arXiv subjects

M. M. Romanova

Publications and source records attributed to M. M. Romanova.

At least 73 records · Page 4Linked to original sources

arXiv2005

Locking of the Rotation of Disk-Accreting Magnetized Stars

We investigate the rotational equilibrium state of a disk accreting magnetized stars using axisymmetric magnetohydrodynamic (MHD) simulations. In this ``locked'' state, the spin-up torque balances the spin-down torque so that the net average torque on the star is zero. We investigated two types of initial conditions, one with a relatively weak stellar magnetic field and a high coronal density, and the other with a stronger stellar field and a lower coronal density. We observed that for both initial conditions the rotation of the star is locked to the rotation of the disk. In the second case, the radial field lines carry significant angular momentum out of the star. However, this did not appreciably change the condition for locking of the rotation of the star. We find that in the equilibrium state the corotation radius $r_{co}$ is related to the magnetospheric radius $r_A$ as $r_{co}/r_A\approx 1.2-1.3$ for case (1) and $r_{co}/r_A\approx 1.4-1.5$ for case (2). We estimated periods of rotation in the equilibrium state for classical T Tauri stars, dwarf novae and X-ray millisecond pulsars.

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arXiv2005

Screening of the Magnetic Field of Disk Accreting Stars

An analytical model is developed for the screening of the external magnetic field of a rotating, axisymmetric neutron star due to the accretion of plasma from a disk. The decrease of the field occurs due to the electric current in the infalling plasma. The deposition of this current carrying plasma on the star's surface creates an induced magnetic moment with a sign opposite to that of the original magnetic dipole. The field decreases independent of whether the star spins-up or spins-down. The time-scale for an appreciable decrease (factor of $>100$) of the field is found to be $\sim 1.6 \times 10^7$ yr, for a mass accretion rate $\dot{M}=10^{-9} M_\odot/$yr and an initial magnetic moment $μ_i = 10^{30}{\rm G cm}^3$ which corresponds to a surface field of $10^{12} $G if the star's radius is $10^6$ cm. The time-scale varies approximately as $μ_i^{3.8}/\dot{M}^{1.9}$. The decrease of the magnetic field does not have a simple relation to the accreted mass. Once the accretion stops the field leaks out on an Ohmic diffusion time scale which is estimated to be $ > 10^9$ yr.

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arXiv2005

Gamma-ray Flares and VLBI Outbursts of Blazars

A model is developed for the time dependent electromagnetic - radio to gamma-ray - emission of active galactic nuclei, specifically, the blazars, based on the acceleration and creation of leptons at a propagating discontinuity or {\it front} of a Poynting flux jet. The front corresponds to a discrete relativistic jet component as observed with very-long-baseline-interferometry (VLBI). Equations are derived for the number, momentum, and energy of particles in the front taking into account synchrotron, synchrotron-self-Compton (SSC), and inverse-Compton processes as well as photon-photon pair production. The apparent synchrotron, SSC, and inverse-Compton luminosities as functions of time are determined. Predictions of the model are compared with observations in the gamma, optical and radio bands. The delay between the high-energy gamma-ray flare and the onset of the radio is explained by self-absorption and/or free-free absorption by external plasma. Two types of gamma-ray flares are predicted depending on pair creation in the front.

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arXiv2005

Winds, B-Fields, and Magnetotails of Pulsars

We investigate the emission of rotating magnetized neutron stars due to the acceleration and radiation of particles in the relativistic wind and in the magnetotail of the star. We consider that the charged particles are accelerated by driven collisionless reconnection. Outside of the light cylinder, the star's rotation acts to wind up the magnetic field to form a predominantly azimuthal, slowly decreasing with distance, magnetic field of opposite polarity on either side of the equatorial plane normal to the star's rotation axis. The magnetic field annihilates across the equatorial plane with the magnetic energy going to accelerate the charged particles to relativistic energies. For a typical supersonically moving pulsar, the star's wind extends outward to the standoff distance with the interstellar medium. At larger distances, the power output of pulsar's wind $\dot{E}_w$ of electromagnetic field and relativistic particles is {\it redirected and collimated into the magnetotail} of the star. In the magnetotail it is proposed that equipartition is reached between the magnetic energy and the relativistic particle energy. For such conditions, synchrotron radiation from the magnetotails may be a significant fraction of $\dot{E}_w$ for high velocity pulsars. An equation is derived for the radius of the magnetotail $r_m(z^\prime)$ as a function of distance $z^\prime$ from the star. For large distances $z^\prime$, of the order of the distance travelled by the star, we argue that the magnetotail has a `trumpet' shape owing to the slowing down of the magnetotail flow.

