Quote:
Originally Posted by Jarvamundo
Interesting comments...
"no word on the stars diameter or its density..."
I have some questions:
1) Weight loss: So have you detected "weight loss" or is this an assumption from the model?
2) You say, this is beyond the "accepted limit" so it is clearly outside of "the models" range of assumptions. Are these the same assumptions you are using to infer the "weight"?
3) Which models? i thought 150 solar masses was the limit? Is this another way of saying "nfi"?
4) ok... i'll give you that one... that star is not a human.... but... Which model are you using to determine if this star is middle aged? If you have no model that fits, are you not just making speculations beyond any accepted physics?
I find the article contradictory all the way through....
Empirics:
a) it's bright... real bright...and contains spectrum of heavy elements?
b) no determination of dimensions provided in article(s)
c) can't see any mention of orbital dynamics?
Is all this just "inferred" from spectrometry and flux counts?
I suspect, you have only inferred from a broken model that you say yourself does not permit these measurements?
Very confusing!
edit: link to paper... yes inferred mass it's all from flux counts and estimates from models that as they mention, clearly don't stand up... Why not just say that?
I'm finding it really hard to swallow the "coalescing gas" model of star formation, when with all this "wind" around... and this supermassive "young" short-term stars... anyone slightly familiar with thermodynamics knows hot "wind" gas aint guna hang around long enough to form stars... totally counter intuitive. |
My advice Alex is to grab a textbook book on star formation and the physics behind it. Or goto arXiv.org and grab some of the papers on the subject, especially about the formation of massive stars. You'll learn a bit about the subject by doing so. But, grab the textbook first...get the basics then go onto the harder stuff later.
That wind they're talking about isn't what you think. It's the continuum wind that blows all the time around these stars. It's like an "uber" solar wind, except the driving mechanism is somewhat different.
The 150 solar mass limit is due to the Eddington Limit imposed upon such large stars, however it's not fully understood and is open to change, as you have seen here. The precise cutoff in mass due to the Eddington Limit is a fluid thing and is affected by quite a few factors, least of which is how hot the star is.
The only way to determine the star's size is via spectroscopic analysis. Even in a wide binary, you still need a spectroscope to determine the orbital velocity of the star, apart from other characteristics. And at the distance this star is at, you're not going to be able to directly measure it's angular diameter....it's just too far away. So, you can determine it's size from stellar theory and what measurements you can and do take.