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at 60 pc, tw hydra (tw hya) is the closest example of a star with a gas-rich protoplanetary disk, though tw hya may be relatively old (3-15 myr). as such, tw hya is especially appealing for testing our understanding of the interplay between stellar and disk evolution. we present a high-resolution near-infrared spectrum... | characterizing tw hydra |
the presence of superconducting and superfluid components in the core of mature neutron stars calls for the rethinking of a number of key magnetohydrodynamical notions like resistivity, the induction equation, magnetic energy and flux-freezing. using a multifluid magnetohydrodynamics formalism, we investigate how the m... | magnetic field evolution in superconducting neutron stars |
radio emission from magnetars provides a unique probe of the relativistic, magnetized plasma within the near-field environment of these ultra-magnetic neutron stars. the transmitted waves can undergo birefringent and dispersive propagation effects that result in frequency-dependent conversions of linear to circularly p... | linear to circular conversion in the polarized radio emission of a magnetar |
as a star spins-down during the main sequence, its wind properties are affected. in this work, we investigate how earth's magnetosphere has responded to the change in the solar wind. earth's magnetosphere is simulated using 3d magnetohydrodynamic models that incorporate the evolving local properties of the solar wind. ... | the evolution of earth's magnetosphere during the solar main sequence |
sun-like and low-mass stars possess high-temperature coronae and lose mass in the form of stellar winds, which are driven by thermal pressure and complex magnetohydrodynamic processes. these magnetized outflows probably do not significantly affect the star’s structural evolution on the main sequence, but they brake the... | magnetic braking of sun-like and low-mass stars: dependence on coronal temperature |
small-scale magnetic flux ropes in the solar wind have been studied for decades via both simulation and observation. statistical analysis utilizing various in situ spacecraft measurements is the main observational approach, which helps investigate the generation and evolution of these small-scale structures. in this st... | analysis of small-scale magnetic flux ropes covering the whole ulysses mission |
the quark matter symmetry free energy and the thermodynamical properties of strange quark matter (sqm) in strong magnetic fields and non-zero temperature cases are discussed in this work within nambu-jona-lasinio (njl) model by considering two kinds of vector interactions. the properties of the proto-quark stars (pqss)... | quark matter at finite temperature under strong magnetic fields within nambu-jona-lasinio model |
the pulsar wind model is updated by considering the effect of particle density and pulsar death. it can describe both the short-term and long-term rotational evolution of pulsars consistently. it is applied to model the rotational evolution of the crab pulsar. the pulsar is spun down by a combination of magnetic dipole... | rotational evolution of the crab pulsar in the wind braking model |
we study the simultaneous effects of the symmetry energy and temperature on the crust-core transition of a magnetar. the dynamical and the thermodynamical spinodals are used to calculate the transition region within a relativistic mean-field approach for the equation of state. quantizing magnetic fields with intensitie... | crust-core transition of a neutron star: effects of the symmetry energy and temperature under strong magnetic fields |
cool stars with outer convective envelopes are observed to have magnetic fields with a variety of geometries, which on large scales are dominated by a combination of the lowest-order fields such as the dipole, quadrupole, and octupole modes. magnetized stellar wind outflows are primarily responsible for the loss of ang... | the effect of combined magnetic geometries on thermally driven winds. i. interaction of dipolar and quadrupolar fields |
we study the coupling of the force-free magnetosphere to the long-term internal evolution of a magnetar. we allow the relation between the poloidal and toroidal stream functions - that characterizes the magnetosphere - to evolve freely without constraining its particular form. we find that, on time-scales of the order ... | crust-magnetosphere coupling during magnetar evolution and implications for the surface temperature |
the magnetic interaction between a classical t tauri star and its surrounding accretion disk is thought to influence its rotational evolution. we use 2.5d magnetohydrodynamic, axisymmetric simulations of star-disk interaction, computed via the pluto code, to calculate the net torque acting on these stars. we divide the... | magnetic braking of accreting t tauri stars ii: torque formulation spanning spin-up and spin-down regimes |