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arXiv2005

The analysis of magnetic field measurements of T Tau

It is shown that the existence of hot accretion spots at the surface of T Tau practically has no effect on the accuracy of estimation of its magnetic field strength at photospheric level. We also found that one can interpret results of T Tau's photospheric magnetic field strength measurements carried out via different methods in the frame of the following alternative: 1) if T Tau's inclination angle $i\le 10^\circ,$ then magnetic field of the star may be dipolar with the angle between rotational and magnetic axes is near $85^\circ;$ 2) if it will be found (e.g. from interferometric observations) that $i>10^\circ,$ then magnetic field of T Tau is essentially non-dipolar or/and non-stationary.

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arXiv2004

Relativistic Jets from Accretion Disks

The jets observed to emanate from many compact accreting objects may arise from the twisting of a magnetic field threading a differentially rotating accretion disk which acts to magnetically extract angular momentum and energy from the disk. Two main regimes have been discussed, hydromagnetic jets, which have a significant mass flux and have energy and angular momentum carried by both matter and electromagnetic field and, Poynting jets, where the mass flux is small and energy and angular momentum are carried predominantly by the electromagnetic field. Here, we describe recent theoretical work on the formation of relativistic Poynting jets from magnetized accretion disks. Further, we describe new relativistic, fully-electromagnetic, particle-in-cell simulations of the formation of jets from accretion disks. Analog Z-pinch experiments may help to understand the origin of astrophysical jets.

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arXiv2002

Poynting Jets from Accretion Disks

We give further considerations on the problem of the evolution of a coronal, force-free magnetic field which threads a differentially rotating, conducting Keplerian disk, extending the work of Li {\it et al.} (2001). This situation is described by the force-free Grad-Shafranov (GS) equation for the flux function $Ψ(r,z)$ which labels the poloidal field lines (in cylindrical coordinates). The GS equation involves a function $H(Ψ)$ describing the distribution of poloidal current which is determined by the differential rotation or {\it twist} of the disk which increases linearly with time. We numerically solve the GS equation in a sequence of volumes of increasing size corresponding to the expansion of the outer perfectly conducting boundaries at ($R_{m}, Z_{m}$). The outer boundaries model the influence of an external non-magnetized plasma. The sequence of GS solutions provides a model for the dynamical evolution of the magnetic field in response to (1) the increasing twist of the disk and (2) the pressure of external plasma. We find solutions with {\it magnetically collimated} Poynting jets where there is a {\it continuous} outflow of energy, angular momentum, and toroidal magnetic flux from the disk into the external space.

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arXiv2002

Lepton Acceleration by Relativistic Collisionless Magnetic Reconnection

We have calculated self-consistent equilibria of a collisionless relativistic electron-positron gas in the vicinity of a magnetic $X-$point. For the considered conditions, pertinent to extra-galactic jets, we find that leptons are accelerated up to Lorentz factors $Γ_0 = κe B_0L {\cal E}^2 /mc^2 \gg 1$, where $B_0$ is the typical magnetic field strength, ${\cal E}\equiv E_0/B_0$, with $E_0$ the reconnection electric field, $L$ is the length scale of the magnetic field, and $κ\approx 12$. The acceleration is due to the dominance of the electric field over the magnetic field in a region around the $X-$point. The distribution function of the accelerated leptons is found to be approximately $dn/dγ\propto γ^{-1}$ for $γ\lesssim Γ_0$. The apparent distribution function may be steeper than $γ^{-1}$ due to the distribution of $Γ_0$ values and/or the radiative losses. Self-consistent equilibria are found only for plasma inflow rates to the $X-$point less than a critical value.

