Minimum Magnetic Field Strength Research Articles

Imaging a Large Coronal Loop Using Type U Solar Radio Burst Interferometry

Solar radio U-bursts are generated by electron beams traveling along closed magnetic loops in the solar corona. Low-frequency (<100 MHz) U-bursts serve as powerful diagnostic tools for studying large-sized coronal loops that extend into the middle corona. However, the positive frequency drift component (descending leg) of U-bursts has received less attention in previous studies, as the descending radio flux is weak. In this study, we utilized LOFAR interferometric solar imaging data from a U-burst that has a significant descending leg component, observed between 10 and 90 MHz on 2020 June 5th. By analyzing the radio source centroid positions, we determined the beam velocities and physical parameters of a large coronal magnetic loop that reached just about 1.3 R ⊙ in altitude. At this altitude, we found the plasma temperature to be around 1.1 MK, the plasma pressure around 0.20 mdyn, cm−2, and the minimum magnetic field strength around 0.07 G. The similarity in physical properties determined from the image suggests a symmetric loop. The average electron beam velocity on the ascending leg was found to be 0.21c, while it was 0.14c on the descending leg. This apparent deceleration is attributed to a decrease in the range of electron energies that resonate with Langmuir waves, likely due to the positive background plasma density gradient along the downward loop leg.

Evolutionary implications of a magnetar interpretation for GLEAM-X J162759.5–523504.3

ABSTRACT The radio pulsar GLEAM-X J162759.5–523504.3 has an extremely long spin period ($P = 1091.17\, \mbox{s}$), and yet seemingly continues to spin-down rapidly ($\dot{P} &amp;lt; 1.2 \times 10^{-9}\, \mbox{ss}^{-1}$). The magnetic field strength that is implied, if the source is a neutron star undergoing magnetic dipole braking, could exceed $10^{16}\, \mbox{G}$. This object may therefore be the most magnetized neutron star observed to date. In this paper, a critical analysis of a magnetar interpretation for the source is provided. (i) A minimum polar magnetic field strength of $B \sim 5 \times 10^{15}\, \mbox{G}$ appears to be necessary for the star to activate as a radio pulsar, based on conventional ‘death valley’ assumptions. (ii) Back-extrapolation from magnetic braking and Hall–plastic–Ohm decay suggests that a large angularize momentum reservoir was available at birth to support intense field amplification. (iii) The observational absence of X-rays constrains the star’s field strength and age, as the competition between heating from field decay and Urca cooling implies a surface luminosity as a function of time. If the object is an isolated, young ($\sim 10\, \mbox{kyr}$) magnetar with a present-day field strength of $B \gtrsim 10^{16}\, \mbox{G}$, the upper limit ($\approx 10^{30}\, \mbox{erg s}^{-1}$) set on its thermal luminosity suggests it is cooling via a direct Urca mechanism.

Deriving Large Coronal Magnetic Loop Parameters Using LOFAR J Burst Observations

Large coronal loops around one solar radius in altitude are an important connection between the solar wind and the low solar corona. However, their plasma properties are ill-defined, as standard X-ray and UV techniques are not suited to these low-density environments. Diagnostics from type J solar radio bursts at frequencies above 10 MHz are ideally suited to understand these coronal loops. Despite this, J-bursts are less frequently studied than their type III cousins, in part because the curvature of the coronal loop makes them unsuited for using standard coronal density models. We used LOw-Frequency-ARray (LOFAR) and Parker Solar Probe (PSP) solar radio dynamic spectrum to identify 27 type III bursts and 27 J-bursts during a solar radio noise storm observed on 10 April 2019. We found that their exciter velocities were similar, implying a common acceleration region that injects electrons along open and closed magnetic structures. We describe a novel technique to estimate the density model in coronal loops from J-burst dynamic spectra, finding typical loop apex altitudes around 1.3 solar radius. At this altitude, the average scale heights were 0.36 solar radius, the average temperature was around 1 MK, the average pressure was 0.7~text{mdyn},text{cm}^{-2}, and the average minimum magnetic field strength was 0.13 G. We discuss how these parameters compare with much smaller coronal loops.