tidal interaction between an exoplanet and its host star is a possible pathway to transfer angular momentum between the planetary orbit and the stellar spin. in cases where the planetary orbital period is shorter than the stellar rotation period, this may lead to angular momentum being transferred into the star's rotat... | tidal star-planet interaction and its observed impact on stellar activity in planet-hosting wide binary systems |
magnetohydrodynamic (mhd) kink waves are ubiquitously observed in the solar atmosphere. the propagation and damping of these waves may play relevant roles in the transport and dissipation of energy in the solar atmospheric medium. however, in the atmospheric plasma dissipation of transverse mhd wave energy by viscosity... | magnetohydrodynamic kink waves in nonuniform solar flux tubes: phase mixing and energy cascade to small scales |
turbulent mixing in the radiative regions of stars is usually either ignored or crudely accounted for in most stellar evolution models. however, there is growing evidence that such mixing is present and can affect various aspects of a star's life. here, we present a first attempt at quantifying mixing by horizontal she... | horizontal shear instabilities at low prandtl number |
the magnetorotational instability (mri) is key to physics in accretion disks and is widely considered to play some role in massive star core collapse. models of rotating massive stars naturally develop very strong shear at composition boundaries, a necessary condition for mri instability, and the mri is subject to trip... | the role of the magnetorotational instability in massive stars |
as another step towards understanding the long-term evolution of the magnetic field in neutron stars, we provide the first simulations of ambipolar diffusion in a spherical star. restricting ourselves to axial symmetry, we consider a charged-particle fluid of protons and electrons carrying the magnetic flux through a m... | magnetic field evolution and equilibrium configurations in neutron star cores: the effect of ambipolar diffusion |
understanding how young stars gain their masses through disk-to-star accretion is of paramount importance in astrophysics. it affects our knowledge about the early stellar evolution, the disk lifetime and dissipation processes, the way the planets form on the smallest scales, or the connection to macroscopic parameters... | on the mass accretion rates of herbig ae/be stars. magnetospheric accretion or boundary layer? |
hd189733 is an active k dwarf that is, with its transiting hot jupiter, among the most studied exoplanetary systems. in this first paper of the multiwavelength observations of an evaporating exoplanet and its star (moves) programme, we present a 2-yr monitoring of the large-scale magnetic field of hd189733. the magneti... | moves - i. the evolving magnetic field of the planet-hosting star hd189733 |
the rate at which the solar wind extracts angular momentum (am) from the sun has been predicted by theoretical models for many decades, and yet we lack a conclusive measurement from in situ observations. in this letter we present a new estimate of the time-varying am flux in the equatorial solar wind, as observed by th... | direct detection of solar angular momentum loss with the wind spacecraft |
we consider the case of radio flares from black hole x-ray binaries in which the flare spectrum evolves from optically thick to optically thin, under the assumption that this is due to decreasing optical depth to synchrotron self-absorption. we are able to place upper and lower limits on the size of the emitting region... | synchrotron self-absorption and the minimum energy of optically thick radio flares from stellar mass black holes |
black widows are millisecond pulsars with low-mass companions, a few per cent the mass of the sun, on orbits of several hours. these companions are presumably the remnants of main-sequence stars that lost their mass through a combination of roche lobe overflow and ablation by the host pulsar's high-energy radiation. wh... | black widow formation by pulsar irradiation and sustained magnetic braking |
off-centred dipole configurations have been suggested to explain different phenomena in neutron stars, such as natal kicks, irregularities in polarization of radio pulsars and properties of x-ray emission from millisecond pulsars. here, for the first time, we model magnetothermal evolution of neutron stars with crust-c... | three-dimensional magnetothermal evolution of off-centred dipole magnetic field configurations in neutron stars |
aims: a large number of calcium infrared triplet (irt) spectra are expected from the gaia and carmenes missions. conversion of these spectra into known activity indicators will allow analysis of their temporal evolution to a better degree. we set out to find such a conversion formula and to determine its robustness.met... | the ca ii infrared triplet's performance as an activity indicator compared to ca ii h and k. empirical relations to convert ca ii infrared triplet measurements to common activity indices |
we present the results of the neutron star x-ray binary system cen x-3 performed by insight-hxmt with two observations during 2017 and 2018. during these two observations, the source reached a x-ray luminosity of ~1038 erg s-1 from 2-105 kev. the analysis of the broadband x-ray spectrum reports the presence of two cycl... | discovery of two cyclotron resonance scattering features in x-ray pulsar cen x-3 by insight-hxmt |