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arXiv2002

Three Dimensional MHD Simulations of Accretion to an Inclined Rotator: The "Cubed Sphere" Method

We describe a three-dimensional, Godunov-type numerical magnetohydrodynamics (MHD) method designed for studying disk accretion to a rotating magnetized star in the general case where the star's rotation axis, its magnetic moment, and the normal to the disk all have different directions. The numerical method uses a "cubed sphere" coordinate system which has advantages of Cartesian and spherical coordinate systems but does not have the singular axis ofthe spherical system. The grid is formed by a sequence of concentric spheres of radii $R_j \propto q^j$ with $j=1..N_R$ and $q={\rm const}>1$. The grid on the surface of the sphere consists of six sectors with the grid on each sector topologically equivalent to the equidistant grid on the face of a cube. Simulation results are discussed for the funnel flows (FF) to a star with dipole moment $\rvecmu$ at an angle $Θ=30^\circ$ to the star's rotation axis ${\bf Ω}$ which is aligned with the normal to the disk. Two important new 3D features are found in these simulations: (1) The funnel flow to the stellar surface is mainly in two streams which approach the star from opposite directions. (2) In the $x-z$ cross section of the flow containing $\rvecmu$ and ${\bf Ω}$, the funnel flow often takes the longer of the two possible paths along magnetic field lines to the surface of the star. A subsequent paper will give a detailed description of the method and results on 3D funnel flows at different inclination angles $Θ$.

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arXiv2002

MHD Simulations of Bondi Accretion to a Star in the "Propeller" Regime

This work investigates Bondi accretion to a rotating magnetized star in the "propeller" regime using axisymmetric resistive, magnetohydrodynamic simulations. In this regime accreting matter tends to be expelled from the equatorial region of the magnetosphere where the centrifugal force on matter rotating with the star exceeds the gravitational force. The regime is predicted to occur if the magnetospheric radius larger than the corotation radius and less than the light cylinder radius. The simulations show that accreting matters is expelled from the equatorial region of the magnetosphere and that it moves away from the star in a supersonic, disk-shaped outflow. At larger radial distances the outflow slows down and becomes subsonic. The equatorial matter outflow is initially driven by the centrifugal force, but at larger distances the pressure gradient becomes significant. We find that the star is spun-down mainly by the magnetic torques at its surface with the rate of loss of angular momentum $\dot{L}$ proportional to $-Ω_*^{1.3}μ^{0.8}$, where $Ω_*$ is the star's rotation rate and $μ$ is its magnetic moment. Further, we find that $\dot{L}$ is approximately independent of the magnetic diffusivity of the plasma $η_m$. The fraction of the Bondi accretion rate which accretes to the surface of the star is found to be $\proptoΩ_*^{-1.0}μ^{-1.7}η_m^{0.4}$. Predictions of this work are important for the observability of isolated old neutron stars and for wind fed pulsars in X-ray binaries.

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arXiv2002

MHD Simulations of Disk-Magnetized Star Interactions in Quiescent Regime: Funnel Flows and Angular Momentum Transport

Magnetohydrodynamic (MHD) simulations have been used to study disk accretion to a rotating magnetized star with an aligned dipole moment. Quiescent initial conditions were developed in order to avoid the fast initial evolution seen in earlier studies. A set of simulations was performed for different stellar magnetic moments and rotation rates. Simulations have shown that the disk structure is significantly changed insidea radius r_{br} where magnetic braking is significant. In this region the disk is strongly inhomogeneous. Radial accretion of matter slows as it approaches the area of strong magnetic field and a dense ring and funnel flow form at the magnetospheric radius r_m where the magnetic pressure is equal to the total, kinetic plus thermal, pressure of the matter.

