Evolution of the Radio Remnant of Supernova 1987a: Morphological Changes From Day 7000

Ng, C.‐Y.; Zanardo, Giovanna; Potter, Toby; Gaensler, B. M.; Manchester, R. N.; Tzioumis, A. K.

doi:10.1088/0004-637x/777/2/131

Cited by 39 publications

(102 citation statements)

References 31 publications

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“…These observations are taken using 6-km configurations only, with typically ∼ 10 hr of on-source time. This publication covers all observations taken to February 2017 of the source, with observations prior to 2013 July 18 also discussed by Ng et al (2013). Our new observations are summarized in Table 2.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…We fit two geometries to the remnant: a 3D torus model and a 2D ring model. Based on previous studies of 9-GHz observations (e.g., Ng et al 2008Ng et al , 2013 and the complex remnant geometry (see simulations by (Potter et al 2014)), we fit the data with two geometrical model: a 2D ring and a 3D torus. The 2D models allow us to compare to the model used in X-ray studies (Racusin et al 2009;Helder et al 2013;Frank et al 2016).…”

Section: Fittingmentioning

confidence: 99%

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The Reacceleration of the Shock Wave in the Radio Remnant of SN 1987A

Cendes

Gaensler

et al. 2018

ApJ

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We report on updated radio imaging observations of the radio remnant of Supernova 1987A (SN 1987A) at 9 GHz, taken with the Australia Telescope Compact Array (ATCA), covering a 25-year period . We use Fourier modeling of the supernova remnant to model its morphology, using both a torus model and a ring model, and find both models show an increasing flux density, and have shown a continuing expansion of the remnant. As found in previous studies, we find the torus model most accurately fits our data, and has shown a change in the remnant expansion at Day 9,300 ±210 from 2,300 ±200 km/s to 3,610 ±240 km/s. We have also seen an increase in brightness in the western lobe of the remnant, although the eastern lobe is still the dominant source of emission, unlike what has been observed at contemporary optical and X-ray wavelengths. We expect to observe a reversal in this asymmetry by the year ∼2020, and note the south-eastern side of the remnant is now beginning to fade, as has also been seen in optical and X-ray data. Our data indicate that high-latitude emission has been present in the remnant from the earliest stages of the shockwave interacting with the equatorial ring around Day 5,000. However, we find the emission has become increasingly dominated by the low-lying regions by Day 9,300, overlapping with the regions of X-ray emission. We conclude that the shockwave is now leaving the equatorial ring, exiting first from the south-east region of the remnant, and is re-accelerating as it begins to interact with the circumstellar medium beyond the dense inner ring.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Fittingmentioning

confidence: 99%

The Reacceleration of the Shock Wave in the Radio Remnant of SN 1987A

Cendes

Gaensler

et al. 2018

ApJ

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“…The outermost ejecta have been interacting with the inner, equatorial ring since day ∼3000, resulting in a number of hotspots appearing in the optical images as well as a sharp increase in flux across the electromagnetic spectrum (e.g., Gröningsson et al 2008;Helder et al 2013;Ng et al 2013). The optical emission from the ring peaked around 8000 days and is now decaying as the ring is being destroyed by the shocks .…”

Section: Introductionmentioning

confidence: 99%

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Larsson

Fransson

Spyromilio³

et al. 2016

ApJ

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Due to its proximity, SN1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN1987A obtained ∼10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Hα to date, the first 3D maps for 44 Ti. The time evolution of Hα shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, Hα and [Si I]+[Fe II] 1.644 μm, show substructures at the level of ∼200-1000 km s -1 and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.

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“…#""" $""" %""" &""" '""" (""" )""" *""" +,-./.0123/.4536178, Ng et al (2013) via fitting the SNR with a torus (black) and an elliptical ring (red: semi-major axis; green: semi-minor axis). The radius of the radio remnant is compared with that derived from X-ray images (blue, from Helder et al 2013).…”

Section: Morphologymentioning

confidence: 99%

The Radio Remnant of Supernova 1987A − A Broader View

Zanardo

Indebetouw

et al. 2017

Proc. IAU

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Abstract. Supernova remnants (SNRs) are powerful particle accelerators. As a supernova (SN) blast wave propagates through the circumstellar medium (CSM), electrons and protons scatter across the shock and gain energy by entrapment in the magnetic field. The accelerated particles generate further magnetic field fluctuations and local amplification, leading to cosmic ray production. The wealth of data from Supernova 1987A is providing a template of the SN-CSM interaction, and an important guide to the radio detection and identification of core-collapse SNe based on their spectral properties. Thirty years after the explosion, radio observations of SNR 1987A span from 70 MHz to 700 GHz. We review extensive observing campaigns with the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/submillimeter Array (ALMA), and follow-ups with other radio telescopes. Observations across the radio spectrum indicate rapid changes in the remnant morphology, while current ATCA and ALMA observations show that the SNR has entered a new evolutionary phase.Keywords. circumstellar matter, ISM: supernova remnants, radio continuum: general, supernovae: individual (SN 1987A), acceleration of particles, radiation mechanisms: nonthermal BackgroundRadio supernovae are most consistently identified with core-collapse supernovae (CCSNe) and their transition into supernova remnants (SNRs). The radio emission results from the collision of the supernova (SN) shock and the progenitor's circumstellar medium (CSM). Many radio SNe can be associated with HII regions or regions of active star formation. Given the high ambient pressure of the surrounding HII region, radio SNe and their remnants are primarily identified by dense CSM environments. The SN shock wave modifies the CSM as it passes through it, both by compression and shock heating. The 1 arXiv:1707.09503v2 [astro-ph.HE]

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Evolution of the Radio Remnant of Supernova 1987a: Morphological Changes From Day 7000

Cited by 39 publications

References 31 publications

The Reacceleration of the Shock Wave in the Radio Remnant of SN 1987A

The Reacceleration of the Shock Wave in the Radio Remnant of SN 1987A

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

The Radio Remnant of Supernova 1987A − A Broader View

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