we report on the presence of numerous tiny bright dots in and around an emerging flux region (an x-ray/coronal bright point) observed with solo's eui/hrieuv in 174 å. these dots are roundish and have a diameter of 675 ± 300 km, a lifetime of 50 ± 35 s, and an intensity enhancement of 30% ± 10% above their immediate sur... | solo/eui observations of ubiquitous fine-scale bright dots in an emerging flux region: comparison with a bifrost mhd simulation |
we show that the performances of a stern-gerlach apparatus can be improved by using a magnetic field profile for the atomic spin evolution designed with the shortcut-to-adiabaticity technique. interestingly, it can be made more compact, for atomic beams propagating at a given velocity, and more resilient to a dispersio... | shortcut to adiabaticity in a stern-gerlach apparatus |
we present the initial results of the large impact of magnetic fields on the evolution of hot stars (life) project. the focus of this project is the search for magnetic fields in evolved oba giants and supergiants with visual magnitudes between 4 and 8, with the aim to investigate how the magnetic fields observed in up... | first results from the life project: discovery of two magnetic hot evolved stars |
the role of slow-mode magnetohydrodynamic (mhd) shocks in magnetic reconnection is of great importance for energy conversion and transport, but in many astrophysical plasmas the plasma is not fully ionised. in this paper, we use numerical simulations to investigate the role of collisional coupling between a proton-elec... | the formation and evolution of reconnection-driven, slow-mode shocks in a partially ionised plasma |
we present submillimeter array 880 μm dust polarization observations of six massive dense cores in the dr21 filament. the dust polarization shows complex magnetic field structures in the massive dense cores with sizes of 0.1 pc, in contrast to the ordered magnetic fields of the parsec-scale filament. the major axes of ... | magnetic fields in the massive dense cores of the dr21 filament: weakly magnetized cores in a strongly magnetized filament |
context. forming massive stars launch outflows of magnetic origin, which in fact serve as a marker for finding sites of massive star formation. however, both the theoretical and observational study of the mechanisms that intervene in the formation and propagation of such magnetically driven outflows has been possible o... | modeling disks and magnetic outflows around a forming massive star. ii. dynamics of jets from massive protostars |
ɛ lupi a is a binary system consisting of two main-sequence early b-type stars aa and ab in a short period, moderately eccentric orbit. the close binary pair is the only doubly magnetic massive binary currently known. using photometric data from the brite constellation we identify a modest heartbeat variation. combinin... | ɛ lupi: measuring the heartbeat of a doubly magnetic massive binary with brite constellation |
energetic outflows from main sequence stars accreting mass at very high rates might account for the powering of some eruptive objects, such as merging main sequence stars, major eruptions of luminous blue variables, e.g., the great eruption of eta carinae, and other intermediate luminosity optical transients (ilots; re... | binary interactions with high accretion rates onto main sequence stars |
accretion on to a highly magnetized neutron star runs through a magnetospheric flow, where the plasma follows the magnetic field lines in the force-free regime. the flow entering the magnetosphere is accelerated by the gravity of the star and then abruptly decelerated in a shock located above the surface of the star. f... | simulating the shock dynamics of a neutron star accretion column |
we investigate the effect of non-ideal magnetohydrodynamics (mhd) on the formation of binary stars using a suite of three-dimensional smoothed particle magnetohydrodynamics simulations of the gravitational collapse of 1 m⊙, rotating, perturbed molecular-cloud cores. alongside the role of ohmic resistivity, ambipolar di... | the impact of non-ideal magnetohydrodynamics on binary star formation |
both observations and numerical simulations suggest that alfvénic waves may carry sufficient energy to sustain the hot temperatures of the solar atmospheric plasma. however, the thermalization of wave energy is inefficient unless very short spatial scales are considered. phase mixing is a mechanism that can take energy... | transition to turbulence in nonuniform coronal loops driven by torsional alfvén waves |
tidal disruption events (tdes) occur when a star gets torn apart by the strong tidal forces of a supermassive black hole, which results in the formation of a debris stream that partly falls back towards the compact object. this gas moves along inclined orbital planes that intersect near pericentre, resulting in a so-ca... | the nozzle shock in tidal disruption events |