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arXiv2001

Propagation of Magnetized Neutron Stars Through the Interstellar Medium

This work investigates the propagation of magnetized, isolated old neutron stars through the interstellar medium. We performed axisymmetric non relativistic magnetohydrodynamic (MHD) simulations of the propagation of a non-rotating star with dipole magnetic field aligned with its velocity through the interstellar medium (ISM). Effects of rotation will be discussed in a subsequent work. We consider two cases: (1) where theaccretion radius $R_{acc}$ is comparable to the magnetic standoff distance or Alfvén radius $R_A$ and gravitational focusing is important; and (2) where $R_{acc}<< R_A$ and the magnetized star interacts with the ISM as a ``magnetic plow'', without significant gravitational focusing. For the first case simulations were done at a low Mach number ${\cal M}=3$ for a range of values of the magnetic field $B_*$. For the second case, simulations were done for higher Mach numbers, ${\cal M}=10,$ 30, and 50. In both cases, the magnetosphere of the star represents an obstacle for the flow, and a shock wavestands in front of the star. Magnetic field lines are stretched downwind from the star and form a hollow elongated magnetotail. Reconnection of the magnetic field is observed in the tail which may lead to acceleration of particles. Similar powers are estimated to be released in the bow shock wave and in the magnetotail. The estimated powers are, however, below present detection limits. Results of our simulations maybe applied to other strongly magnetized stars, for example, white dwarfs and magnetic Ap stars. Future more sensitive observations may reveal long magnetotails of magnetized stars moving through the ISM.

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arXiv2001

Funnel Flows from Disks to Magnetized Stars

This work considers flows from an accretion disk corotating with the aligned dipole magnetic field of a rotating star. Ideal magnetohydrodynamics (MHD) is assumed with the pressure and density related as $p \propto ρ^γ$ and with $ρ{\bf v}^2 \ll {\bf B}^2/4π$, where ${\bf v}$ is the flow velocity. This limit corresponds to the Alfvén radius for the disk accretion larger than the corotation radius. Transonic flows, which go from subsonic motion near the disk to supersonic inflow near the star, are shown to be possible only for a narrow range of $R_d \sim r_c \equiv (GM/Ω^2)^{1/3}$, where $R_d$ is the radius at which the dipole field line intersects the disk, $r_c$ the corotation radius, $M$ the mass of the star, and $Ω$ its angular rotation rate. The transonic flows have very different behaviors for $γ> 7/5$ and $< 7/5$. In both cases, the plasma flow velocity ${\bf v}$ (which is parallel to ${\bf B}$) increases with decreasing distance $R$ from the star. However, for $γ>7/5$, the Mach number ${\cal M} \equiv |{\bf v}|/c_s$ (with $c_s$ the sound speed) initially increases with $R$ decreasing from $R_d$, but for $R$ decreasing from $\approx 0.22 R_d$ (for $γ=5/3$)the Mach number surprisingly {\it decreases}. In the other limit, $γ< 7/5$, ${\cal M}$ increases monotonically with decreasing $R$. Application of these results is made to funnel flows to rotating magnetized neutron stars and young stellar objects.

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arXiv2001

Poynting Jets from Accretion Disks

The powerful narrow jets observed to emanate from many compact accreting objects may arise from the twisting of a magnetic field threading a differentially rotating accretion disk which acts to magnetically extract angular momentum and energy from the disk. Two main regimes have been discussed, {\it hydromagnetic outflows}, which have a significant mass flux and have energy and angular momentum carried by both the matter and the electromagnetic field and, Poynting outflows, where the mass flux is negligible and energy and angular momentum are carried predominantly by the electromagnetic field. Here we consider a Keplerian disk initially threaded by a dipole-like magnetic field and we present solutions of the force-free Grad-Shafranov equation for the coronal plasma. We find solutions with Poynting jets where there is a continuous outflow of energy and toroidal magnetic flux from the disk into the external space. This behavior contradicts the commonly accepted ``theorem'' of Solar plasma physics that the motion of the footpoints of a magnetic loop structure leads to a stationary magnetic field configuration with zero power and flux outflows. In addition we discuss recent magnetohydrodynamic (MHD) simulations which establish that quasi-stationary collimated Poynting jets similar to our Grad-Shafranov solutions arise from the inner part of a disk threaded by a dipole-like magnetic field. At the same time we find that there is a steady uncollimated hydromagnetic outflow from the outer part of the disk. The Poynting jets represent a likely model for the jets from active galactic nuclei, microquasars, and gamma ray burst sources.

