three topics: the effect of baryonic processes on dark matter halos, how stellar feedback leads to 'self-regulated' galaxy formation, and the interplay amongst stellar feedb... | galaxy evolution from hydrodynamical simulations: what have we learned about the physical processes governing galaxy evolution? |
the origin of large-scale magnetic fields in most astrophysical systems like the sun, stars and galaxies remains a challenging open problem. dynamo action in the underlying turbulent fluid is thought to be responsible for the emergence of coherent magnetic fields. due to the enormity of magnetic reynolds numbers in the... | generation of coherent magnetic fields in periodic (closed) and non-periodic (open) domains |
with energies a thousand times greater than an average solar flare, stellar superflares can strip away atmospheres and endanger life on planetary surfaces. these violent outbursts often go hand in hand with coronal mass ejections, shaping the evolution of planets near and far.a bit of solar system historyastronauts on ... | launching a stellar superflare |
in recent omega laser experiments we have created narrowly collimated mg plasma jets by using 20 omega beams from one hemisphere to form a hollow ring pattern on a flat ch target, and characterized the properties of these jets as a function ring radius d and target composition (pure ch vs. 2 percent fe-doped ch). the s... | collision of two magnetized jets created by hollow ring lasers |
molecular clouds, the birthplaces of stars in galaxies throughout the universe, are complicated and dynamic environments. a new series of simulations has explored how these clouds form, grow, and collapse over their lifetimes.this composite image shows part of the taurus molecular cloud. [eso/apex (mpifr/eso/oso)/a. ha... | star-forming clouds feed, churn, and fall |
neutron stars contain the strongest magnetic fields known in the universe. using numerical simulations restricted to axially symmetric geometry, we study the long-term evolution of the magnetic field in the interior of an isolated neutron star under the effect of ambipolar diffusion, i.e. the drift of the magnetic fiel... | magnetic field evolution in neutron stars |
modern theories of structure formation unequivocally predict that density perturbations seeded in the big bang collapse to produce``halos'' of dark matter filled with hot, virialized gas. the physics of this hot halo gas fundamentally determines the mass-scale of galaxies, and likely plays a critical role in their subs... | the origin and survival of cold gas in hot halos |
in this paper, we present the numerical simulation for the steady and unsteady incompressible viscous magnetohydrodynamic (mhd) rotating flow over a rotating sphere near the equator and investigate the effect of the ratio of the angular velocities of the sphere and the fluid, the suction/injection and magnetic field on... | an improvement to the unsteady mhd rotating flow over a rotating sphere near the equator via two radial basis function schemes |
we carried out high resolution simulations of weakly-magnetized core-collapse supernovae in two-dimensional axisymmetry in order to see the influence of the magnetic field and rotation on the explosion. we found that the magnetic field amplified by magnetorotational instability (mri) has a great positive impact on the ... | magnetically assisted explosions of weakly magnetized stars |
the computational advances of the past several decades have allowed theoretical astrophysics to proceed at a dramatic pace. numerical simulations can now simulate the formation of individual molecules all the way up to the evolution of the entire universe. observational astrophysics is producing data at a prodigious ra... | star and planet formation throughout cosmic history |
this thesis presents investigations in four areas of theoretical astrophysics: the production of sterile neutrino dark matter in the early universe, the evolution of small-scale baryon perturbations during the epoch of cosmological recombination, the effect of primordial magnetic fields on the redshifted 21-cm emission... | the astrophysics of strongly interacting systems |
the expansion of hot, dense plasma (100 ev, 1018 cm-3) into vacuum occupied by a strong magnetic field (β =pkinetic /pmag ~ 1) along the expansion axis is a seemingly elementary physics problem, yet it is one that has scarcely been investigated. as well as being a fundamental problem in plasma physics, understanding su... | laboratory study of the shaping and evolution of magnetized episodic plasma jets |
high resolution observations of young stellar object (yso) jets show them to be composed of many small-scale knots or clumps. 2-d and 3-d numerical simulations were conducted with the code astrobear to study how such clumps interact and create morphologies and kinematic patterns seen in emission line observations. two ... | outflows from young stellar objects: bringing numerical simulations closer to observations of herbig-haro objects |
with the recent discovery of gravitational waves from the merger of two black holes, its especially important to understand the electromagnetic signals resulting from mergers of compact objects. new simulations successfully follow a merger of two neutron stars that produces a short burst of energy via a jet consistent ... | jets from merging neutron stars |
the x-ray spectra of central compact objects (ccos) with weak magnetic fields, and quiescent magnetars with strong magnetic fields, are very similar despite the four orders of magnitude difference in their dipole magnetic field strengths. for cco pulsars, the apparently localized surface emission indicated by their lar... | probing the magnetic structure of young neutron stars |
