main sequence

The star used to be like the sun, a "main sequence" star that burns hydrogen by nuclear fusion, producing helium.

Confirmation of a planet circling a "normal" main-sequence star did not come until 1995.

The greater the mass of such a star, the more quickly it will use its hydrogen fuel and the shorter it stays on the main sequence.

A heavy star at the upper end of the main sequence has a rather different later history.

As these luminous and massive stars exhaust their hydrogen fuel, they begin to depart from the upper end of the main sequence.

As the main-sequence mass of the star increases, the mass of the final remnant left as a white-dwarf star also increases.

Nuclear fusion is what powers all Main Sequence stars in the universe, and efforts to exploit this energy have been ongoing for decades.

In general, the distance from the main sequence metric attempts to compensate for real-world implementations.

By monitoring the distance from the main sequence metric, you can gauge whether packages are becoming unbalanced.

By plotting packages along this line and measuring their distance from the main sequence, you can infer a package's balance.

Examining the distance from the main sequence metric yields interesting results.

In the H- R diagram below , our Sun is now in the main sequence .

While on the main sequence, they are hot and blue, some 1, 000 to 1 million times as luminous as the sun and are roughly 10 times wider.

Our sun should leave the main sequence in about 5 billion years.

A main sequence of instructions.

When a massive proto -star approaches the main sequence, its surface temperature is low and it can not ionize the ambient gas.

Document the prerequisites and main sequence for running scripts

Lithium and Beryllium Depletions in Low Main-Sequence Stars

Turn-off point from main sequence