Infrared and X‐Ray Evidence for Circumstellar Grain Destruction by the Blast Wave of Supernova 1987A

Dwek, Eli; Arendt, Richard G.; Bouchet, P.; Burrows, D. N.; Challis, Peter; Danziger, I. J.; Buizer, James M. De; Gehrz, R. D.; Kirshner, R.; McCray, Richard; Park, Sangwook; Polomski, Elisha; Woodward, C. E.

doi:10.1086/529038

Cited by 69 publications

(118 citation statements)

References 28 publications

(48 reference statements)

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“…This is denser, hotter, and at higher pressure than the line emitting regions, suggesting that the observed IR line emission does not arise for the same part of the ER as the dust continuum emission. To reach equilibrium temperatures of T ≈ 180 K for silicate grains, collisional heating at the low gas temperatures implied by the emission line ratios would require densities of n e  10 6 cm −3 (Bouchet et al 2006;Dwek et al 2008). Such high densities are ruled out by the observed line ratios (Figures 17 and 18).…”

Section: Gas Diagnosticsmentioning

confidence: 92%

“…Cutouts of the lines in the SH and LH data are shown in Figure 11, and lines in the SL and LL data are shown in Figure 12. Here we only discuss the lines, as the continuum in the SL and LL spectra has been analyzed by Bouchet et al (2006) and (Dwek et al 2008(Dwek et al , 2010. The continuum in the SH and LH data adds no new information and is less reliably measured as the concatenation of many spectral orders.…”

Section: Line Identificationmentioning

confidence: 99%

“…About 1000 days later, Dwek et al (2008) reported that further Spitzer observations had shown the dust was unchanged in temperature and increasing in brightness, but not increasing as rapidly as the X-ray emission. The decreasing ratio of IR to X-ray emission (IRX) was interpreted as destruction of dust behind the blast wave on timescales shorter than that for the cooling of the shocked, X-ray emitting gas.…”

Section: Introductionmentioning

confidence: 99%

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Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

Arendt

Dwek

Bouchet

et al. 2016

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Spitzer observations of SN 1987A have now spanned more than a decade. Since day ∼4000, mid-infrared (mid-IR) emission has been dominated by that from shock-heated dust in the equatorial ring (ER). From 6000 to 8000 days after the explosion, Spitzer observations included broadband photometry at 3.6-24 μm, and low and moderate resolution spectroscopy at 5-35 μm. Here we present later Spitzer observations, through day 10,377, which include only the broadband measurements at 3.6 and 4.5 μm. These data show that the 3.6 and 4.5 μm brightness has clearly begun to fade after day ∼8500, and no longer tracks the X-ray emission as well as it did at earlier epochs. This can be explained by the destruction of the dust in the ER on timescales shorter than the cooling time for the shocked gas. We find that the evolution of the late time IR emission is also similar to the now fading optical emission. We provide the complete record of the IR emission lines, as seen by Spitzer prior to day 8000. The past evolution of the gas as seen by the IR emission lines seems largely consistent with the optical emission, although the IR [Fe II] and [Si II] lines show different, peculiar velocity structures.

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Section: Gas Diagnosticsmentioning

confidence: 92%

Section: Line Identificationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

Arendt

Dwek

Bouchet

et al. 2016

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“…The equilibrium temperature radius provides an estimate of the physical size of the hot, circumstellar dust and is given by (e.g., Smith et al 2016) is assumed for the calculation. Note that if the heating of the mid-IR emitting dust is instead dominated locally by collisions with hot electrons in a post-shock environment (e.g., Dwek 1987;Dwek et al 2008), R Eq will not reflect the physical size of the system. However, it is unlikely that the mid-IR emitting dust is dominantly heated by a shock driven from the initial outburst since the observed mass of an illuminated shell of shock-heated dust should increase rapidly as a function of time as it propagates outward radially ( et al 2011).…”

Section: Properties Of Thementioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

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We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

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“…Exhaustive study has been made of shock structure, ionization stages, and internal shock velocities (Dewey et al 2008;Gröningsson et al 2008;Heng & McCray 2007;Reighard & Drake 2007;Haberl et al 2006). Dust formation and destruction in SNRs is a subject of high current interest, and is studied in depth in SN 1987A (Dwek et al 2008;Ercolano et al 2007;Bouchet et al 2006); the general case will be discussed in §4.3. Although efforts have also been bent toward finding a pulsar, the search has not yet resulted in a detection; see Manchester (2007) for a review.…”

Section: Snr 1987amentioning

confidence: 99%

Supernova remnants in the Magellanic Clouds

Williams¹

2008

Proc. IAU

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Abstract. At the 1998 IAU Symposium on the Magellanic Clouds, Dr. Robert Petre observed that we were reaching a time where it was possible "to study the MC SNRs at a level of detail comparable with many Galactic remnants", while retaining the benefits of a global view in the MCs. Over the past decade, many researchers have taken advantage of these newly accessible populations. New MC-wide surveys at various wavelengths have enabled broader searches for SNR candidates, extending our census of MC SNRs to less prominent objects -older SNRs, SNRs in complex regions, et cetera. The use of light-echoes has provided a new avenue to probe young SNRs. Higher spatial and spectral resolutions in many wavelength regimes have enabled detailed studies of individual remnants, revealing progenitor types, pulsar-wind nebulae, expansion details, and environmental effects.Perhaps the newest conceptual development is the increasing use of the MC SNRs to study physical problems of wider significance to many fields of astronomy. For example, researchers have examined the energy and hot gas inputs of MC SNRs to the ISM, including their collective effects within superbubbles, in order to evaluate their effects on stellar feedback cycles in a galaxy. Other scientists have investigated the fraction of SNR energies going to the acceleration of cosmic rays, which has significant implications for the role of SNRs in cosmic-ray production. Most recently, the onslaught of Spitzer data has led to new exploration of dust in MC SNRs, allowing us to probe dust creation, depletion, and destruction in the MC SNR populations. In summary, the study of SNRs in the MCs appears to have "come of age" over the past decade, becoming a mature field with rich potential for future scientific work.

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Infrared and X‐Ray Evidence for Circumstellar Grain Destruction by the Blast Wave of Supernova 1987A

Cited by 69 publications

References 28 publications

Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

Infrared Continuum and Line Evolution of the Equatorial Ring Around Sn 1987a

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Supernova remnants in the Magellanic Clouds

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