Fourier Modeling of the Radio Torus Surrounding SN 1987A

Ng, C.‐Y.; Gaensler, B. M.; Staveley‐Smith, L.; Manchester, R. N.; Kesteven, M. J.; Ball, Lewis; Tzioumis, A. K.

doi:10.1086/590330

Cited by 41 publications

(70 citation statements)

References 48 publications

(103 reference statements)

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“…The three-dimensional effects and emission regions also likely differ between these components. Ng et al (2008) predict that they will soon see a deceleration in the radio remnant expansion similar to that we have observed from the X-ray remnant due to the forward shock interacting with the optical inner ring.…”

Section: Resultssupporting

confidence: 73%

X-Ray Evolution of SNR 1987a: The Radial Expansion

Racusin¹,

Park²,

Zhekov³

et al. 2009

ApJ

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We present the evolution of the radial expansion of SNR 1987A as measured using Chandra X-ray observations taken over the last 10 years. To characterize the complex structure of the remnant and isolate the expansion measurement, we fit the images to several empirical models including: a simple circular torus, a torus with bilateral lobes, and a torus with four tangentially extended lobes. We discuss the results of this measure in the context of the overall evolution of the supernova remnant, for which we believe we have measured the end of the free expansion phase and its transition to the adiabatic phase (at least along the equatorial ring). The timing of this event is in agreement with early predictions of the remnant evolution.

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Section: Resultssupporting

confidence: 73%

X-Ray Evolution of SNR 1987a: The Radial Expansion

Racusin¹,

Park²,

Zhekov³

et al. 2009

ApJ

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“…1), making it the highest radio frequency at which this has now been accomplished. The 3-mm image shows similarities with the images at 7 and 12 mm (Manchester et al 2005;Potter et al 2009) and at 3 cm (Ng et al 2008). The emission is broadly distributed along the equatorial ring, but unlike the optical images the radio appearance is asymmetric with the emission peaking in the eastern lobe (Fig.…”

Section: Discussionmentioning

confidence: 58%

“…The flux ratio between the eastern and western halves of the image is ≈1.3. By fitting an optically thin shell, this asymmetry was found to be ≈1.3 at 7 mm (Potter et al 2009) and ≈1.4 at 3 cm (Ng et al 2008). The maximum asymmetry with respect to the VLBI position in the 3-mm image occurs near position angle 90…”

Section: Discussionmentioning

confidence: 88%

The remnant of supernova 1987A resolved at 3-mm wavelength

Lakićević

Zanardo

Loon

et al. 2012

A&A

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Context. The proximity of core-collapse supernova 1987A (SN 1987A) in the Large Magellanic Cloud (LMC) and its rapid evolution make it a unique case study of the development of a young supernova remnant. Aims. We aim at resolving the remnant of SN 1987A for the first time in the 3-mm band (at 94 GHz). Methods. We observed the source at 3-mm wavelength with a 750-m configuration of the Australia Telescope Compact Array (ATCA). We compared the image with a recent 3-cm image and with archival X-ray images.Results. We present a diffraction-limited image with a resolution of 0. 7, revealing the ring structure seen at lower frequencies and at other wavebands. The emission peaks in the eastern part of the ring. The 3-mm image bears resemblance to early X-ray images (from 1999-2000). We place an upper limit of 1 mJy (2σ) on any discrete source of emission in the centre (inside of the ring). The integrated flux density at 3 mm has doubled over the six years since the previous observations at 3 mm. Conclusions. At 3 mm -i.e. within the operational domain of the Atacama Large Millimeter/submillimeter Array (ALMA) -SN 1987A appears to be dominated by synchrotron radiation from the inner rim of the equatorial ring, characterised by moderately weak shocks. There is no clear sign of emission of a different nature, but the current limits do not rule out such component altogether.

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“…The dotted vertical line marks the current epoch. The observed radius and speed of the SN shock, as determined by radio observations (Ng et al 2008), are shown as well. The scaling values are R i = R T = 3.1 × 10 17 cm and V i = 28,000 km s −1 .…”

Section: Particle Acceleration Modelmentioning

confidence: 79%

Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Berezhko

Ksenofontov

Völk

2011

ApJ

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A nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants (SNRs) is employed to re-examine the nonthermal properties of the remnant of SN 1987A for an extended evolutionary period of 5-100 yr. It is shown that an efficient production of nuclear CRs leads to a strong modification of the outer SNR shock and to a large downstream magnetic field B d ≈ 20 mG. The shock modification and the strong field are required to yield the steep radio emission spectrum observed, as well as the considerable synchrotron cooling of high-energy electrons which diminishes their X-ray synchrotron flux. These features are also consistent with the existing X-ray observations. The expected γ -ray energy flux at TeV energies at the current epoch is nearly γ F γ ≈ 4 × 10 −13 erg cm 2 s −1 under reasonable assumptions about the overall magnetic field topology and the turbulent perturbations of this field. The general nonthermal strength of the source is expected to increase roughly by a factor of two over the next 15-20 years; thereafter, it should decrease with time in a secular form.

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Fourier Modeling of the Radio Torus Surrounding SN 1987A

Cited by 41 publications

References 48 publications

X-Ray Evolution of SNR 1987a: The Radial Expansion

X-Ray Evolution of SNR 1987a: The Radial Expansion

The remnant of supernova 1987A resolved at 3-mm wavelength

Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

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