What is a blue giant, and what is the difference between a red giant and a blue giant

"Blue Giant" is a machine that can accurately detect the pitch, rhythm and intonation of the singer, so as to give a scientific evaluation of singing. "The system has four difficulty settings, such as simple, standard, advanced, and expert, and different difficulties use different scoring rules, and the higher the difficulty, the higher the requirements for the players. At the same time, the real-time subtitle scrolling display method can intuitively tell the contestants the lyrics, pitch, pronunciation time and other elements.

The producer of the column told reporters yesterday that compared with the rating machine used in other satellite TV programs, the function of "Blue Giant" is more powerful and more intuitive, and it can instantly display the similarity between each lyric of the singer and the original song in pitch, rhythm and pitch on the screen, and finally give a score. "Blue Giant" was formerly known as "Shanda Network", a singing pitch system for online interactive communities.

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A thing that scores the pitch of a sing.

Red supergiants and blue supergiants are about the same size.

Although the size of the two is about the same, but the other places are very different, according to the names of the two, it can be judged that the color of the two is different, one is red and the other is blue, and it is also named after the color of the star, and the reason for the formation is that it is squeezed or collided in space.

Red supergiants and blue supergiants featuresThe surface temperature of the two is different, the temperature of the blue supergiant is relatively high, it can reach 10,000 to 50,000 degrees, and the brightness is also very bright, the red supergiant is much worse in temperature and brightness, the mass of the blue supergiant is also ten times that of the sun, and it is a very large existence in the universe.

1. When a star passes its long period of young adulthood, the main sequence stage, and enters old age, it will first become a red giant.

2. Blue giants are high-quality main-sequence stars, and their internal nuclear reaction rates are very large, and they are oversized stars.

3. Red giants are orange-red in color, have a low temperature (k m type), and are usually old stars; Blue giants, on the other hand, have extremely high temperatures and are a model for young stars.

Blue giants differ in size and mass from blue supergiants, with giants exploding into dwarfs and supergiants turning into neutron stars (or pulsars) or black holes. Blue giants and bright blue giants have different temperatures.

Blue supergiants are stars of type o or b spectral type in the first class of the spectral classification of stars. In layman's terms, it is the main sequence star of a massive star. These stars are usually more than 10 times more massive than the Sun, and because they burn at an extremely fast rate and release energy, they have a very high surface temperature (usually above 10,000 degrees), so they appear blue.

Blue supergiants evolve into red supergiants (red giants that are different from low-mass stars) when they enter the carbon fusion phase.

Most of these stars cause supernovae when they die.

In fact, it is a giant planet next to the black hole, which orbits the black hole at a certain angle and at a certain speed (the sky completes one revolution), and the black hole sucks hundreds of tons of gas from the blue giant star every day, and I can only provide that.

Blue giants are naturally occurring giants with extremely high temperatures, high mass, and small size. Red giants are another form of dwarf stars (except brown dwarfs, white dwarfs, and black dwarfs), and are low-temperature, small-mass super-large stars with medium Sunpocust mass stars that have passed through the main-sequence stage.

Blue supergiants are the first level of the spectral classification of stars and belong to one of the supergiant stars. They are very hot and bright, with a surface temperature of 20,000 to 50,000 °C and a mass of about 10 50 times that of the Sun.

The most famous blue pennymph supergiant is Betelgeuse, S.N. in the constellation Orion

1987a was also the result of a blue supergiant's hand search**, and most of the second type 2 supernovae (type supernovae) were thought to be red supergiants, however, the predecessor of supernova 1987a, the potato wheel, was a blue supergiant.

However, he may have been a red supergiant before the powerful stellar winds blew away several layers of gas shells outside. This is also the first time astronomers have observed a blue supergiant**.

Blue supergiants have fast but sparse stellar winds, which can cause material that has been released during the red supergiant stage to be compressed into the extended shell.

Blue supergiants are stars of type O or B in the first class of the stellar light dispersion spectrum classification of stars. In layman's terms, it is the main sequence star of a massive star. These stars are usually more than 10 times more massive than the Sun, and because of their extremely fast combustion rate and strong energy release, their surface temperatures are very high (usually above 10,000 degrees), so they appear blue.

Blue supergiants evolve into red supergiants (as opposed to red giants with stars in the small mass segment) when they enter the carbon fusion phase.

Most of these stars cause supernovae when they die.

A special blue giant: Wolf-Layet.

wolf-rayetstar

There are many very wide emission lines superimposed on a continuum similar to that of type stars, which were first discovered by French astronomers Wolf and Laille, hence the name, WR or W for short. About 250 have been discovered in the Milky Way and several neighboring galaxies. WR is divided into two subtypes:

The nitrogen and carbon sequences are denoted as wn and wc, respectively. Compared with the elemental abundances in the atmospheres of ordinary O-type and B-type stars, the content of hydrogen in the atmosphere of WR stars is 50 150 times less, the nitrogen content of WN stars is 50 100 times higher, and the carbon content of WC stars is 400 700 times higher. On the Herault diagram, the WR star is located above the main sequence.

According to the analysis of the spectral line profile, the WR star has a strong stellar wind, and the estimated mass loss rate is 10-5 10-4 solar mass years. Such a large mass loss rate cannot be maintained for a long time, indicating that the WR star is not very old, but due to the rapid evolution of the massive star, the hydrogen has been burned out and is in the post-main sequence stage.