A 1.05-A/m Minimum Magnetic Field Strength Single-Chip, Fully Integrated Biometric Smart Card SoC Achieving 792.5-ms Transaction Time With Anti-Spoofing Fingerprint Authentication

A single-chip, fully integrated biometric authentication smart card system-on-a-chip (SoC) has been developed that integrates an analog front-end for fingerprint sensors (FPSs), a high-speed processor dedicated to fingerprint information processing, and a dual-interface smart card system with a secure element. The chip is mounted on a cost-effective single package with a capacitive FPS and a few external capacitors. The implemented biometric smart card system shows a total processing time of 792.5 ms including anti-spoofing fingerprint authentication at a magnetic field strength of 1.05 A/m.

X-ray flares of the young planet host Ds Tucanae A

The discovery of planets around young stars has spurred novel studies of the early phases of planetary formation and evolution. Stars are strong emitters at X-ray and UV wavelengths in their first billion of years and this strongly affects the evaporation, thermodynamics, and chemistry in the atmospheres of the young planets orbiting around them. In order to investigate these effects in young exoplanets, we observed the 40 Myr old star DS Tuc A with XMM-Newton. We recorded two X-ray bright flares, with the second event occurring about 12 ks after the first one. Their duration, from the rise to the end of the decay, was about 8 − 10 ks in soft X-rays (0.3–10 keV). The flares were also recorded in the 200–300 nm band with the UVM2 filter of the Optical Monitor. The duration of the flares in UV was about 3 ks. The observed delay between the peak in the UV band and in X-rays is a probe of the heating phase, followed by evaporation and an increase in the density and emission of the flaring loop. The coronal plasma temperature at the two flare peaks reached 54–55 MK. Diagnostics based on the temperatures and timescales of the flares applied to these two events have allowed us to infer a loop length of 5 − 7 × 1010 cm, which is about the extent of the stellar radius. We also inferred the values of electron density at the flare peaks of 2.3 − 6.5 × 1011 cm−3, along with a minimum magnetic field strength on the order of 300–500 G that is needed to confine the plasma. The energy released during the flares was on the order of 5 − 8 × 1034 erg in the bands 0.3 − 10 keV and 0.9 − 2.7 × 1033 erg in the UV band (200–300 nm). We speculate that the flares were associated with coronal mass ejections (CMEs) that hit the planet about 3.3 h after the flares, which dramatically increased the rate of evaporation for the planet. From the RGS spectra, we retrieved the emission measure distribution and the abundances of coronal metals during the quiescent and flaring states, respectively. Finally, we inferred a high electron density measurement, which is in agreement with the inferences drawn from time-resolved spectroscopy and EPIC spectra, as well as the analysis of RGS spectra during the flares.

Экспериментальные исследования электромагнитных полей на электрическом подвижном составе

Objective: To identify the influence of electromagnetic interference of various origins on the func- tioning of electronic components of control systems in electric rolling stock (ERS) and radio commu- nication devices, and the effect of electromagnetic fields (EMF) on humans. To carry out experi- mental studies of the ERS EMF characteristics taken as source data, allowing to assess the need to take appropriate actions to ensure electromagnetic safety. One of such measures is the optimal ar- rangement of electric equipment in the driver’s cabin of an electric locomotive or electric train, which will make it possible to achieve the minimum electric and magnetic field strength values under specified conditions. Methods: Direct measurement of the electromagnetic field characteristics in the driver’s cabin of a new 2ES-5 (2ЭС-5) AC electric locomotive (joint production of Transmashhol- ding JSC, Russia, and Alstom, France), as well as on a 2ES4K (2ЭС4К) DC electric locomotive (driver’s cabin, high-voltage chamber, electric locomotive roof) and an ED4M (ЭД4М) DC electric train (dri- ver’s cabin, train car). In the driver’s cabin, measurements were carried out near the working appa- ratus, near the driver’s and assistant's seats and at frequencies for which the maximum permissible levels have been set. Results: The magnetic field strengths (as having the greatest effect on the func- tioning of the electronic components of the ERS control systems and on the person) in the driver’s cabin of electric locomotives and electric trains were measured at different currents under the fol- lowing conditions: starting, traction, braking in the high-voltage chamber and on the electric locomo- tive roof. Practical importance: The given electromagnetic field characteristics do not exceed the specifications set forth in the regulatory documents of the Russian Federation. However, when trains move, there are bursts of EMF strength values due to transient processes in the power supply sys- tem: on DC ERS, the magnetic field strength in the driver’s cabin reached 100 A/m, the electric field strength — 8,5 kV/m, magnetic induction on the DC electric locomotive roof — 400 μT. These values exceed the maximum permissible levels and require the relevant actions to ensure electromagnetic safety.

