Faraday rotation effects for diagnosing magnetism in bubble environments

Ignace, Richard

doi:10.5194/ap-1-1-2014

Cited by 3 publications

(2 citation statements)

References 17 publications

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“…Our 1420 MHz polarization images reveal Faraday-rotation structures in the region(s) surrounding GD 561, with the most prominent structures appearing downstream. Faraday rotation is expected in the Strömgren zone around an isolated white dwarf (see Ignace 2014). Also, since a white dwarf is expected to leave behind an ionized trail (see McCullough & Benjamin 2001), it may be reasonable to find downstream Faraday rotation as well.…”

Section: A Strömgren-zone Interpretation For Sh 2-174mentioning

confidence: 98%

THE EMISSION NEBULA Sh 2-174: A RADIO INVESTIGATION OF THE SURROUNDING REGION

Ransom

Kothes²,

Geisbuesch³

et al. 2015

ApJ

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Sh 2-174 is believed to be either a planetary nebula (PN) or ionized, ambient interstellar medium (ISM). We present in this paper 1420 MHz polarization, 1420 MHz total intensity (Stokes-I), and neutral hydrogen (H I) images of the region around Sh 2-174. The radio images address not only the nature of the object, but also the history of the relationship between Sh 2-174 and its surrounding environment. The H I images show that Sh 2-174 sits presently at the center of a ∼1.2 • × ∼0.4 • cloud (with peak hydrogen density n H = 4 ± 2 cm −3 ). The Stokes-I image shows thermal-emission peaks (with electron densities n e = 11 ± 3 cm −3 ) coincident with the R-band optical nebula, as well as low-surface-brightness emission from an ionized "halo" around Sh 2-174 and from an ionized "plateau" extending southeast from the cloud. The polarization images reveal Faradayrotation structures along the projected trajectory of Sh 2-174, including a highcontrast structure with "arms" that run precisely along the eastern edge of the H I cloud and a wide central region which merges with the downstream edge of Sh 2-174. The high-contrast structure is consistent with an ionized tail which has both early-epoch (before Sh 2-174 entered the cloud) and present-epoch (after Sh 2-174 entered the cloud) components. Furthermore, our rotation-measure analysis indicates that the ISM magnetic field is deflected at the leading edge of Sh 2-174. The downstream tail and upstream field deflection point to a PN-ISM interaction. Our estimated space velocity for the host white dwarf (GD 561) demonstrates that Sh 2-174 entered the cloud ∼27,000 yr ago, and gives a PN-ISM interaction timescale 2.0 × 10 5 yr. We estimate an ambient magnetic field in the cloud of 11 ± 3 µG.

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Section: A Strömgren-zone Interpretation For Sh 2-174mentioning

confidence: 98%

THE EMISSION NEBULA Sh 2-174: A RADIO INVESTIGATION OF THE SURROUNDING REGION

Ransom

Kothes²,

Geisbuesch³

et al. 2015

ApJ

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“…On one hand, novel methods have been proposed to diagnose the magnetic field, such as the laser-driven ion-beam trace probe in magnetic confinement fusion [1] and ultrafast proton radiography at laser facilities [2]; on the other hand, traditional methods remain a major role in magnetic field diagnostic and their applications are greatly expanded. This expansion includes not only novel techniques to fabricate key components of traditional diagnostics, such as CMOS Hall effect sensor [3] and magnetic coils based on electron assisted chemical vapor deposition [4], but also the usage of traditional methods under extreme conditions, such as Zeeman effect measurements in upper solar atmosphere [5] and on tokamaks [6], the motional Stark effect measurement on tokamaks [7], the Faraday effect in interstellar magnetic field diagnosis [8], and Stokes shift measurements in chromospheric jets [9]. Among these traditional methods, the magnetic coil is the most frequently used, known as the B-dot probe on laser facilities [10].…”

Section: Introductionmentioning

confidence: 99%

Fabrication and absolute calibration of B-dot probe for magnetic field measurement on a high power laser facility

Kuang¹,

Xue²,

Jing³

et al. 2020

Plasma Sci. Technol.

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The fabrication and absolute calibration of a B-dot probe is employed to measure the pulsed magnetic field at the Shenguang-II high power laser facility. Copper enameled silk with a cross section diameter of 0.1 mm is used to wind the one-turn coil with a 1 mm diameter. Two coils are paired and reversely linked to their respective circuits to form a differential B-dot probe that is sealed in and protected by a quartz shell. This B-dot probe is experimentally calibrated and then used to measure the pulsed magnetic field in laser targeting experiments at the Shenguang-II high power laser facility. Signals show a high performance of this B-dot probe. The common mode noise can be effectively canceled out by the differential pair. The magnetic field of over 300 T can be extrapolated at the location close to the target.

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Interacting large-scale magnetic fields and ionized gas in the W50/SS433 system

Farnes

Gaensler

Purcell

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The W50/SS433 system is an unusual Galactic outflow-driven object of debatable origin. We have used the Australia Telescope Compact Array (ATCA) to observe a new 198 pointing mosaic, covering 3 • × 2 • , and present the highest-sensitivity full-Stokes data of W50 to date using wide-field, wide-band imaging over a 2 GHz bandwidth centred at 2.1 GHz. We also present a complementary Hα mosaic created using the Isaac Newton Telescope Photometric Hα Survey of the Northern Galactic Plane (IPHAS). The magnetic structure of W50 is found to be consistent with the prevailing hypothesis that the nebula is a reanimated shell-like supernova remnant (SNR), that has been re-energised by the jets from SS433. We observe strong depolarization effects that correlate with diffuse Hα emission, likely due to spatiallyvarying Faraday rotation measure (RM) fluctuations of ≥ 48 to 61 rad m −2 on scales ≤ 4.5 to 6 pc. We also report the discovery of numerous, faint, Hα filaments that are unambiguously associated with the central region of W50. These thin filaments are suggestive of a SNR's shock emission, and almost all have a radio counterpart. Furthermore, an RM-gradient is detected across the central region of W50, which we interpret as a loop magnetic field with a symmetry axis offset by ≈90 • to the east-west jet-alignment axis, and implying that the evolutionary processes of both the jets and the SNR must be coupled. A separate RM-gradient is associated with the termination shock in the Eastern ear, which we interpret as a ring-like field located where the shock of the jet interacts with the circumstellar medium. Future optical observations will be able to use the new Hα filaments to probe the kinematics of the shell of W50, potentially allowing for a definitive experiment on W50's formation history.

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Faraday rotation effects for diagnosing magnetism in bubble environments

Cited by 3 publications

References 17 publications

THE EMISSION NEBULA Sh 2-174: A RADIO INVESTIGATION OF THE SURROUNDING REGION

THE EMISSION NEBULA Sh 2-174: A RADIO INVESTIGATION OF THE SURROUNDING REGION

Fabrication and absolute calibration of B-dot probe for magnetic field measurement on a high power laser facility

Interacting large-scale magnetic fields and ionized gas in the W50/SS433 system

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