we perform the first 3d fully coupled magneto-thermal simulations of neutron stars (including the most realistic background structure and microphysical ingredients so far) applied to a very complex initial magnetic field topology in the crust, similar to what was recently obtained by proto-neutron stars dynamo simulati... | 3d evolution of neutron star magnetic fields from a realistic core-collapse turbulent topology |
strong magnetic fields play an important role in powering the emission of neutron stars. nevertheless, a full understanding of the interior configuration of the field remains elusive. in this work, we present general relativistic magnetohydrodynamics (mhd) simulations of the magnetic field evolution in neutron stars la... | long-term general relativistic magnetohydrodynamics simulations of magnetic field in isolated neutron stars |
context. understanding the collapse of dense molecular cloud cores to stellar densities and the subsequent evolution of the protostar is of importance to model the feedback effects such an object has on its surrounding environment, as well as describing the conditions with which it enters the stellar evolutionary track... | the birth and early evolution of a low-mass protostar |
solar-type stars, which shed angular momentum via magnetized stellar winds, enter the main sequence with a wide range of rotational periods prot. this initially wide range of rotational periods contracts and has mostly vanished by a stellar age $t\sim {0.6}\, {\rm gyr}$, after which solar-type stars spin according to t... | the winds of young solar-type stars in the pleiades, ab doradus, columba, and β pictoris |
we present the implementation of general-relativistic resistive magnetohydrodynamics solvers and three divergence-free handling approaches adopted in the general-relativistic multigrid numerical (gmunu) code. in particular, implicit-explicit runge-kutta schemes are used to deal with the stiff terms in the evolution equ... | an extension of gmunu: general-relativistic resistive magnetohydrodynamics based on staggered-meshed constrained transport with elliptic cleaning |
context. for moderate and slow rotation, the magnetic activity of solar-like stars is observed to strongly depend on rotation, while for rapid rotation, only a very weak or no dependency is detected. these observations do not yet have a solid explanation in terms of dynamo theory.aims: we aim to find such an explanatio... | rotational dependence of turbulent transport coefficients in global convective dynamo simulations of solar-like stars |
we study the general-relativistic dynamics of matter being accreted on to and ejected by a magnetized and non-rotating neutron star. the dynamics is followed in the framework of fully general relativistic magnetohydrodynamics (grmhd) within the ideal-mhd limit and in two spatial dimensions. more specifically, making us... | grmhd simulations of accreting neutron stars i: non-rotating dipoles |
context. magnetic fields influence the formation and evolution of stars and impact the observed stellar properties. magnetic a-type stars (ap stars) are a prime example of this. access to precise and accurate determinations of their stellar fundamental properties, such as masses and ages, is crucial to understand the o... | fundamental properties of a selected sample of ap stars: inferences from interferometric and asteroseismic constraints |
as followup to our recent detection of a pre-transit signal around hd 189733 b, we obtained full pre-transit phase coverage of a single planetary transit. the pre-transit signal is again detected in the balmer lines but with variable strength and timing, suggesting that the bow shock geometry reported in our previous w... | variation in the pre-transit balmer line signal around the hot jupiter hd 189733b |
we have studied numerically the evolution of magnetic fields in barotropic neutron stars, by performing non-linear magnetohydrodynamical simulations with the code pluto. for both initially predominantly poloidal and toroidal fields, with varying strengths, we find that the field settles down to a mixed poloidal-toroida... | magnetic field configurations in neutron stars from mhd simulations |
we present the results obtained from the analysis of high-mass x-ray binary pulsar 4u 1909+07 using nustar and astrosat observations in july 2015 and 2017, respectively. x-ray pulsations at ≈604 s are clearly detected in our study. based on the long-term spin-frequency evolution, the source is found to spun-up in the l... | revisiting the spectral and timing properties of 4u 1909+07 with nustar and astrosat |
in a previous paper, we reported simulations of the evolution of the magnetic field in neutron star (ns) cores through ambipolar diffusion, taking the neutrons as a motionless uniform background. however, in real nss, neutrons are free to move, and a strong composition gradient leads to stable stratification (stability... | two-fluid simulations of the magnetic field evolution in neutron star cores in the weak-coupling regime |
