After six years since SN 2008in, the beautiful Messier 61 spiral galaxy in Virgo seems to host a new [52 million light years distant] supernova. Its temporary designation is PSN J12215757+0428185, and was discovered by the Japanese amateur astronomer K. Itagaki on 29.83 Oct. 2014. We are a way for the universe to know itself. Some part of our being knows this is where we came from. We long to return. And we can, because the cosmos is also within us. Were made of star stuff, Sagan famously stated ...So, all life on Earth and the atoms in our bodies were created in the furnace of now-long-dead stars, virtualtelescope.eu/wordpress/wp-content/uploads/2014/10/m61_PSNJ12215757+0428185_31oct2014.jpg Supernova PSN-J12215757+0428185 Supernova (SN) A supernova is an exploding star. This star can brighten up as much as his host galaxy during days or weeks. SN Type I These result in some binary star systems between a red giant and a white dwarf. In such a system, mass flows from the red giant to the white dwarf. Eventually, so much mass piles up on the white dwarf that it can no longer support itself and it collapses. Spectras show absorption lines of Ca II, Si, etc., but no hydrogen lines are present in the spectra. The expanding envelope almost lacks hydrogen. During 20-30 days following maximum light, the brightness decreases by approximately 0.1 mag per day, then the rate of fading slows and reaches a constant value of 0.014/day. SN Type II These supernovae occur at the end of a massive stars lifetime, when its nuclear fuel is exhausted and it is no longer supported by the release of nuclear energy. If the stars iron core is massive enough then it will collapse and become a supernova. Lines of hydrogen and other elements are apparent in their spectra. The expanding envelope consists mainly of H and He. Light curves show greater diversity than those of type I supernovae. Usually after 40-100 days since maximum light, the rate of fading is 0.1 mag per day.
Posted on: Fri, 31 Oct 2014 22:40:35 +0000
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