Soft Ferrofluid Actuator Based on 3D-Printed Scaffold Removal.

Fabricating soft functional materials via additive manufacturing is an emerging field with a wide variety of applications due to their ability to respond to specifically engineered stimuli (e.g., mechanical, electrical, magnetic, chemical). This article describes an approach to engineering magnetically sensitive structures using three-dimensional printing of acrylonitrile butadiene styrene scaffolds. These scaffolds are encapsulated in polydimethylsiloxane (PDMS) and removed using organic solvents. The open channels that remain after removal are filled in with a ferrofluid to render the structure magnetically sensitive. A three-point flexural test shows that introducing a channel in this way only reduces the flexural modulus of the PDMS by a factor ∼8%. We perform magnetic deflection experiments on samples with three different channel diameters. Our results show a linear dependence between applied magnetic field strength and deflection. We also find that there is a minimum magnetic field strength that needs to be applied to achieve deflection. These results suggest that there is a minimum yield stress, beyond which deflection will occur. We perform experiments on a more complex channel geometry to find that there are multiple modes of deflection. A rational approach to channel design may enable us to tune the mechanical response and direct these actuators to undergo complex motion.

EvryFlare. II. Rotation Periods of the Cool Flare Stars in TESS across Half the Southern Sky

Abstract We measure rotation periods and sinusoidal amplitudes in Evryscope light curves for 122 two-minute K5–M4 TESS targets selected for strong flaring. The Evryscope array of telescopes has observed all bright nearby stars in the south, producing 2-minute cadence light curves since 2016. Long-term, high-cadence observations of rotating flare stars probe the complex relationship between stellar rotation, starspots, and superflares. We detect periods from 0.3487 to 104 days and observe amplitudes from 0.008 to 0.216 g′ mag. We find that the Evryscope amplitudes are larger than those in TESS with the effect correlated to stellar mass (p-value = 0.01). We compute the Rossby number (R o ) and find that our sample selected for flaring has twice as many intermediate rotators (0.04 &lt; R o &lt; 0.4) as fast (R o &lt; 0.04) or slow (R o &gt; 0.44) rotators; this may be astrophysical or a result of period detection sensitivity. We discover 30 fast, 59 intermediate, and 33 slow rotators. We measure a median starspot coverage of 13% of the stellar hemisphere and constrain the minimum magnetic field strength consistent with our flare energies and spot coverage to be 500 G, with later-type stars exhibiting lower values than earlier-type stars. We observe a possible change in superflare rates at intermediate periods. However, we do not conclusively confirm the increased activity of intermediate rotators seen in previous studies. We split all rotators at R o ∼ 0.2 into bins of P Rot &lt; 10 days and P Rot &gt; 10 days to confirm that short-period rotators exhibit higher superflare rates, larger flare energies, and higher starspot coverage than do long-period rotators, at p-values of 3.2 × 10−5, 1.0 × 10−5, and 0.01, respectively.

Trajectory Simulation of Magnetic Particles in Dry Belt Type Magnetic Separation

Magnetic separation, which has been widely used in various industries (e.g., mineral and waste treatment) is an important part of mineral processing. In this study, the simulations of particle trajectories and the relationships between the main parameters in a dry belt-type magnetic separation system are presented. The magnetic field strength simulated by finite element analysis depended upon the vertical distance; the maximum strength was formed at a 0.31 m along the x-axis from a permanent magnet. Simulations of particle trajectories were conducted on ferromagnetic (magnetite), paramagnetic (ilmenite), and diamagnetic (quartz) materials, with variable parameters such as magnetic field strength, particle size, and degree of liberation. The simulation results showed that the key factors of magnetic susceptibility and field strength considerably affected the particle trajectory, as compared with particle size and specific gravity. Hence, the minimum magnetic field strength needed to separate magnetite and ilmenite could be obtained by the regression equation.문초록