the theory of the formation of the first stars in the universe, the so-called population iii (pop iii), has until now largely neglected the impact of magnetic fields. complementing a series of recent studies of the magnetohydrodynamic (mhd) aspects of pop iii star formation, we here carry out a suite of idealized numer... | impact of magnetic fields on population iii star formation |
fast radio bursts (frbs) are mysterious radio transients with millisecond durations. recently, ~16 days of periodic activity and ~159 days of possible periodicity were detected to arise from frb 180916.j0158+65 and frb 121102, respectively, and the spin period of a slow-rotation magnetar was further considered to be on... | do the periodic activities of repeating fast radio bursts represent the spins of neutron stars? |
recent numerical simulations have demonstrated that transverse coronal loop oscillations are susceptible to the kelvin-helmholtz (kh) instability due to the counterstreaming motions at the loop boundary. we present the first analytical model of this phenomenon. the region at the loop boundary where the shearing motions... | an analytical model of the kelvin-helmholtz instability of transverse coronal loop oscillations |
magnetic fields and mass accretion processes create dark and bright spots on the surface of young stars. these spots manifest as surface thermal inhomogeneities, which alter the global temperature measured on the stars. to understand the effects and implications of these starspots, we conducted a large ishell high-reso... | the effects of starspots on spectroscopic mass estimates of low-mass young stars |
we present an observational study of the plasma dynamics at the base of a solar coronal jet, using high resolution extreme ultraviolet imaging data taken by the extreme ultraviolet imager on board solar orbiter, and by the atmospheric imaging assembly on board solar dynamics observatory. we observed multiple plasma eje... | a highly dynamic small-scale jet in a polar coronal hole |
stellar magnetism plays an important role in stellar evolution theory. approximatively 10 per cent of observed main sequence (ms) and pre-main-sequence (pms) radiative stars exhibit surface magnetic fields above the detection limit, raising the question of their origin. these stars host outer radiative envelopes, which... | magnetic fields driven by tidal mixing in radiative stars |
context. the sub-millimetre polarisation of dust emission from star-forming clouds carries information on grain properties and on the effects that magnetic fields have on cloud evolution.aims: using observations of a dense filamentary cloud g035.39-00.33, we aim to characterise the dust emission properties and the vari... | dust spectrum and polarisation at 850 μm in the massive irdc g035.39-00.33 |
magnetic fields (b-fields) play a key role in the formation and evolution of protoplanetary disks, but their properties are poorly understood due to the lack of observational constraints. using canaricam at the 10.4 m gran telescopio canarias, we have mapped out the mid-infrared polarization of the protoplanetary disk ... | an ordered magnetic field in the protoplanetary disk of ab aur revealed by mid-infrared polarimetry |
we report on magnetic field measurements of 157 chemically peculiar a/b stars (ap/bp) based on resolved, magnetically split absorption lines present in h-band spectra provided by the sloan digital sky survey (sdss)/apache point observatory galactic evolution experiment (apogee) survey. these stars represent the extreme... | discovery of resolved magnetically split lines in sdss/apogee spectra of 157 ap/bp stars |
in the standard scenario for spin evolution of isolated neutron stars, a young pulsar slows down with a surface magnetic field b that does not change. thus the pulsar follows a constant b trajectory in the phase space of spin period and spin period time derivative. such an evolution predicts a braking index n = 3 while... | magnetic field growth in young glitching pulsars with a braking index |
the model for the generation of magnetic fields in a neutron star, based on the magnetic field instability caused by the electroweak interaction between electrons and nucleons, is developed. using the methods of the quantum field theory, the helicity flip rate of electrons in their scattering off protons in dense matte... | relaxation of the chiral imbalance and the generation of magnetic fields in magnetars |
it has recently been established that the evolution of protoplanetary disks is primarily driven by magnetized disk winds, requiring a large-scale magnetic flux threading the disks. the size of such disks is expected to shrink with time, as opposed to the conventional scenario of viscous expansion. we present the first ... | global non-ideal magnetohydrodynamic simulations of protoplanetary disks with outer truncation |
context. relativistic jets are ubiquitous in the universe. in microquasars, especially in high-mass x-ray binaries, the interaction of jets with the strong winds driven by the massive and hot companion star in the vicinity of the compact object is fundamental for understanding the jet dynamics, nonthermal emission, and... | 3d rmhd simulations of jet-wind interactions in high-mass x-ray binaries |
