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Supernova in M31

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    Supernova in M31

    Wie weet meer?
    30cm en 20cm Hofheim kofferdobsons | Polarex model 132 | Lunt LS50tha | Swarovski 12*50 EL

    #2
    ik ga nu zoeken..

    Net ontploft? Tenminste, voor ons gesproken dan? nee toch?
    I (L) MY LB!

    Jij bent gek Brazilliaanze hakkebar!

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      #3
      # Nova M31 2006 7, CBET 615 discovered 2006/09/03.516 by Koichi Itagaki Found in M31 at R.A. = 00h42m33s.16, Decl. = +4110'06".8
      # Located 11.1" west and 6'02' south of the center of NGC 224 (= M31) (Discovery image)
      # Mag 16.0, Extragalactic Nova

      http://www.rochesterastronomy.org/sn2006/novae.html
      Vuja De': the strange feeling you get that nothing has happened before.
      http://www.everyoneweb.com/demelzaramakers/

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        #4
        Magn. 16? hmmm... Dat gaat niet lukken met mijn scoop. Jammer
        "Dat is geen bewolking! Dat zijn de Magelheanse wolken.."

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          #5
          Het kan natuurlijk helderder worden!
          30cm en 20cm Hofheim kofferdobsons | Polarex model 132 | Lunt LS50tha | Swarovski 12*50 EL

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            #6
            Volgens http://www.daviddarling.info/encyclopedia/N/nova.html :

            * Fast novae rise very steeply rise to maximum, stay at maximum for a few days at most, then decline, rapidly to begin with (typically fading by a factor of 10 in three months). The fading may involve a prolonged series of marked fluctuations. A classic example is Nova Persei 1901.
            * Slow novae rise gradually to maximum, then remain there for several weeks or months before declining. They tend to fade slowly at first with fluctuations, after which the rate of fading quickens. As these novae continue to decrease in brightness, it is common to see them brighten slowly and irregularly to a second maximum, followed by a return to the minimum state. A factor-of-10 dimming from maximum typically takes 150 days or more. Some slow novae show a deep, wide minimum about 2 to 5 months after maximum, which may be due to dust condensation that blocks the visible light. As the ejected material dissipates, the nova recovers to a brightness approximately equal to that expected in an undisturbed decline. Nova Herculis 1934 is a well-known example.
            * Very slow novae are a small group with maxima that extend over years and with declines that also take place extremely slowly. In 1915, RT Serpentis, the first of this type to be observed, rose slowly to magnitude 10.5, remained at this level for almost 10 years, and then began to fade very slowly, reaching magnitude 14 in 1942. Very slow novae are also referred to as symbiotic novae or RR Telescopii stars.

            Welke van de drie zou dit zijn?
            The scientific theory I like best is that the rings of Saturn are composed entirely of lost airline luggage. ~ Mark Russell

            A MacBook user!

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