2011A&A...527A..35T


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:42:23

2011A&A...527A..35T - Astronomy and Astrophysics, volume 527A, 35-35 (2011/3-1)

The outer rings of SN 1987A.

TZIAMTZIS A., LUNDQVIST P., GROENINGSSON P. and NASOUDI-SHOAR S.

Abstract (from CDS):

We investigate the physical properties and structure of the outer rings of SN 1987A to understand their formation and evolution. We used low resolution spectroscopy from VLT/FORS1 and high resolution spectra from VLT/UVES to estimate the physical conditions in the outer rings, using nebular analysis for emission lines such as [O II], [O III], [N II], and [S II]. We also measured the velocity at two positions of the outer rings to test a geometrical model for the rings. Additionally, we used data from the HST science archives to check the evolution of the outer rings of SN 1987A for a period that covers almost 11 years. We measured the flux in four different regions, two for each outer ring. We chose regions away from the two bright neighbouring stars and as far as possible from the inner ring and created light curves for the emission lines of [O III], Hα, and [N II]. The light curves display a declining behaviour, which is consistent with the initial supernova-flash powering of the outer rings. The electron density of the emitting gas in the outer rings, as estimated by nebular analysis from the [O II] and [S II] lines, is ≲3x103cm–3, has not changed over the last ∼15-years, and the [N II] temperature remains also fairly constant at ∼1.2x104K. We find no obvious difference in density and temperature for the two outer rings. The highest density, as estimated from the decay of Hα, could be ∼5x103cm–3 however, and because the decay is somewhat faster in the southern outer ring than it is in the northern, the highest density in the outer rings may be found in the southern outer ring. For an assumed distance of 50kpc to the supernova, the distance between the supernova and the closest parts of the outer rings could be as short as ∼1.7x1018cm. Interaction between the supernova ejecta and the outer rings could therefore start in less than ∼20-years. We do not expect the outer rings to show the same optical display as the equatorial ring when this happens. Instead soft X-rays should provide a better way of observing the ejecta - outer rings interaction.

Abstract Copyright:

Journal keyword(s): line: profiles - ISM: supernova remnants - ISM: individual objects: SN 1987A

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
2 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4484 2
3 HD 81408 ** 09 25 05.3928990350 -12 58 00.585558346   10.59 9.62     K1/2V 39 0
4 CD-34 6792 PM* 10 32 13.6185042385 -35 37 41.710291605   12.84 11.84     F:wl: 125 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:42:23

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