we propose to model magnetized gas as it flows into galaxy disks in milky way-like and redshift 2 environments in order to understand the pc to kpc scale physics that control a crucial link in galaxy evolution: how do galaxies get the gas which sustains star formation over cosmic time? uv observations with the cosmic o... | gaseous infall and star formation from redshift 2 to the milky way |
atmospheric escape is capable of shaping a planet's atmospheric composition and total mass, and thus the planet's long-term habitability. loss to space of atmospheric particles has played a key role in the atmospheric evolution of both mars and venus. intrinsic planetary magnetic fields like the earth's have long been ... | do magnetic fields prevent atmospheric escape? |
with the observation of a kilonova signal following the detection of the binary neutron star merger gw170817, the need for an extended duration simulation of the post-merger environment has become important in order to determine the effects of the stability of the remnant by secular processes on any observed signals. i... | an implementation of axisymmetry in numerical relativity using a multipatch scheme |
the advance in both instrumentation and numerical simulation techniques in the past decade have unfolded the importance of magnetic fields in regulating filamentary clouds formation, evolution, and physical properties of star-forming processes in molecular clouds. in particular, there are emerging interests on the effe... | links between magnetic fields and molecular cloud fragmentation: bimodal mass distribution and density structures. |
we explore the effect of galactic evolution on the rotation of giant molecular clouds (gmcs) in isolated magnetized galaxy simulation. in this model, without prominent structures, we have extracted about 1000 isolated clouds. the properties (mass, size, velocity dispersion) and scaling relations of these clouds consist... | velocity gradients of giant molecular clouds at galactic scales |
the process of star formation is fundamental to understand planet formation and galaxy evolution. almost all stars form in clusters embedded in massive filaments. we present an analysis of the gas kinematics of the integral shaped filament in orion a using different molecular transitions (12co, 13co, nh3, n2h+) to trac... | velocity structure of the orion a integral shaped filament |
the interaction between galaxies and the surrounding gas plays a key role in galaxy formation and evolution. feedback processes driven by star formation and active galactic nuclei facilitate the exchange of mass and energy between the galaxy and the circumgalactic medium through inflowing and outflowing gas. these outf... | evolution, disruption, and composition of galactic outflows around starburst galaxies |
stable magnetic fields have been observed in stars of a wide range of ages, from intermediate-mass stars in the main-sequence up to degenerate stars. what is the equilibrium configuration of the magnetic field inside these stars and which conditions allow it to remain stable over the star's lifetime are still open ques... | stellar magnetic equilibria with the pencil code |
type-i superluminous supernovae (slsne) are an exotic class of core-collapse sn (ccsn) that can be up to 100 times brighter and more slowly-evolving than normal ccsne. slsne represent the end-stages of the most massive stripped stars, and are thought to be powered by the spin-down energy of a millisecond magnetar. stud... | roman ccs white paper: characterizing superluminous supernovae with roman |
we explore the collapsar scenario for long gamma-ray bursts by performing axisymmetric neutrino-radiation magnetohydrodynamics simulations in full general relativity for the first time. in this paper, we pay particular attention to the outflow energy and the evolution of the black-hole spin. we show that for a strong m... | outflow energy and black-hole spin evolution in collapsar scenarios |
we use high-resolution mhd simulations of isolated disk galaxies to investigate the co-evolution of magnetic fields with a self-regulated, star-forming interstellar medium (ism). the simulations are conducted using the ramses amr code on the standard agora initial condition, with gas cooling, star formation and feedbac... | regulating star formation in a magnetized disk galaxy |
the angular momentum of molecular cloud cores plays a key role in the star formation process. however, the evolution of the angular momentum of molecular cloud cores formed in magnetized molecular filaments is still unclear. in this paper, we perform three-dimensional magnetohydrodynamics simulations to reveal the effe... | evolution of the angular momentum of molecular cloud cores in magnetized molecular filaments |
the cosmological 21-cm signal from neutral hydrogen, which is considered as a promising tool, is being used to observe and study the cosmic dawn (cd) and epoch of reionization (eor). a significant part of this thesis focuses on the semi-analytical modeling of the global hi 21-cm signal from cd considering several physi... | unveiling the cosmic dawn and epoch of reionization using cosmic 21-cm signal |
