A search for soft X-rays from supernova 1987A

Aschenbach, B.; Briel, U. G.; Pfeffermann, E.; Bräuninger, H.; Hippmann, H.; Trümper, J.

doi:10.1038/330232a0

Cited by 19 publications

(4 citation statements)

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“…While the presence of large-scale macroscopic mixing of ejecta in core collapse SNe has been well established on both observational and theoretical grounds (see and references therein), such mixing is not complete on a microscopic level. For example, X-ray observations of the Vela SNR (Aschenbach et al 1995) show several fragments outside of the general boundary, and ASCA (Tsunemi et al 1999) and XMM-Newton (Aschenbach & Miyata 2003) observations of fragment A have revealed a significant overabundance of Si and Mg, confirming that this fragment is ejecta. Widespread evidence that the ejecta of core collapse supernovae are clumpy is further noted in Wang & Chevalier (2002).…”

Section: Discussionmentioning

confidence: 98%

The formation of broad emission line regions in supernova-QSO wind interactions

Pittard

Dyson

Falle

et al. 2003

A&A

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Abstract. One aspect of supernova remnant evolution that is relatively unstudied is the influence of an AGN environment. A high density ambient medium and a nearby powerful continuum source will assist the cooling of shocked ejecta and sweptup gas. Motion of the surrounding medium relative to the remnant will also affect the remnant morphology. In an extension to previous work we have performed 2D hydrodynamical calculations of SNR evolution in an AGN environment, and have determined the evolutionary behaviour of cold gas in the remnant. The cold gas will contribute to the observed broad line emission in AGNs, and we present preliminary theoretical line profiles from our calculations. A more detailed comparison with observations will be performed in future work. The SNR-AGN interaction may be also useful as a diagnostic of AGN winds.

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Section: Discussionmentioning

confidence: 98%

The formation of broad emission line regions in supernova-QSO wind interactions

Pittard

Dyson

Falle

et al. 2003

A&A

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“…In soft X-rays it took a long time, actually almost 3.5 years, to detect soft X-rays. The first attempt which was carried out with a sounding rocket experiment and an imaging X-ray telescope in August 1987, just half a year after the explosion, provided an upper limit of 1.5×10 36 erg/s, which indicated a very low ambient matter density compliant with a wind of a blue supergiant (Aschenbach et al, 1987). Since the launch of ROSAT SN 1987A has been monitored regularly and the monitoring is now being taking over by Chandra and XMM-Newton.…”

Section: Sn 1987amentioning

confidence: 99%

X-rays from supernova remnants

Aschenbach

1999

Nuclear Physics B - Proceedings Supplements

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“…An upper limit of 1.5 × 10 36 erg s −1 could be established which excluded an ambient dense and slow wind typical for a red supergiant wind, but which is still compatible with a blue supergiant (Aschenbach et al 1987). X-rays from SN 1987 A became clearly visible in the ROSAT images not much before spring 1992 (Beuermann et al 1994;Gorenstein et al 1994).…”

Section: Introductionmentioning

confidence: 99%

XMM-Newton observations of SN 1987 A

Haberl¹,

Geppert²,

Aschenbach³

et al. 2006

A&A

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Context. We report on XMM-Newton observations of SN 1987 A in the Large Magellanic Cloud. Aims. The large collecting area telescopes together with the European Photon Imaging Cameras (EPIC) provide X-ray spectra with unprecedented statistical quality and make it possible to investigate the spectral evolution during the brightening observed since the discovery in X-rays. High resolution spectra from the Reflection Grating Spectrometers yield a complementary view and allow us to perform more detailed investigations of prominent emission lines. Methods. The X-ray spectra were modeled with two-temperature emission components from a hot plasma in collisional ionization equilibrium and in non-equilibrium (NEI). Results. We find a temperature for the equilibrium component of 0.24 ± 0.02 keV in January 2000 and April 2001 which increased to 0.30 ± 0.02 keV in May 2003 and also an indication for a temperature increase in the hot NEI component from ∼2 keV to ∼3 keV. Emission line ratios inferred from the RGS spectra suggest temperatures as low as 100 eV and an increase in the ionization state of oxygen and neon consistent with the observed temperature increases. The fast readout of the EPIC-pn instrument yields X-ray fluxes free of CCD pile-up effects which we used to normalize pile-up corrections for the published Chandra fluxes. The corrected X-ray light curve of SN 1987 A in the 0.5−2.0 keV energy band is best represented by a linear increase up to about day 4000 after the explosion and an exponential rise afterwards until the last published Chandra observation on day 6716. Modeling the light curve by emission from the inner ring which is approximated by a circular torus a central density n H = 1.15 × 10 4 cm −3 is found. In this model the forward shock has just passed the center of the torus. Conclusions. SN 1987 A continues to brighten exponentially in soft X-rays. The X-ray spectra can be represented by pure thermal emission without significant contribution from a compact object yet.

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A search for soft X-rays from supernova 1987A

Cited by 19 publications

References 0 publications

The formation of broad emission line regions in supernova-QSO wind interactions

The formation of broad emission line regions in supernova-QSO wind interactions

X-rays from supernova remnants

XMM-Newton observations of SN 1987 A

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