Detection and Timing of Gamma-Ray Pulsations from the 707 Hz Pulsar J0952−0607

Abstract The Low-Frequency Array radio telescope discovered the 707 Hz binary millisecond pulsar (MSP) J0952−0607 in a targeted radio pulsation search of an unidentified Fermi gamma-ray source. This source shows a weak energy flux of F γ = 2.6 × 10−12 erg cm−2 s−1 in the energy range between 100 MeV and 100 GeV. Here we report the detection of pulsed gamma-ray emission from PSR J0952−0607 in a very sensitive gamma-ray pulsation search. The pulsar’s rotational, binary, and astrometric properties are measured over 7 years of Fermi-Large Area Telescope data. For this we take into account the uncertainty on the shape of the gamma-ray pulse profile. We present an updated radio-timing solution now spanning more than 2 years and show results from optical modeling of the black-widow-type companion based on new multiband photometric data taken with HiPERCAM on the Gran Telescopio Canarias on La Palma and ULTRACAM on the New Technology Telescope at ESO La Silla (based on observations collected at the European Southern Observatory, Chile; programme 0101.D-0925, PI: Clark, C. J.). PSR J0952−0607 is now the fastest-spinning pulsar for which the intrinsic spin-down rate has been reliably constrained ( ). The inferred surface magnetic field strength of is among the 10 lowest of all known pulsars. This discovery is another example of an extremely fast spinning black-widow pulsar hiding within an unidentified Fermi gamma-ray source. In the future such systems might help to pin down the maximum spin frequency and the minimum surface magnetic field strength of MSPs.

Improving the mechanical properties of Fe3O4/carbon nanotube reinforced nanocomposites by a low-magnetic-field induced alignment

Abstract The aim of the paper is to develop a novel nanocomposite with high mechanical properties. The mechanical properties are improved by aligning the Fe3O4/multi-walled carbon nanotubes (MWCNTs) into a highly oriented manner in epoxy resin (EP) via a low magnetic field. Fe3O4 nanoparticles were tethered onto the surface of MWCNTs by a novel water-in-oil (W/O) method without heating at high temperatures or the protection of inert gas. Then, the modified magnetic MWCNTs (m-MWCNTs) were added into EP and aligned in a low magnetic field (100 mT). A method was presented to estimate the minimum magnetic field strength for aligning the m-MWCNTs. Besides, the morphology and microstructures of the fabricated m-MWCNTs and m-MWCNTs/EP highly ordered nanocomposites were characterized. Finally, the mechanical properties measurements were performed. The results of the experiments showed that this method was very efficient in aligning m-MWCNTs embedded in polymer matrix leading to a highly ordered composite for improving mechanical properties.

Highly ordered structured montmorillonite/brominated butyl rubber nanocomposites: Dramatic enhancement of the gas barrier properties by an external magnetic field

This work is to develop a novel nanocomposites with high gas barrier properties. The permeability is reduced by aligning the magnetic nanoplatelets into a highly oriented manner in brominated butyl rubber (BIIR) latex via a low magnetic field. Iron oxide (Fe3O4) nanoparticles were deposited on the surface of montmorillonites (MMTs) modified with γ-aminopropyltriethoxysilane (APTES) and octadecyl trimethyl ammonium bromide (OTAB) to produce m-OMMTs nanocomposites. The morphology and microstructures of the prepared m-OMMTs and m-OMMTs/BIIR highly ordered nanocomposites were characterized by X-ray power diffraction (XRD), Fourier Transform infrared spectroscopy (FTIR), scanning electron microscope (SEM), and transmission electron microscope (TEM). Systematic characterization demonstrated that APTES was chemically bonded onto MMTs and Fe3O4 nanoparticles and further confirmed the bond formation between Fe3O4 and MMTs platelets, which could ensure the adhesion between the Fe3O4 nanoparticles and MMT platelets. The modified magnetic MMT nanoplatelets (m-OMMTs) were added into BIIR latex and aligned in a low magnetic field Tm=80 mT. Besides, a ellipsoidal shell model was presented to estimate the minimum magnetic field strength for aligning m-OMMTs in BIIR latex. Finally, the helium permeability measurements were performed by GDP-C gas permeation apparatus. It can be observed that the new method was proved very useful to align m-OMMTs embedded in polymer matrix leading to a highly ordered composite with excellent gas barrier properties.

