Magnetic Fields in the Milky Way

Haverkorn, M.

doi:10.1007/978-3-662-44625-6_17

Cited by 126 publications

(100 citation statements)

References 98 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…By not correcting for the foreground RM, which is perhaps as high as 1500 rad m −2 , we overestimate | B | by 15%. For PSR J1746-2856 B = 33 µG, and for PSR J1746-2849 B = 16 µG, which are both much higher than the strength of the ordered and turbulent magnetic field in the vicinity of the Sun (1.5-2 µG and 3-6 µG, respectively: e.g., Haverkorn 2015). Strong magnetic fields are not uncommon in the GC: in their analysis of the 'Snake' NTF, Gray et al (1995) derived B ≈ 7 µG for the foreground ISM.…”

Section: Discussionmentioning

confidence: 95%

“…However, the signs of the RMs of PSRs J1746-2856 and J1746-2849 contradict this particular solution. By combining the observed DMs and RMs, and correcting for the foreground contribution to DM, we derive LOS lengths of the magnetic field vector between ∼ 16 − 33 µG, which is much larger than the strength of the large-scale and small-scale magnetic field in the vicinity of the Sun (Haverkorn 2015). If the GC, including the warm ionized medium that is probed by our observations, is pervaded by a strong magnetic field, B ∼ 160 µG (Crocker et al 2011), then our measurements imply that the magnetic field makes an angle 12…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Radio polarimetry of Galactic Centre pulsars

Schnitzeler

Eatough

Ferrière

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

To study the strength and structure of the magnetic field in the Galactic centre (GC) we measured Faraday rotation of the radio emission of pulsars which are seen towards the GC. Three of these pulsars have the largest rotation measures (RMs) observed in any Galactic object with the exception of Sgr A ⋆ . Their large dispersion measures, RMs and the large RM variation between these pulsars and other known objects in the GC implies that the pulsars lie in the GC and are not merely seen in projection towards the GC. The large RMs of these pulsars indicate large line-of-sight magnetic field components between ∼ 16 − 33 µG; combined with recent model predictions for the strength of the magnetic field in the GC this implies that the large-scale magnetic field has a very small inclination angle with respect to the plane of the sky (∼ 12• ). Foreground objects like the Radio Arc or possibly an ablated, ionized halo around the molecular cloud G0.11-0.11 could contribute to the large RMs of two of the pulsars. If these pulsars lie behind the Radio Arc or G0.11-0.11 then this proves that lowscattering corridors with lengths 100 pc must exist in the GC. This also suggests that future, sensitive observations will be able to detect additional pulsars in the GC. Finally, we show that the GC component in our most accurate electron density model oversimplifies structure in the GC.

show abstract

Section: Discussionmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 99%

Radio polarimetry of Galactic Centre pulsars

Schnitzeler

Eatough

Ferrière

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The synchrotron polarization together with Faraday rotation can be used to explore the properties of magnetic field, which is termed the traditional Faraday rotation synthesis (e.g., Burn 1966;Brentjens & de Bruyn 2005;Frick et al 2011;Beck et al 2012). This technique recently applying to polarized observational data provides a significant insight into magnetic field structures of galaxies (e.g., Fletcher et al 2011;Beck & Wielebinski 2013;Haverkorn 2015 for a review) and the properties of the interstellar medium (ISM, e.g., Jelić et al 2015;Van Eck et al 2017;Dickey et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Tracing magnetic field with synchrotron polarization gradients: parameter study

Zhang

Lazarían

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We employ synthetic observations obtained with MHD simulations to study how to trace the distribution of turbulent magnetic fields using the synchrotron polarization gradient techniques suggested by . Both synchrotron polarization gradients and its derivative gradients with regard to the squared wavelength λ 2 are used to explore the probing ability of the technique in magnetic fields from sub-to super-Alfvénic turbulence. We focus on studies that involve multi-frequency measurements in the presence of strong Faraday rotation and show the ways of how to recover the projected mean magnetic fields in the plane of the sky and the local magnetic fields within a tomographic slice. We conclude that the new techniques can successfully reconstruct the 3D magnetic field within our Milky Way and other galaxies. This paper opens an avenue for applying our new techniques to a large number of data cubes such as those from the Low Frequency Array for Radio astronomy and the Square Kilometer Array.

show abstract

“…Magnetic fields in the Milky Way's disk were recently reviewed [97][98][99][100][101]. Basically, there are large radial regions where the magnetic field direction is going clockwise (between 2 and 5 kpc from the Galactic Center; and between 7 and 12 kpc from the Galactic Center), or counterclockwise (between 5 and 7 kpc from the Galactic Center) -see [9].…”

Section: Magnetic Field Map and Relations To The Armsmentioning

confidence: 99%

A guided map to the spiral arms in the galactic disk of the Milky Way

Vallée

2017

Astronomical Review

View full text Add to dashboard Cite

An up-to-date overview of the recent history is given, aiming is to present a helpful working guide to the literature and at the same time introduce key systems and observational results, starting from the Sun and going toward the Galactic Center and parts of the Zona Galactica Incognita, and beyond. We start by presenting an observational view of the Milky Way's disk plane (cartographic, dynamical, chemical crosscut, magnetic). This included the four long spiral arms in the disk of the Milky Way galaxy, their geometry, components, velocity, their widths and internal layers as well as onion-like ordered offsets, the central galactic bars, arm tangents, arm pitch and arm shape, arm origins near the Galactic Center, and other possible players in the spiral arm, such as the magnetic field and the dark matter content. After, we present a basic analysis of some theoretical predictions from galactic arm formation: numerical simulations or analytical theories, and observations are checked against predictions from various numerical simulations and analytical (theoretical) models.

show abstract

Magnetic Fields in the Milky Way

Cited by 126 publications

References 98 publications

Radio polarimetry of Galactic Centre pulsars

Radio polarimetry of Galactic Centre pulsars

Tracing magnetic field with synchrotron polarization gradients: parameter study

A guided map to the spiral arms in the galactic disk of the Milky Way

Contact Info

Product

Resources

About