We report here on 5-GHz global very-long-baseline interferometry (VLBI) observations of SN 1986J, 16 yr after its explosion. We obtained a high-resolution image of the supernova, which shows a distorted shell of radio emission, indicative of a deformation of the shock front. The angular size of the shell is ~4.7 mas, corresponding to a linear size of ~6.8 × 1017 cm for a distance of 9.6 Mpc to NGC 891. The average speed of the shell has decreased from ~7400 km s-1 in 1988.74 down to about 6300 km s-1 in 1999.14, indicative of a mild deceleration in the expansion of SN 1986J. Assuming a standard density profile for the progenitor wind (?cs~r-s, s= 2), the swept-up mass by the shock front is ~2.2 Msolar. This large swept-up mass, coupled with the mild deceleration suffered by the supernova, suggests that the mass of the hydrogen-rich envelope ejected at explosion was >~12 Msolar. Thus, the supernova progenitor must have kept intact most of its hydrogen-rich envelope by the time of explosion, which favours a single, massive star progenitor scenario. We find a flux density for SN 1986J of ~7.2 mJy at the observing frequency of 5 GHz, which results in a radio luminosity of ~1.4 × 1037 erg s-1 for the frequency range 107-1010 Hz (?=-0.69 S?~??). We detect four bright knots that delineate the shell structure, and an absolute minimum of emission, which we tentatively identify with the centre of the supernova explosion. If this is the case, SN 1986J has then suffered an asymmetric expansion. We suggest that this asymmetry is due to the collision of the supernova ejecta with an anisotropic, clumpy (or filamentary) medium.
A distorted radio shell in the young supernova SN1986J
2002
Abstract
We report here on 5-GHz global very-long-baseline interferometry (VLBI) observations of SN 1986J, 16 yr after its explosion. We obtained a high-resolution image of the supernova, which shows a distorted shell of radio emission, indicative of a deformation of the shock front. The angular size of the shell is ~4.7 mas, corresponding to a linear size of ~6.8 × 1017 cm for a distance of 9.6 Mpc to NGC 891. The average speed of the shell has decreased from ~7400 km s-1 in 1988.74 down to about 6300 km s-1 in 1999.14, indicative of a mild deceleration in the expansion of SN 1986J. Assuming a standard density profile for the progenitor wind (?cs~r-s, s= 2), the swept-up mass by the shock front is ~2.2 Msolar. This large swept-up mass, coupled with the mild deceleration suffered by the supernova, suggests that the mass of the hydrogen-rich envelope ejected at explosion was >~12 Msolar. Thus, the supernova progenitor must have kept intact most of its hydrogen-rich envelope by the time of explosion, which favours a single, massive star progenitor scenario. We find a flux density for SN 1986J of ~7.2 mJy at the observing frequency of 5 GHz, which results in a radio luminosity of ~1.4 × 1037 erg s-1 for the frequency range 107-1010 Hz (?=-0.69 S?~??). We detect four bright knots that delineate the shell structure, and an absolute minimum of emission, which we tentatively identify with the centre of the supernova explosion. If this is the case, SN 1986J has then suffered an asymmetric expansion. We suggest that this asymmetry is due to the collision of the supernova ejecta with an anisotropic, clumpy (or filamentary) medium.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