we study the dynamics of stellar wind from one of the bodies in the binary system, where the other body interacts only gravitationally. we focus on following three issues: (i) we explore the origin of observed periodic variations in maser intensity; (ii) we address the nature of bipolar molecular outflows; and (iii) we... | dynamics of stellar wind in a roche potential: implications for (i) outflows & periodicities relevant to astronomical masers, and (ii) generation of baroclinicity |
rotating plasmas are found in astrophysical phenomena such as magnetized neutron stars and pulsar electrospheres, as well as in laboratory experiments such as pure electron/ion plasmas trapped in penning-malmberg (pm) traps and fusion plasmas. in many of these cases, external velocity shear or velocity strain flows aff... | electron plasma vortices under external strain - a study using 2d particle-in-cell simulations |
the injection of energy and momentum into the interstellar medium by young massive stars' intense radiation fields and their fast, radiatively driven winds can have a profound influence on their formation and environment. massive star forming regions are rare and highly obscured, making the early moments of their forma... | the destructive birth of massive stars & massive star clusters |
understanding how the baryonic physics affects the formation and evolution of galax- ies is one of the most critical questions in modern astronomy. significant progress in understanding stellar feedback and modeling them explicitly in simulations have made it possible to reproduce a wide range of observed galaxy proper... | stellar feedback, agn feedback and fluid microphysics in galaxy evolution |
galaxy clusters are harsh environments for their constituent galaxies. a variety of physical processes effective in these dense environments transform gas-rich, spiral, star-forming galaxies to elliptical or spheroidal galaxies with very little gas and therefore minimal star formation. the consequences of these process... | simulating the dynamical evolution of galaxies in group and cluster environments |
during common envelope evolution, an initially weak magnetic field may undergo amplification by interacting with spiral density waves and turbulence generated in the stellar envelope by the inspiralling companion. using 3d magnetohydrodynamical simulations on adaptively refined spherical grids with excised central regi... | post-dynamical inspiral phase of common envelope evolution. the role of magnetic fields |
charged particles are constantly accelerated to non-thermal energies by the reconnecting magnetic field in the solar atmosphere. our understanding of the interactions between the particles and their environment can benefit from three-dimensional atmospheric simulations accounting for non-thermal particle beams. in a pr... | accelerated particle beams in a 3d simulation of the quiet sun. effects of advanced beam propagation modelling |
coronal mass ejections (cmes) are solar eruptions of plasma and magnetic fields that significantly impact space weather, causing disruptions in technological systems and potential damage to power grids when directed towards earth. traditional coronagraphs along the sun-earth line struggle to precisely track the early e... | coronal dimmings as indicators of early cme propagation direction |
in this thesis, the origin of large-scale structures in hot star winds, believed to be responsible for the presence of discrete absorption components (dacs) in the absorption troughs of ultraviolet resonance lines, is constrained using both observations and numerical simulations. these structures are understood as aris... | investigating the potential magnetic origin of wind variability in ob stars |
simulations from the scales of isolated galaxies to clouds have been instrumental in informing us about molecular cloud formation and evolution. simulations are able to investigate the roles of gravity, feedback, turbulence, heating and cooling, and magnetic fields on the physics of the interstellar medium, and star fo... | 2a results: galaxy to cloud scales |
over a hundred millisecond radio pulsars (msps) have been observed in globular clusters (gcs), motivating theoretical studies of the formation and evolution of these sources through stellar evolution coupled to stellar dynamics. here we study msps in gcs using realistic n-body simulations with our cluster monte carlo c... | modeling pulsars in dense star clusters |
recent advanced simulations of protoplanetary disks allow us to search for observational constraints to identify the magnetic field activity in protoplanetary disks. with our 3d radiation non-ideal magneto-hydrodynamical (mhd) models including irradiation from an herbig type star we are able to model the thermal and dy... | how to identify magnetic field activity in young circumstellar disks |
the amplification of magnetic fields via dynamo mechanisms is a fundamental process that not only shapes the dynamics of stars, but also deeply affects the evolution of compact objects from their formation throughout their activity. understanding how magnetic fields are dissipated and amplified in the environment surro... | numerical modeling of dynamos in compact objects: magnetic field amplification and dissipation |
streamers and pseudostreamers structure the corona at the largest scales, as seen in both eclipse and coronagraph white-light images. their inverted-goblet appearance encloses broad coronal loops at the sun and tapers to a narrow radial stalk away from the star. the streamer associated with the global solar dipole magn... | the dynamic formation of pseudostreamers |
