User talk:Sfuerst

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Oh, by the way, I noticed your username. Are you by any chance involved with the Angband computer game? I used to be on the IRC channel as Pakaran. -- Pakaran 05:18, 12 January 2006 (UTC)

Yes, I'm the maintainer of Zangband. (So I know all about the inner workings of Angband.) Sfuerst 05:20, 12 January 2006 (UTC)
 * Ah, I'm sorry for not remembering. I knew the name rang a bell. -- Pakaran 05:40, 12 January 2006 (UTC)

Elements
Good job, it's lookin good :) Tawker 05:50, 10 February 2006 (UTC)

Thanks. :-) Sfuerst 05:55, 10 February 2006 (UTC)

FUTBOLIN
You look like the kind of guy who could comment on this article, languishing on Dead-End pages for 4 months. Is this worth keeping, merging, enhancing? If it's worthwhile, would you be prepared to take ownership and bring it up to standard? MNewnham 19:13, 11 February 2006 (UTC)

Not sure... I've had a look, and basically it is a stub for someones pet code that they have developed. I suppose I can add some more information from their paper... On the other hand, if the article was deleted, I wouldn't really care much. Sfuerst 03:38, 12 February 2006 (UTC)

Is this, then Original Research? MNewnham 20:36, 14 February 2006 (UTC)

Not quite. It is documented elsewhere, albeit in hard to obtain locations. I think this is more equivalent to fancruft. The real problem is that it is difficult to get a neutral POV when there seems to be only one source about this code. Sfuerst 05:54, 16 February 2006 (UTC)

Black hole
"collapse of a large gas cloud via an intermediate stage of a relativistic star"

Can you explain to me what it means? I did a bit google search on "relativistic star" but just found some hits on neutron star spin slow-down. -MegaHasher 21:40, 2 March 2006 (UTC)

A 'relativistic star' is a star where the equation of state has a polytropic index of 4/3. Stars with this equation of state are very unstable with regards to radial perturbations, and don't last very long. They may not even last long enough to obtain hydrostatic equillibrium. See ie. astro-ph/0602363 for one such model where the bars-within-bars instability causes collapse. One of the original papers on this is by S. Chandrasekhar, 1964, ApJ, 140, 417. Sfuerst 23:31, 3 March 2006 (UTC)

Black hole electron
Hi Sfuerst: If you are interested in the Wikipedia "Black hole electron" article, I believe you could provide a significant contribution. An implied time dilation factor at the Kerr-Newman ring singularity is (approx) 1.0251x10 exp-22 to one. This ratio is considered to be a function of gravitational potential and so is independent of any specific mass value. This ratio is only approximatly correct because we don't have a precise value for the constant "G". If the precise applicable G value is very close to 6.6717456x10 exp -11 then a quantized black hole mass value equal to the electron mass can be specified. Let me know if you have interest in this. DonJStevens (talk) 17:41, 6 January 2008 (UTC)

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