The kinematics of the Honeycomb nebula in the vicinity of SN 1987A

Meaburn, J.; Wang, L.; Palmer, J. W.; López, J. A.

doi:10.1093/mnras/263.1.l6

Cited by 7 publications

(6 citation statements)

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“…Hα and [N ii ] 6548 and 6584 Å (Meaburn et al 1993) and [S ii ] 6717 and 6731 Å (Redman et al 1999) line profiles were obtained using the Manchester Echelle Spectrometer (MES; Meaburn et al 1984) on the Anglo‐Australian Telescope along the same (within the 1‐arcsec wide seeing disc) slit position (Fig. 2a).…”

Section: Observationsmentioning

confidence: 99%

“…However, it seemed worthwhile to investigate if optical line brightness ratios of only the high‐speed component of the 30 Doradus radial velocity spikes could be used as a diagnostic of individual SN origin. This opportunity became viable for it was realized that in previous, separate observations of the Honeycomb nebula (Wang 1992), itself most likely of SN origin for it is a non‐thermal radio source (Chu et al 1995; though see for a more radical alternative possibility), that one slit position for Hα and [N ii ] 6548 and 6584 Å long‐slit line profiles (Meaburn et al 1993) matched, within the ‘seeing’ disc, the position for the [S ii ] 6717 and 6731 Å profiles (Redman et al 1999). Sound diagnostic optical line ratios of the high‐speed ionized gas therefore became accessible.…”

Section: Introductionmentioning

confidence: 99%

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Towards an explanation for the 30 Dor (LMC) Honeycomb nebula - the impact of recent observations and spectral analysis

Meaburn¹,

Redman²,

Boumis³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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The unique Honeycomb nebula, most likely a peculiar supernova remnant, lies in 30 Doradus in the Large Magellanic Cloud (LMC). Due to its proximity to SN1987A, it has been serendipitously and intentionally observed at many wavelengths. Here, an optical spectral analysis of forbidden line ratios is performed in order to compare the Honeycomb high-speed gas with supernova remnants in the Galaxy and the LMC, with Galactic Wolf-Rayet nebulae and with the optical line emission from the interaction zone of the SS433 microquasar and W50 supernova remnant system. An empirical spatiokinematic model of the images and spectra for the Honeycomb reveals that its striking appearance is most likely due to a fortuitous viewing angle. The Honeycomb nebula is more extended in soft X-ray emission and could in fact be a small part of the edge of a giant LMC shell revealed for the first time in this short wavelength domain. It is also suggested that a previously unnoticed region of optical emission may in fact be an extension of the Honeycomb around the edge of this giant shell. A secondary supernova explosion in the edge of a giant shell is considered for the creation of the Honeycomb nebula. A microquasar origin of the Honeycomb nebula as opposed to a simple supernova origin is also evaluated.

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Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Towards an explanation for the 30 Dor (LMC) Honeycomb nebula - the impact of recent observations and spectral analysis

Meaburn¹,

Redman²,

Boumis³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…1t).ÈThis object was identiÐed as a multiloop nebula by Wang (1992) and suggested as the result of an SNR shock by Meaburn et al (1993Meaburn et al ( , 1995. A detailed X-ray and optical study of this object has been carried out by Chu et al (1995).…”

Section: Appendix a Individual Snr Properties And Referencesmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

Williams

Chu

Dickel

et al. 1999

ASTROPHYS J SUPPL S

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We have used archival ROSAT data to present X-ray images of 31 supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have classiÐed these remnants according to their X-ray morphologies, into the categories of shell-type, di †use face, centrally brightened, point-sourceÈdominated, and irregular. We suggest possible causes of the X-ray emission for each category and for individual features of some of the SNRs.

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“…This explanation is especially attractive given its association with the Ω lobe, thought to be part of a large-scale outflow from the GC (e.g., [33]). For instance, a helical-like structure-the Honeycomb Nebulahas been observed in the vicinity of the 30 Dor star-forming region of the Large Magellanic Cloud ( [34]; [35]). The structure has a scale of approximately 30 pc, and ( [36]) have proposed that it is produced by the blast wave from a younger SN interacting with an older supernova shell that has undergone a Rayleigh-Taylor instability.…”

Section: Discussionmentioning

confidence: 99%

The Strength and Structure of the Galactic Center Magnetic Field

Larosa

Shore

Joseph

et al. 2006

J. Phys.: Conf. Ser.

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This paper summarizes recently obtained, strong evidence for a weak global field in the Galactic center (GC): the existence of a large-scale region of diffuse, low-frequency, nonthermal emission coincident with the central molecular zone. The overall energetics of this emission, considered along with constraints on GC cosmic ray energy density and diffusion, indicate clearly that the magnetic field pervading this region is ∼ 10 µG. For completeness, additional points on the orientation of the GC nonthermal filaments, rotation measures of extragalactic sources seen through the GC, and comparison with other normal spiral galaxies are also reviewed.

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The kinematics of the Honeycomb nebula in the vicinity of SN 1987A

Cited by 7 publications

References 0 publications

Towards an explanation for the 30 Dor (LMC) Honeycomb nebula - the impact of recent observations and spectral analysis

Towards an explanation for the 30 Dor (LMC) Honeycomb nebula - the impact of recent observations and spectral analysis

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

The Strength and Structure of the Galactic Center Magnetic Field

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