I don't know about owlice, but you sure put that song in my head, Art!neufer wrote:It is my fervent wish that owlice watch Danny Kaye videoBeyond wrote:
tickety-boo Danny Kaye science terminology. Yeah, it's good.
and be incapable of ever bicycling again
without the tickety-boo song running thru her head.
I said the 'terminology' was good - referring to tickety-boo. I DIDN"T listen to the video, so i have no idea what the tune is like.
It is my fervent wish that Ann is now incapable of ever bicyclingAnn wrote:
Tickety-boo!!!!
Ann wrote:Yeah, yeah, yeah...
Sun, 18 Sep 2011 23:40:38 GMT
Name: SN 2011fe
Type: Ia
Mag: 9.9
http://www.aavso.org/supernova-science-general wrote: SN 2011fe is a bit bluer than SN 1994D
RHM's picture
Posted: September 12, 2011 - 1:16pm
Yes, you're absolutely right. The graph below shows that while SN 2011fe is tracking SN 1994D pretty well in V, R and I passbands, it's a bit brighter in the B-band. What exactly does that mean? It's not clear yet. I'd like to see a comparison of the spectra
Ann wrote:
It does appear to be blue. As to what it means, my instinctive guess would be that it is slightly brighter than the other supernova, SN 1994D.
http://astrobob.areavoices.com/?blog=78068 wrote:
Pinwheel Galaxy supernova at brightest; Comet Garradd beckons
Posted on September 17, 2011 by astrobob <<I am jazzed up. I finally got a picture of the supernova SN 2011fe in the Pinwheel Galaxy last night using only a telephoto lens on a tracking mount. The path starts at bright Mizar and zigzags its way up to the supernova, which lies just beyond the arrow tip in the Pinwheel Galaxy in this photo taken last night (Sept. 16). Alkaid and Mizar are the two stars at the end of the Big Dipper's Handle. Details: 150mm lens, f/2.8, ISO 800 and 2-minute exposure. (Photo: Bob King)
The moon is now nearly at last quarter and doesn’t flood the sky with light like it does around full phase. This provides us all with another round of opportunities to see the supernova before it fades. For almost a week, it’s been humming along at magnitude 9.9. As you can tell from the before-and-after sequence above, it’s hard to miss!
It should be noted that SN 2011fe got to a visual magnitude comparable with that of the brightest (blue hypergiant) stars of the Large Magellanic Cloud which is over a hundred times closer to us than M101Ann wrote:
It's fading!!!
On Mon, 19 Sep 2011 22:40:34 GMT, SN 2011fe was at magnitude 10.0!
http://en.wikipedia.org/wiki/S_Doradus wrote:
<<S Doradus is the brightest star in the Large Magellanic Cloud, a satellite of the Milky Way. A hypergiant, it is one of the most luminous stars known (sometimes more luminous than −10 absolute magnitude), but so far away that it is invisible to the naked eye. This star belongs to its own eponymous S Doradus class of variable stars (these classes are usually named after their prototypes); also designated as the class luminous blue variable or LBV. S Doradus exhibits long, slow changes in brightness, punctuated by occasional outbursts.>>
http://www.daviddarling.info/encyclopedia/S/S_Doradus.html wrote: <<The brightest star in the Large Magellanic Cloud (LMC), one of the brightest stars known, and the prototype for the class of variable known as S Doradus stars (luminous blue variables). It lies in the young open cluster NGC 1910 on the northern rim of the LMC's central bar.
S Doradus has a spectrum very similar to that of P Cygni (see P Cygni profile), another variable of the same type. These stars are extremely massive (at least 60 solar masses) and luminous, using up their nuclear fuel so fast that their lifetimes can't exceed a few million years; they will then explode as supernovae. The very high luminosity also results in an enormous radiation pressure at the star's surface, which tends to blow away significant portions of the stellar mass by way of an intense stellar wind and, occasionally, in the form of an ejected gaseous shell. The light curve of S Doradus also points to a long period (40-year) eclipsing variable behavior.
Recent observations of S Dor have shown that its optical spectrum now resembles that of an F-type supergiant, with a rich complex of absorption lines. Despite nearly 50 years of spectroscopic monitoring, such a spectrum has never previously been seen for S Dor despite many occasions when the star was equally bright. Such F-type spectra have, however, been seen in other luminous blue variables, including Var B in M33 during a recent outburst, and in Eta Carina during an outburst in 1893. The singly ionized metal lines arise in a layer moving away from the star (toward us) at 50 km/s, consistent with the lines forming in a "pseudo photosphere" originating in the stellar wind. The temperature suggested by the F-type spectrum is as cool as an LBV can get.>>
Beyond wrote:
I don't know if the super nova was really all that bright. It blew itself up, didn't it
I guess it will go to the great green pastures of the retired supernovae in the sky!Beyond wrote:It's 'pooped'. After expending all that energy, it's retiring from it's supernova job and getting ready to take up something easier for the rest of it's life.