recent observations of the low-mass (0.1-0.6 {m}⊙ ) rotation distributions of the pleiades and praesepe clusters have revealed a ubiquitous correlation between mass and rotation, such that late m dwarfs rotate an order-of-magnitude faster than early m dwarfs. in this paper, we demonstrate that this mass-rotation correl... | m dwarf rotation from the k2 young clusters to the field. i. a mass-rotation correlation at 10 myr |
context. the importance of magnetic fields at the onset of star formation related to the early fragmentation and collapse processes is largely unexplored today.aims: we want to understand the magnetic field properties at the earliest evolutionary stages of high-mass star formation.methods: the atacama large millimeter ... | magnetic fields at the onset of high-mass star formation |
one of the most important problems in the context of cataclysmic variables (cvs) is the lack of observations of systems with periods between 2 and 3.12 hr, known as the period gap. the orbital evolution of cvs with periods shorter than those in the gap is dominated by gravitational radiation, while for periods exceedin... | the magnetic nature of the cataclysmic variable period gap |
large-scale morphology and time evolution are investigated for the unified model of bipolar outflows outlined in shang et al. (2006), where an outflow forms by a radially directed, wide-angle magnetized wind interacting with magnetized isothermal toroids in various quasistatic states. the primary wide-angle wind is tor... | a unified model for bipolar outflows from young stars: the interplay of magnetized wide-angle winds and isothermal toroids |
we study the long-term evolution of the centroid energy of cyclotron lines - often referered to as cyclotron resonance scattering features (crsfs) - in her x-1, vela x-1, and cen x-3, using survey observations of the burst alert telescope onboard swift. we find a significant decrease of the fundamental crsf energy in h... | long-term evolutions of the cyclotron line energies in her x-1, vela x-1, and cen x-3 as observed with swift/bat |
this article briefly reviews our current understanding of the evolution of magnetic fields in neutron stars, which basically defines the evolutionary pathways between different observational classes of neutron stars. the emphasis here is on the evolution in binary systems and the newly emergent classes of millisecond p... | magnetic fields of neutron stars |
results are presented of a first study of collisionless magnetic reconnection starting from a recently found exact nonlinear force-free vlasov-maxwell equilibrium. the initial state has a harris sheet magnetic field profile in one direction and a non-uniform guide field in a second direction, resulting in a spatially c... | particle-in-cell simulations of collisionless magnetic reconnection with a non-uniform guide field |
we explore the thermal and magnetic field structure of a late-stage proto-neutron star (proto-ns). we find the dominant contribution to the entropy in different regions of the star, from which we build a simplified equation of state (eos) for the hot neutron star (ns). with this, we numerically solve the stellar equili... | magnetic fields in late-stage proto-neutron stars |
instabilities in a neutron star can generate alfvén waves in its magnetosphere. propagation along the curved magnetic field lines strongly shears the wave, boosting its electric current j a. we derive an analytic expression for the evolution of the wavevector k and the growth of j a. in the strongly sheared regime, j a... | relativistic alfvén waves entering charge-starvation in the magnetospheres of neutron stars |
accreting x-ray pulsars undergo luminous x-ray outbursts during which the luminosity-dependent spectral and timing features of the neutron star's emission can be analyzed in detail, thus shedding light on the accretion regime at work. we took advantage of a monitoring campaign that was performed with nustar, swift/xrt,... | accreting on the edge: a luminosity-dependent cyclotron line in the be/x-ray binary 2s 1553-542 accompanied by accretion regimes transition |
we present radio spectra spanning 0.1-10 ghz for the sample of heavily obscured luminous quasars with extremely red mid-infrared-optical colors and compact radio emission. the spectra are constructed from targeted 10 ghz observations and archival radio survey data that together yield 6-11 flux-density measurements for ... | radio spectra of luminous, heavily obscured wise-nvss selected quasars |
we report on our investigation of the evolution of a system of spark discharges in the inner acceleration region (iar) above the pulsar polar cap. the surface of the polar cap is heated to temperatures of around 106 k and forms a partially screened gap (psg), due to thermionic emission of positively charged ions from t... | two-dimensional configuration and temporal evolution of spark discharges in pulsars |
we made near-infrared polarimetric observations toward serpens south. this region contains three dense filaments that are roughly parallel to one another. using the histogram of relative orientations, the three filaments are found to be roughly perpendicular to the global magnetic field. the morphology of the plane-of-... | magnetic field structure in serpens south |