my thesis work has focused on understanding the physics of star formation in galaxies and its role in shaping the galaxies and the universe. i have conducted a series of multiscale simulations of star cluster formation in isolated turbulent giant molecular clouds (gmcs) using ramses, a state-of-the-art radiation-magnet... | multiscale radiation-mhd simulations of dense star clusters |
context. the main driving forces supplying energy to the interstellar medium (ism) are supernova explosions and stellar winds. such localized sources are assimilable to curl-free velocity fields as a first approximation. they need to be combined with other physical processes to replicate real galactic environments, suc... | vorticity and magnetic dynamo from subsonic expansion waves |
we investigate the thermal, kinematic, and magnetic structure of small-scale heating events in an emerging flux region (efr). we use high-resolution multiline observations (including ca ii 8542 å, ca ii k, and the fe i 6301 å line pair) of an efr located close to the disk center from the crisp and chromis instruments a... | solar atmospheric heating due to small-scale events in an emerging flux region |
the complete orbital and spin period evolutions of the double neutron star (ns) system psr j0737-3039 are simulated from birth to coalescence, which include the two observed radio pulsars classified as primary ns psr j0737-3039a and companion ns psr j0737-3039b. by employing the characteristic age of psr j0737-3039b to... | simulation of the orbit and spin period evolution of the double pulsars psr j0737-3039 from their birth to coalescence induced by gravitational wave radiation |
magnetic field evolution of neutron star crusts is best described using the formalism of hall magnetohydrodynamics (mhd). for magnetic fields ≥ 1014 g and typical temperatures for most of the lifetime of a magnetar, landau quantization of electrons can significantly alter the crust's thermodynamic and transport propert... | hall mhd in magnetar crusts with landau-quantized electrons |
context. density decreases exponentially with height in the gravitationally stratified solar atmosphere, and therefore collisional coupling between the ionized plasma and the neutrals also decreases. reconnection is a process observed at all heights in the solar atmosphere.aims: here, we investigate the role of collisi... | two-fluid reconnection jets in a gravitationally stratified atmosphere |
we present a three-dimensional, time-dependent mhd simulation of the short-term interaction between a protoplanetary disk and the stellar corona in a t tauri system. the simulation includes the stellar magnetic field, self-consistent coronal heating and stellar wind acceleration, and a disk rotating at sub-keplerian ve... | three-dimensional, time-dependent mhd simulation of disk-magnetosphere-stellar wind interaction in a t tauri, protoplanetary system |
we investigate the dynamic evolution of the gaseous regions around fs cma post-mergers. owing to the slow rotation of the central b-type star, the dynamics is driven mainly by the magnetic field of the central star. recent observations have allowed us to set realistic initial conditions, such as the magnetic field valu... | 2.5d magnetohydrodynamic models of circumstellar discs around fs cma post-mergers - i. non-stationary accretion stage |
we summarize recent attempts to unravel the role of plasma kinetic effects in radiation mediated shocks. such shocks form in all strong stellar explosions and are responsible for the early electromagnetic emission released from these events. a key issue that has been overlooked in all previous works is the nature of th... | anomalous coupling in radiation mediated shocks |
filamentary molecular clouds are regarded as the place where newborn stars form. in particular, a hub region, a place where it appears as if several filaments are colliding, often indicates active star formation. to understand the star formation in filament structures, we investigate the collisions between two filament... | simulation of head-on collisions between filamentary molecular clouds threaded by a lateral magnetic field and subsequent evolution |
the spontaneous evolution of magnetic reconnection in generalized situations (with thermodynamic asymmetry regarding the current sheet and magnetic shear) is investigated using a two-dimensional magnetohydrodynamic simulation. we focus on the asymptotic state of temporal evolution, i.e., the self-similarly expanding ph... | effects of magnetic shear and thermodynamic asymmetry on spontaneous magnetohydrodynamic reconnection |
magnetic fields play a vital role in numerous astrophysical processes such as star formation and the interstellar medium. in particular, their role in the formation and evolution of galaxies is not well understood. this paper presents high-resolution magnetohydrodynamic (mhd) simulations performed with gizmo to investi... | magnetic fields in primordial galaxies |
we study the impact of an upwind scheme on the numerical convergence of simulations of the hall and ohmic effect in neutron stars crusts. while simulations of these effects have explored a variety of geometries and wide ranges of physical parameters, they are limited to relatively low values of the hall parameter, play... | application of an upwind integration method to plane parallel hall-mhd |
the observational properties of isolated nss are shaped by their magnetic field and surface temperature. they evolve in a strongly coupled fashion, and modelling them is key in understanding the emission properties of nss. much effort was put in tackling this problem in the past but only recently a suitable 3d numerica... | modelling magnetar behaviour with 3d magnetothermal simulations |