Rayleigh–Taylor Instability in Interacting Supernovae: Implications for Synchrotron Magnetic Fields

Abstract Synchrotron emission from a supernova (SN) necessitates a magnetic field, but it is unknown how strong the relevant magnetic fields are, and what mechanism generates them. In this study, we perform high-resolution numerical gas dynamics calculations in axisymmetry to determine the growth of turbulence due to Rayleigh–Taylor (RT) instability, and the resulting kinetic energy in turbulent fluctuations, as a means of inferring how strong magnetic fields can become when amplified by this turbulence. Assuming rough equipartition between kinetic and magnetic energy in the turbulence, we find that RT instability may produce turbulent fluctuations strong enough to amplify magnetic fields to a few percent of equipartition with the thermal energy. This turbulence stays concentrated near the reverse shock, but averaging this magnetic energy throughout the shocked region (weighting by emissivity) sets the magnetic fields at a minimum of 0.3 percent of equipartition. This line of argument predicts a minimum effective magnetic field strength ( ) that should be present in all interacting SNe. This provides a prediction for what should be found in highly resolved, three-dimensional magnetohydrodynamics calculations. The strength and spatial distribution of turbulently generated magnetic fields would have implications for the shape and luminosity of SN radio light curves.

Evaluation of inductive heating energy of ITER toroidal field conductor by calorimetry

The influence of a fast electromagnetic perturbation, such as plasma disruption, on the ITER toroidal field (TF) coil conductor was studied. When a fast magnetic field change is superimposed, the TF conductor is inductively heated by internally generated eddy currents. To measure the inductive heating (IH) energy amount by calorimetry, an IH experiment using short TF conductor samples with length of 20 cm was performed in a liquid He bath. The sample components used were a TF conductor, TF jacket and a TF conductor cable. A 60-turn, single layer solenoid coil was installed around each sample as an IH coil. Also, the Joule heat of the IH coil was solely measured to subtract its thermal contribution from the other samples. A 1 kHz sinusoidal AC current was applied to each IH coil, changing the current amplitude. The heat generated in the samples, including the IH coil, was eventually absorbed into the liquid He, and the liquid He was then vaporized. Thus, the heat amount was measured by a He level sensor inside a gas collection cylinder attached above the sample. The validity of the experimental results was confirmed by comparing them with computation results of the IH energy of the samples with a computation model. Also, the consumed energy was calculated from the measured waveforms of the applied AC voltage and current to the samples. As the result, the measured and calculated IH energy were found to be in good agreement. Finally, based on the results of the experiment, the minimum magnetic field strength, which triggers quench of the TF conductor by fast dumping like plasma disruption, was evaluated using estimated TF conductor minimum quench energy.

Indications of stellar prominence oscillations on fast rotating stars: the cases of HK Aqr and PZ Tel

We present the analysis of six nights of spectroscopic monitoring of two young and fast rotating late-type stars, namely the dMe star HK Aqr and the dG/dK star PZ Tel. On both stars we detect absorption features reminiscent of signatures of co-rotating cool clouds or prominences visible in H$\alpha$. Several prominences on HK Aqr show periodic variability in the prominence tracks which follow a sinusoidal motion (indication of prominence oscillations). On PZ Tel we could not find any periodic variability in the prominence tracks. By fitting sinusoidal functions to the prominence tracks we derive amplitudes and periods which are similar to those of large amplitude oscillations seen in solar prominences. In one specific event we also derive a periodic variation of the prominence track in the H$\beta$ spectral line which shows an anti-phase variation with the one derived for the H$\alpha$ spectral line. Using these parameters and estimated mass density of a prominence on HK Aqr we derive a minimum magnetic field strength of $\sim$2G. The relatively low strength of the magnetic field is explained by the large height of this stellar prominence ($\ge$ 0.67 stellar radii above the surface).

Magnetofluidic concentration and separation of non-magnetic particles using two magnet arrays

The present paper reports the use of diluted ferrofluid and two arrays of permanent magnets for the size-selective concentration of non-magnetic particles. The micro magnetofluidic device consists of a straight channels sandwiched between two arrays of permanent magnets. The permanent magnets create multiple capture zones with minimum magnetic field strength along the channel. The complex interaction between magnetic forces and hydrodynamic force allows the device to operate in different regimes suitable for concentration of non-magnetic particles with small difference in size. Our experimental results show that non-magnetic particles with diameters of 3.1 μm and 4.8 μm can be discriminated and separated with this method. The results from this study could be used as a guide for the design of size-sensitive separation devices for particle and cell based on negative magnetophoresis.