galactic winds are a crucial player in galaxy formation and evolution, but observations of them have proven extraordinarily difficult to interpret, leaving large uncertainties even in basic quantities such as mass outflow rates. here we present an analysis of the wind of the nearby dwarf starburst galaxy m82 using a se... | the observable properties of cool winds from galaxies, agn, and star clusters - ii. 3d models for the multiphase wind of m82 |
it has been suggested that a non-repeating fast radio burst (frb) represents the final signal of a magnetized neutron star collapsing to a black hole. in this model, a supramassive neutron star supported by rapid rotation, will collapse to a black hole several thousand to million years after its birth, as a result of s... | electromagnetic emission from blitzars and its impact on non-repeating fast radio bursts |
black hole x-ray binaries undergo occasional outbursts caused by changing inner accretion flows. here we report high angular resolution radio observations of the 2013 outburst of the black hole candidate x-ray binary system xte j1908+094, using data from the very long baseline array and european vlbi network. we show t... | resolved, expanding jets in the galactic black hole candidate xte j1908+094 |
magnetically arrested disks (mads) appear when accretion flows are supplied with a sufficient amount of magnetic flux. in this work, we use results of magnetohydrodynamic simulations to set the configuration of the magnetic field and investigate the dynamics and radiative properties of the resulting accretion flow (i.e... | radiative properties of magnetically arrested disks |
we present a statistical analysis for the characteristics and radial evolution of linear magnetic holes (lmhs) in the solar wind from 0.166 to 0.82 au using parker solar probe observations of the first two orbits. it is found that the lmhs mainly have a duration less than 25 s and the depth is in the range from 0.25 to... | characteristics of magnetic holes in the solar wind revealed by parker solar probe |
treatment of the vortex motion in the superfluids of the inner crust and the outer core of neutron stars is a key ingredient in modelling a number of pulsar phenomena, including glitches and magnetic field evolution. after recalculating the microscopic vortex velocity in the inner crust, we evaluate the velocity for th... | microscopic vortex velocity in the inner crust and outer core of neutron stars |
we report on quasi-simultaneous observations from radio to x-ray frequencies of the neutron star x-ray binary aql x-1 over accretion state transitions during its 2016 outburst. all the observations show radio to millimetre spectra consistent with emission from a jet, with a spectral break from optically thick to optica... | the evolving jet spectrum of the neutron star x-ray binary aql x-1 in transitional states during its 2016 outburst |
pulsars are famous for their rotational stability. most of them steadily spin-down and display a highly repetitive pulse shape. but some pulsars experience timing irregularities such as nulling, intermittency, mode changing and timing noise. as changes in the pulse shape are often correlated with timing irregularities,... | evolution of non-spherical pulsars with plasma-filled magnetospheres |
neutron stars radiate in a broad-band spectrum from radio wavelengths up to very high energies. they have been sorted into several classes depending on their respective place in the p-\dot{p} diagram and depending on spectral/temporal properties. fundamental physical parameters such as their characteristic age and magn... | the illusion of neutron star magnetic field estimates |
we study breaking stress of deformed coulomb crystals in a neutron star crust, taking into account electron plasma screening of ion-ion interaction; calculated breaking stress is fitted as a function of electron screening parameter. we apply the results for analysing torsional oscillation modes in the crust of a non-ma... | deformed crystals and torsional oscillations of neutron star crust |
intermittency and anisotropy are two important aspects of plasma turbulence, which the solar wind provides a natural laboratory to investigate. however, their forms and nature are still under debate, making it difficult to achieve a consensus in the theoretical interpretation. here, we perform higher-order statistics f... | on the scaling and anisotropy of two subranges in the inertial range of solar wind turbulence |
context. the question of the origin and evolution of magnetic fields in stars possessing a radiative envelope, like the a-type stars, is still regarded as a challenge for stellar physics. those zones are likely to be differentially rotating, which suggests that strong interactions between differential rotation and magn... | three-dimensional evolution of magnetic fields in a differentially rotating stellar radiative zone |
