Multifrequency Radio Studies of G359.1-00.2

Gray, A. D.; Nicholls, Jennifer; Ekers, R. D.; Cram, L. E.

doi:10.1086/175949

Cited by 60 publications

(149 citation statements)

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“…Incidentally, a weaker field is easier to reconcile with the minimum-energy field strength 90 μG derived by Gray et al (1995). Since the Snake lies at a greater projected radius than the other NRFs, a simple way to explain its weaker field is to invoke an overall decrease in the interstellar magnetic field strength outside a radius 100 pc.…”

Section: Radio Continuum Observationsmentioning

confidence: 89%

Interstellar magnetic fields in the Galactic center region

Ferrière¹

2009

A&A

107

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Aims. We seek to obtain a picture of the interstellar magnetic field in the Galactic center region that is as clear and complete as possible. Methods. We review the observational knowledge that has built up over the past 25 years on interstellar magnetic fields within ∼200 pc of the Galactic center. We then critically discuss the various theoretical interpretations and scenarios proposed to explain the existing observations. We also study the possible connections with the general Galactic magnetic field and describe the observational situation in external galaxies. Results. We propose a coherent picture of the magnetic field near the Galactic center, which reconciles some of the seemingly divergent views and which best accounts for the vast body of observations. Our main conclusions are the following. In the diffuse intercloud medium, the large-scale magnetic field is approximately poloidal and its value is generally close to equipartition with cosmic rays (∼10 μG), except in localized filaments where the field strength can reach ∼1 mG. In dense interstellar clouds, the magnetic field is approximately horizontal and its value is typically ∼1 mG.

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Section: Radio Continuum Observationsmentioning

confidence: 89%

Interstellar magnetic fields in the Galactic center region

Ferrière¹

2009

A&A

107

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“…The Pelican (G358.85+0.47) consists of multiple parallel strands which also become more evident near its ends . The Snake shows a bifurcation at its major kink (Gray et al 1995). In some cases the filaments appear to be braided, e.g.…”

Section: Observationsmentioning

confidence: 99%

“…Such a situation is also characteristic of a subject in its infancy. A number of theories for the Galactic filaments were reviewed by Gray et al (1995). Here we concentrate on some of the more recent attempts but also include some of the older models that have survived to the present or which have played a significant role in our attempts to understand these filaments.…”

Section: Theorymentioning

confidence: 99%

“…This model was discussed fully by Gray et al (1995). Rosner & Bodo (1996) proposed that the source of relativistic electrons is the terminal bow shock of the wind from a massive star, or cluster of stars.…”

Section: Star-based Modelsmentioning

confidence: 99%

“…Since the processes of twisting and kinking of the flux tube are related to the magnetic field the relevant dynamical timescale is the Alfvén time, t A = L tube /v a , where L tube is the length of the tube and v A = B/(4π µnm p ) 1/2 is the Alfvén speed. Scaling to the visible length of the Snake, t A ≈ 1.7 × 10 5 (L tube /60 pc)(B/0.4 mG) −1 (n/10 cm −3 ) −1/2 yr. (The fiducial value of n = 10 cm −3 is based upon the estimate of n ∼ 7-14 cm −3 (Gray et al 1995) for the ambient ISM ionised density, derived from rotation measure variations.) 2.…”

Section: Timescalesmentioning

confidence: 99%

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Filaments in the Galactic Centre—with Special Reference to the ‘Snake’

Bicknell

2001

Publ. – Astron. Soc. Aust

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The non-thermal filaments in the Galactic centre constitute one of the great mysteries of this region of the Galaxy. We summarise the observational data on these filaments and critically review the various theories which currently outnumber the observed filaments. We summarise our theory for the longest of these filaments, the Snake, and discuss the relevance of this model for the other filaments in the Galactic centre region. The physics involved in our model for the Snake involves much of the physics that has dominated the career of Professor Don Melrose. In particular, the diffusion of relativistic electrons in the Snake is determined from the theory of resonant scattering by Alfvén waves.

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The Galactic Center Nonthermal Filaments: Recent Observations and Theory

Larosa¹,

Nord²,

Joseph³

et al. 2003

Proceedings of the Galactic Center Workshop 2002

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New high-resolution, wide-field 90 cm VLA 1 observations of the Galactic Center region by Nord et al. have revealed twenty nonthermal filament (NTF) candidates. We report 6 cm polarization observations of six of these. All of the candidates have the expected NTF morphology, and two show extended polarization confirming their identification as NTFs. One of the new NTFs appears to be part of a system of NTFs located in the Sgr B region, 64 pc in projection north of Sgr A. These filaments cross the Galactic plane with an orientation similar to the filaments in the Galactic Center Radio Arc. They extend the scale over which the NTF phenomena is known to occur to almost 300 pc along the Galactic plane. Another NTF was found in the Galactic plane south of the Sgr C filament but with an orientation of 45• to the Galactic plane. This is only the second of 12 confirmed NTFs that is not oriented perpendicular to the Galactic plane. An additional candidate in the Sgr C region was resolved into multiple filamentary structures. Polarization was detected only at the brightness peak of one of the filaments. Several of these filaments run parallel to the Galactic plane and can be considered additional evidence for non-poloidal magnetic fields at the GC. Together the 90 and 6 cm observations indicate that the Galactic center magnetic field may be more complex than a simple globally ordered dipole field.

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Multifrequency Radio Studies of G359.1-00.2

Cited by 60 publications

References 0 publications

Interstellar magnetic fields in the Galactic center region

Interstellar magnetic fields in the Galactic center region

Filaments in the Galactic Centre—with Special Reference to the ‘Snake’

The Galactic Center Nonthermal Filaments: Recent Observations and Theory

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