Physical parameters and long-term photometric variability of V1481 Ori, an SB2 member of Orion nebula Cluster with an accreting component

We present the results of our analysis on V1481 Ori (JW 239), a young SB2 in the Orion Nebula Cluster with a circumbinary disc accreting on the lower-mass component. The analysis is based on high-resolution spectroscopic data and high-quality photometric time series about 20-yr long. Thanks to the spectroscopy, we confirm the binary nature of this system consisting of M3 + M4 components and derive the mass ratio M_B/M_A = 0.54, a variable luminosity ratio L_B/L_A = 0.68--0.94, and an orbital period P_orb = 4.433d. The photometric data allowed us to measure the rotation periods of the two components P_phot = 4.4351d and they are found to be synchronized with the orbital period. The simultaneous modeling of V-, I-band, and radial velocity curves in the 2005 season suggests that the variability is dominated by one hot spot on the secondary component covering at least about 3.5% of the stellar surface and about 420K hotter than the unperturbed photosphere. Such a spot may originate from the material of the circumbinary disc accreting onto the secondary component. We also detect an apparent 6-yr periodic variation in the position of this hot spot, which is inferred from the phase migration of the light curve maximum, which we interpret as due to either the presence of surface differential rotation as large as 0.065%, a value compatible with the fully convective components, or to a periodic exchange of angular momentum between the disc and the star, which implies a minimum magnetic field strength of 650G at the stellar surface.

Neutrino viscosity and drag: impact on the magnetorotational instability in protoneutron stars

The magnetorotational instability (MRI) is a promising mechanism to amplify the magnetic field in fast rotating protoneutron stars. The diffusion of neutrinos trapped in the PNS induces a transport of momentum, which can be modelled as a viscosity on length-scales longer than the neutrino mean free path. This neutrino-viscosity can slow down the growth of MRI modes to such an extent that a minimum initial magnetic field strength of $\gtrsim 10^{12}\, {\rm G}$ is needed for the MRI to grow on a sufficiently short time-scale to potentially affect the explosion. It is uncertain whether the magnetic field of fast rotating progenitor cores is strong enough to yield such an initial magnetic field in PNS. At MRI wavelengths shorter than the neutrino mean free path, on the other hand, neutrino radiation does not act as a viscosity but rather induces a drag on the velocity with a damping rate independent of the wavelength. We perform a linear analysis of the MRI in this regime, and apply our analytical results to the PNS structure from a one-dimensional numerical simulation. We show that in the outer layers of the PNS, the MRI can grow from weak magnetic fields at wavelengths shorter than the neutrino mean free path, while deeper in the PNS MRI growth takes place in the viscous regime and requires a minimum magnetic field strength.

Improving the gas barrier properties of Fe3O4/graphite nanoplatelet reinforced nanocomposites by a low magnetic field induced alignment

Abstract The aim of the paper is to develop a novel nanocomposite with high gas barrier property for linerless composite tanks. The permeability is reduced by aligning, the Fe3O4/graphite nanoplatelets (GNPs) into a highly oriented manner in epoxy resin (EP) via a low magnetic field. Fe3O4 nanoparticles were tethered onto the surface of GNPs by the wet-chemical coprecipitation method, and the modified magnetic graphite nanoplatelets (m-GNPs) were added into epoxy resin and aligned in a low magnetic field (40 mT). A method was presented to estimate the minimum magnetic field strength for aligning the m-GNPs. Besides, the morphology and microstructures of the fabricated m-GNPs and m-GNPs/EP highly ordered nanocomposites were characterized. Finally, the helium permeability measurements were performed. The experiments results showed that this method was proved very efficient to align m-GNPs embedded in polymer matrix leading to a highly ordered composite with remarkable gas barrier properties.

ACHANDRAVIEW OF NON-THERMAL EMISSION IN THE NORTHWESTERN REGION OF SUPERNOVA REMNANT RCW 86: PARTICLE ACCELERATION AND MAGNETIC FIELDS

The shocks of supernova remnants (SNRs) are believed to accelerate particles to cosmic ray (CR) energies. The amplification of the magnetic field due to CRs propagating in the shock region is expected to have an impact on both the emission from the accelerated particle population, as well as the acceleration process itself. Using a 95 ks observation with the Advanced CCD Imaging Spectrometer (ACIS) onboard the Chandra X-ray Observatory, we map and characterize the synchrotron emitting material in the northwestern region of RCW 86. We model spectra from several different regions, filamentary and diffuse alike, where emission appears dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across 3 different non-thermal rims in this region. The narrow width (l = 10''-30'') of these filaments constrains the minimum magnetic field strength at the post-shock region to be approximately 80 {\mu}G.