Abstract
Physical properties of supernova 1987A were investigated including: Expansion velocity; Current mass; Radius; Temperature and the Rate of the expansion by applying Counting Pixels Method (CPM) in comparison with the application of the Povida and Self-Similar Solution theoretical models which in forced the idea for adopting such a model to be applied for supernova type II. Then tow results are found to be in a good agreement with the Self-Similar solution model rather than that of Povida model. The high density of the region that surrounded the exploding system acting as decelerating parameter and down the expansion velocity of the supernova from 3900 km·s-1 to 1200 km·s-1 during the past 23 years from the explosion, with a current size equal 0.39 pc, and with an expansion rate of 0.41 per a year.
Highlights
Physical properties of supernova 1987A were investigated including: Expansion velocity; Current mass; Radius; Temperature and the Rate of the expansion by applying Counting Pixels Method (CPM) in comparison with the application of the Povida and Self-Similar Solution theoretical models which in forced the idea for adopting such a model to be applied for supernova type II
Core-collapse supernovae represent the dramatic endpoint of the life of a massive star and most of our information about it was from the theoretical hypotheses of astrophysicists; this was the case until 1987 when the nature has offered us a unique opportunity to learn the details of one of the most frequent and violent events in the universe, this was the discovery of Supernova 1987A (SN 1987A) that occurred in the Large Magellanic Cloud (LMC), a companion galaxy to our own Milky Way galaxy, on 24 February 1987 [1]
The optical study of the southern hemisphere and especially in Chili observatory confirmed that this supernova occurred in the LMC at a distance about 50 Kpc from our Milky Way galaxy at Right Ascension [α = 05h 35m 49.992s] and Declination [δ = −69 ̊17'50.08"] [7], and it cause from the exploding of 20 Mʘ Blue Supergiant star (BSG) which is called in the astronomical atlas as Sk −69 ̊ 202 [2] and like all blue supergiant it was extremely luminous with an absolute visual magnitude of −6.3m, and with a visual magnitude 12.4m and spectral class B3I [3]
Summary
Core-collapse supernovae represent the dramatic endpoint of the life of a massive star and most of our information about it was from the theoretical hypotheses of astrophysicists; this was the case until 1987 when the nature has offered us a unique opportunity to learn the details of one of the most frequent and violent events in the universe, this was the discovery of Supernova 1987A (SN 1987A) that occurred in the Large Magellanic Cloud (LMC), a companion galaxy to our own Milky Way galaxy, on 24 February 1987 [1]. The unusual properties of this supernova deduced due to the extent of the stellar winds from both the red and blue supergiant due to this transition, such as the high density region that surround the exploding star which represented by the triple ring system that consisting of a central circular ring of diameter 0.4 pc called equatorial ring and two other similar rings of diameter 0.9 pc one on either side which is oriented north and south of the supernova forming an hour-glass structure [12] This system had been observed after 310 days from the explosion by Ground-based and HST [13] through its λ 5007 Å [OIII] emission line [14], which emitted due to the interaction that occurred between the soft X-ray from the explosion and these stationary rings. The optical images of the remnant of SN 1987A which observed by HST will be interpreted in order to measure the physical size of the remnant in addition to the overall rate of expansion, using a simple method called Counting Pixels Method in comparison with the results that obtained from applying two theoretical models, which are Povida model and Self-Similar Solution model as will preformed
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