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arXiv1999

Origin of Blazar Activity

Models of Blazars based on the propagation of finite discontinuities or fronts in the Poynting flux jet from the innermost regions of an accretion disk around a black hole are discussed. Such fronts may be responsible for short time-scale (from less than hours to days) flares in different wavebands from high frequency radioband to TeV, with delay in low radio frequencies as a result of synchrotron self-absorption. The cases of magnetic fields of one and opposite polarities across the front are investigated. We find that annihilation of magnetic field in the front leads to higher energy spectrum of leptons and possibility of strong TeV flares. Electron-positron pairs form in most cases as a result of interaction between numerous synchrotron photons and SSC photons, and constitute the majority species, compared with the ions at subparsec scales. Frequent weak outbursts may be responsible for flickering core radiation in all wavebands, while the stronger outbursts may be observed as short time-scale flares.

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arXiv1998

Magneto-centrifugally driven winds: comparison of MHD simulations with theory

Stationary magnetohydrodynamic (MHD) outflows from a rotating, conducting Keplerian accretion disk threaded by B-field are investigated numerically by time-dependent, axisymmetric (2.5D) simulations using a Godunov-type code. A large class of stationary magneto-centrifugally driven winds are found where matter is accelerated from a thermal speed at the disk to much larger velocity, greater than the fast magnetosonic speed and larger than the escape speed. The flows are approximately spherical outflows with only small collimation within the simulation region. Numerical results are shown to coincide with the theoretical predictions of ideal, axisymmetric MHD to high accuracy. Investigation of the influence of outer boundary conditions, particularly that on the toroidal component of magnetic field shows that the commonly used ``free'' boundary condition leads to artificial magnetic forces which can act to give spurious collimation. New boundary conditions are proposed which do not generate artificial forces. Artificial results may also arise for cases where the Mach cones on the outer boundaries are partially directed into the simulation region.

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arXiv1998

Magnetic propeller outflows

A model is developed for magnetic `propeller'-driven outflows which cause a rapidly rotating magnetized star accreting from a disk to spin-down. Energy and angular momentum lost by the star goes into expelling most of the accreting disk matter. The theory gives an expression for the effective Alfven radius $R_A$ (where the inflowing matter is effectively stopped) which depends on the mass accretion rate, the star's mass and magnetic moment, and the star's rotation rate. The model points to a mechanism for `jumps' between spin-down and spin-up evolution and for the reverse transition, which are changes between two possible equilibrium configurations of the system. In for example the transistion from spin-down to spin-up states the Alfven radius $R_A$ decreases from a value larger than the corotation radius to one which is smaller. In this transistion the `propeller' goes from being ``on'' to being ``off.'' The ratio of the spin-down to spin-up torque (or the ratio for the reverse change) in a jump is shown to be of order unity.

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arXiv1998

Spherical Bondi accretion onto a magnetic dipole

Quasi-spherical supersonic (Bondi-type) accretion to a star with a dipole magnetic field is investigated using resistive magnetohydrodynamic simulations. A systematic study is made of accretion to a non-rotating star, while sample results for a rotating star are also presented. A new stationary subsonic accretion flow is found with a steady rate of accretion to the magnetized star smaller than the Bondi accretion rate. Dependences of the accretion rate and the flow pattern on the magnetic momentum of the star and the magnetic diffusivity are presented. For slow star's rotation the accretion flow is similar to that in non-rotating case, but in the case of fast rotation the structure of the subsonic accretion flow is fundamentally different and includes a region of ``propeller'' outflow. The methods and results described here are of general interest and can be applied to systems where matter accretes with low angular momentum.

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