the sunrise chromospheric infrared spectropolarimeter (scip) has been developed for the third flight of the sunrise balloon-borne stratospheric solar observatory. the aim of the scip is to reveal the evolution of three-dimensional magnetic fields in the solar photosphere and chromosphere using spectropolarimetric measu... | high-speed data processing onboard sunrise chromospheric infrared spectropolarimeter for the sunrise iii balloon telescope |
the solar atmosphere is known to contain many different types of wave-like oscillation. waves and other fluctuations (e.g., turbulent eddies) are believed to be responsible for at least some of the energy transport and dissipation that heats the corona and accelerates the solar wind. thus, it is important to understand... | magnetohydrodynamic mode conversion in the solar corona: insights from fresnel-like models of waves at sharp interfaces |
the tayler-spruit dynamo is one of the most promising mechanisms proposed to explain angular momentum transport during stellar evolution. its development in proto-neutron stars spun-up by supernova fallback has also been put forward as a scenario to explain the formation of very magnetized neutron stars called magnetar... | numerical simulations of the tayler-spruit dynamo in proto-magnetars |
the rotation of sunspots around their umbral center has long been considered as an important process in leading to solar eruptions, but the underlying mechanism remains unclear. a prevailing physical picture on how sunspot rotation leads to eruption is that, by twisting the coronal magnetic field lines from their footp... | magnetic reconnection as the key mechanism in sunspot rotation leading to solar eruption |
context. the rotation periods of young low-mass stars after disks have dissipated (≲-pagination10 myr) but before magnetized winds have removed significant angular momentum is an important launch point for gyrochronology and models of stellar rotational evolution; the rotation of these stars also regulates the magnetic... | the post-disk (or primordial) spin distribution of m dwarf stars |
aims: we used solar observations of a plage-enhanced network with the atacama large millimeter/sub-millimeter array (alma) in band 3 and band 6, together with synthetic continuum maps from numerical simulations with bifrost in the same bands, to carry out a detailed study of bright small-scale magnetic features.methods... | the sun at millimeter wavelengths. iv. magnetohydrodynamic waves in small-scale bright features |
the extragalactic gamma-ray sky is dominated by blazars, active galactic nuclei (agn) with a relativistic jet that is closely aligned with the line of sight. galaxies develop an active nucleus if the central supermassive black hole (bh) accretes large amounts of ambient matter and magnetic flux. the inflowing mass accu... | spectral imprints from electromagnetic cascades in blazar jets |
stars spend most of their lives in rather quiescent phases dominated by slow fluid flow, be it low mach number convection or wave-like motions. yet accurately modeling these phases is of great importance for understanding mixing in stars, the resulting impact on nucleosynthesis, and the rich data coming from asteroseis... | the challenge of simulating slow flows in stellar astrophysics |
how molecular clouds fragment and create the dense structures which go on to eventually form stars is an open question. this thesis numerically investigates various aspects of fragmentation and structure formation in young molecular clouds based on the silcc-zoom and silcc deep-zoom simulations. the silcc-zoom simulati... | morphology, fragmentation, and dynamic balance: an investigation into early stages of structure formation in molecular clouds |
the recent discovery of the moderate differential rotation between the core and the envelope of intermediate-mass (im) main-sequence and evolved stars, and the population of im red giants presenting a surprisingly low-amplitude of their mixed modes (i.e. modes that behave as acoustic modes in their external envelope an... | probing fossil magnetic field effects in the core of evolved low-mass stars using mixed-mode frequencies |
a radio telescope on the far side of the moon can have a revolutionary impact in the field of cosmology. it can measure signals at frequencies below 30 mhz, which represent some of the earliest signals in the cosmological history of the universe, but are blocked from reaching terrestrial radio telescopes by the earth's... | ultra-long wavelength radio astronomy using the lunar crater radio telescope (lcrt) on the farside of the moon |
hex-p is a probe-class mission concept that will combine high spatial resolution x-ray imaging (<10 arcsec fwhm) and broad spectral coverage (0.1-150 kev) with an effective area far superior to current facilities (including xmm-newton and nustar) to enable revolutionary new insights into a variety of important astro... | the high energy x-ray probe (hex-p): broadband x-ray observations of magnetars and other young isolated neutron stars |
we investigate, using a multi-fluid approach, the main properties of standing ion-acoustic modes driven by non-linear standing alfvén waves. the standing character of the alfvénic pump is due to the superposition of two identical circularly polarised counter-propagating waves. we consider parallel propagation along the... | excitation of ion-acoustic waves by non-linear finite-amplitude standing alfvén waves |
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