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Someone suggested this object to be 31 Ori. After further research, equipped with the name, I confirmed this object to be 31 Ori. Source of confirmation: http://www.astrostudio.org/xhip.php?hip=25737

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There are several misconceptions in your question. First, a star does not vacuum everything in its vicinity. Rather it forms from a condensation in a gas cloud, which in turn collapses to a proto-star surrounded by a gas disc, which can contribute further material. Once formed in this way, a star typically does not acquire more gas (exceptions are symbiotic ...

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I'm no expert on stellar atmospheres, so I have a limited idea of how things like $\log g$ affect the lines. But I work with stellar models, so I can take a stab at that part. The overall principle is that computing stellar model ages is a kind of optimization problem. We model the structure of stellar interiors by constructing a system of differential ...

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For some very large (and hence relatively cool) red giants you might be able to ascertain something from their spectra, as emission lines are sometimes seen - these are typically brighter central patches seen the middle of the more typical absorption (dark) spectral lines - caused by the large size of (realtively!) hot gas clouds that surround the giants. ...

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From this webpage, I have a few statistics regarding required density and temperature to burn a specific element. Burning phase; Required temperature; Required mean density; Duration Hydrogen burning: $4 \times 10^7 \text{ degrees K; } 5 \text{ gm per cubic cm; } 7,000,000 \text{ years}$ Helium burning: \$2 \times 10^8 \text{ degrees K; } 700 \text{ gm ...

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Gravitational collapse occurs when an object's internal pressure is insufficient to resist the object's own gravity. In the cases of stars, it normally usually happens because of one of these 2 reasons: The star has too little "fuel" left to maintain its temperature The star that would have been stable receives extra matter in a way that does not raise ...

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