magnetic activity is known to be correlated to the rotation period for moderately active main-sequence solar-like stars. in turn, the stellar rotation period evolves as a result of magnetized stellar winds that carry away angular momentum. understanding the interplay between magnetic activity and stellar rotation is th... | the open flux evolution of a solar-mass star on the main sequence |
subvirial gravitational collapse is one mechanism by which star clusters may form. here we investigate whether this mechanism can be inferred from observations of young clusters. to address this question, we have computed smoothed particle hydrodynamics simulations of the initial formation and evolution of a dynamicall... | signatures of star cluster formation by cold collapse |
while it has been suggested that there is a connection between the magnetic properties and the internal structure of young stars, there have not been enough magnetic measurements to firmly establish such a correlation at the earliest ages. here, we contribute to this endeavor by presenting stellar parameters and magnet... | measuring the magnetic field of young stars using ishell observations: bp tau and v347 aur |
context. the role of magnetic fields during the formation of high-mass stars is not yet fully understood, and the processes related to the early fragmentation and collapse are as yet largely unexplored. the high-mass star forming region g9.62+0.19 is a well known source, presenting several cores at different evolutiona... | alma reveals the magnetic field evolution in the high-mass star forming complex g9.62+0.19 |
this report presents a three-dimensional (3d) numerical magnetohydrodynamics (mhd) model of the white-light coronagraph observational phenomena known as coronal inflows and in/out pairs. coronal inflows in the large angle and spectrometric coronagraph/c2 field of view (approximately $2\mbox{--}6\,{r}_{\odot }$ ) were t... | a model for coronal inflows and in/out pairs |
gro j1008-57, as a be/x-ray transient pulsar, is considered to have the highest magnetic field in known neutron star x-ray binary systems. observational data of the x-ray outbursts in gro j1008-57 from 2017 to 2020 were collected by the insight-hxmt satellite. in this work, the spin period of the neutron star in gro j1... | accretion torque reversals in gro j1008-57 revealed by insight-hxmt |
failed supernovae (fsn) are a possible channel for the formation of heavy stellar-mass black holes (m bh > ~30 m ⊙). however, the effects of metallicity, rotation, and magnetic field on the islands of explodabilty of massive stars are not clear. here, we simulate the stellar structure and evolution in the mass range... | the effects of rotation, metallicity, and magnetic field on the islands of failed supernovae |
a novel scheme has been developed to show that the observed phase behavior associated with subpulse drifting from two pulsars, j1034-3224 and j1720-2933, can be used to obtain the magnetic field configuration in the partially screened gap (psg). the outflowing plasma along the open magnetic field line region of pulsars... | estimating the evolution of sparks in the partially screened gap of pulsars from subpulse drifting |
context. close-by planets can excite various kinds of oscillations in their host stars through their time-varying tidal potential.aims: magnetostrophic oscillations with a frequency much smaller than the stellar rotation frequency have recently been proposed to account for the spin-orbit commensurability observed in se... | tidal excitation of auto-resonant oscillations in stars with close-by planets |
in this paper, we present the detailed analysis of recurrent homologous jets originating from an emerging negative magnetic flux at the edge of an active region. the observed jets show multithermal features. their evolution shows high consistence with the characteristic parameters of the emerging flux, suggesting that ... | on the magnetic and energy characteristics of recurrent homologous jets from an emerging flux |
we analyze the evolutionary status of recently discovered long-period radio sources psr j0901-4046, gleam-x j1627-52, and gpm j1839-10. we discuss the hypothesis that all three sources are radio pulsars. in the framework of standard scenarios, it is often accepted that the pulsar mechanism is switched off when an exter... | evolutionary status of long-period radio pulsars |
we show that magnetar models for ultraluminous x-ray sources (ulxs) have serious internal inconsistencies. the magnetic fields required to increase the limiting luminosity for radiation pressure above the observed (assumed isotropic) luminosities are completely incompatible with the spin-up rates observed for pulsing u... | ultraluminous x-ray sources are beamed |
we revisit the various approximations employed to study the long-term evolution of the magnetic field in neutron star cores and discuss their limitations and possible improvements. a recent controversy on the correct form of the induction equation and the relevant evolution time-scale in superconducting neutron star co... | on the magnetic field evolution time-scale in superconducting neutron star cores |
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